The class Cosmology. More...

#include "Headers/Cosmology.h"

Public Member Functions
Constructors/destructors
	Cosmology (const double Omega_matter=0.27, const double Omega_baryon=0.046, const double Omega_neutrinos=0., const double massless_neutrinos=3.04, const int massive_neutrinos=0, const double Omega_DE=0.73, const double Omega_radiation=0., const double hh=0.7, const double scalar_amp=2.46e-9, const double scalar_pivot=0.05, const double n_spec=0.96, const double w0=-1., const double wa=0., const double fNL=0., const int type_NG=1, const double tau=0.09, const std::string model="LCDM", const bool unit=true)
	constructor More...

	Cosmology (const CosmologicalModel cosmoModel, const std::string model="LCDM", const bool unit=true)
	constructor using built-in cosmological models More...

	~Cosmology ()=default
	default destructor

Functions to get the private members of the class
double	value (const CosmologicalParameter parameter) const
	get the private member specified by the enum CosmologicalParameter More...

double	Omega_matter () const
	get the private member Cosmology::m_Omega_matter More...

double	Omega_baryon () const
	get the private member Cosmology::m_Omega_baryon More...

double	Omega_neutrinos () const
	get the private member Cosmology::m_Omega_neutrinos More...

double	massless_neutrinos () const
	get the private member Cosmology::m_massless_neutrinos More...

int	massive_neutrinos () const
	get the private member Cosmology::m_massive_neutrinos More...

double	Omega_DE () const
	get the private member Cosmology::m_Omega_DE More...

double	Omega_radiation () const
	get the private member Cosmology::m_Omega_radiation More...

double	Omega_k () const
	get the private member Cosmology::m_Omega_k More...

double	Omega_CDM () const
	get the private member Cosmology::m_Omega_CDM More...

double	H0 () const
	get the private member Cosmology::m_H0 More...

double	hh () const
	get the private member Cosmology::m_hh More...

double	t_H () const
	get the private member Cosmology::m_t_H More...

double	D_H () const
	get the private member Cosmology::m_D_H More...

double	sigma8 () const
	get the private member Cosmology::m_sigma8 More...

double	scalar_amp () const
	get the private member Cosmology::m_scalar_amp More...

double	scalar_pivot () const
	get the private member Cosmology::m_scalar_pivot More...

double	n_spec () const
	get the private member Cosmology::m_n_spec More...

double	w0 () const
	get the private member Cosmology::m_w0 More...

double	wa () const
	get the private member Cosmology::m_wa More...

double	RhoZero () const
	get the private member Cosmology::m_RhoZero More...

double	fNL () const
	get the private member Cosmology::m_fNL More...

int	type_NG () const
	get the private member Cosmology::m_type_NG More...

double	tau () const
	get the private member Cosmology::m_tau More...

double	rs () const
	get the sound horizon at recombination More...

double	Pk0_EH () const
	get the private member Cosmology::m_Pk0_EH More...

double	Pk0_CAMB () const
	get the private member Cosmology::m_Pk0_CAMB More...

double	Pk0_MPTbreeze () const
	get the private member Cosmology::m_Pk0_MPTbreeze More...

double	Pk0_CLASS () const
	get the private member Cosmology::m_Pk0_CLASS More...

std::string	model () const
	get the private member Cosmology::m_model More...

bool	unit () const
	get the private member Cosmology::m_unit More...

void	print_parameters () const
	print the values of the private members on the screen

Functions to set the private members of the class
void	set_parameter (const CosmologicalParameter parameter, const double value)
	set the value of one cosmological paramter More...

void	set_parameters (const std::vector< CosmologicalParameter > parameter, const std::vector< double > value)
	set the value of some cosmological paramters More...

void	set_Omega_all (const double OmegaB, const double OmegaCDM, const double OmegaNu, const double OmegaR, const double OmegaDE)
	set the value of \(\Omega_{\rm b}\), \(\Omega_{\rm cdm}\), \(\Omega_{\nu}\), \(\Omega_{\rm rad}\), \(\Omega_{\rm DE}\), and consequently the values of More...

void	set_Omega (const double Omega_matter=0.27)
	set the value of Ω_M, keeping Ω_DE=1-Ω_M-Ω_rad-Ω_k More...

void	set_OmegaB (const double Omega_baryon=0.046)
	set the value of Ω_b, keeping Ω_CDM=Ω_M-Ω_b More...

void	set_OmegaB_h2 (const double Omega_baryonh2=0.0222)
	set the value of Ω_b, keeping Ω_CDM=Ω_M-Ω_b More...

void	set_OmegaM (const double Omega_matter=0.27)
	set the value of Ω_M More...

void	set_OmegaDE (const double Omega_DE=0.73)
	set the value of Ω_DE More...

void	set_OmegaNu (const double Omega_neutrinos=0., const double massless_neutrinos=3.04, const int massive_neutrinos=0)
	set the value of Ω_ν More...

void	set_Omega_radiation (const double Omega_radiation)
	set the private member Cosmology::m_Omega_radiation More...

void	set_hh (const double hh=0.7, const bool warn=true)
	set the value of h More...

void	set_H0 (const double H0=70., const bool warn=true)
	set the value of H₀ More...

void	set_sigma8 (const double sigma8=-1.)
	set the value of σ₈ More...

void	set_scalar_amp (const double scalar_amp=2.46e-9)
	set the value of A_s More...

void	set_scalar_pivot (const double scalar_pivot=0.05)
	set the value of the scalar pivot More...

void	set_n_spec (const double n_spec)
	set the value of n_spec More...

void	set_w0 (const double w0=-1.)
	set the value of w₀ More...

void	set_wa (const double wa=0.)
	set the value of w_a More...

void	set_RhoZero (const double RhoZero=7.5e10)
	set the value of ρ₀ More...

void	set_fNL (const double fNL=0.)
	set the value of f_NL More...

void	set_type_NG (const int type_NG=1)
	set the value of the non-Gaussian shape More...

void	set_tau (const double tau=0.09)
	set the value of the τ More...

void	set_rs (const double rs=-1)
	set the value of the \(r_s\); More...

void	set_model (const std::string model="LCDM")
	set the cosmologial model used to compute distances More...

void	set_unit (const bool unit=true)
	set the value of unit More...

Functions to estimate general cosmological parameters
double	OmegaM (const double redshift=0.) const
	the matter density at a given redshift More...

double	OmegaDE (const double redshift=0.) const
	the dark energy density at a given redshift More...

double	OmegaR (const double redshift=0.) const
	the radiation density at a given redshift More...

double	OmegaR_zeq (const double z_eq=3395.) const
	the radiation density, as a function of the redshift of radiation-matter equality More...

double	OmegaNu (const double redshift=0.) const
	the neutrino density at a given redshift More...

double	OmegaK (const double redshift=0.) const
	the density of curvature energy at a given redshift More...

double	Omega (const double redshift=0.) const
	the cosmic density at a given redshift More...

double	Omega_neutrinos (const double Mnu) const
	the density of massive neutrinos, given the neutrino mass More...

double	neutrino_mass () const
	the total neutrino mass More...

double	rho_crit (const double redshift, const bool unit1=false) const
	the critical cosmic density More...

double	rho_m (const double redshift=0., const bool unit1=false, const bool nu=false) const
	the mean cosmic background density More...

double	Delta_c (const double redshift, const std::string author="BryanNorman") const
	the critical overdensity More...

double	M_vir (const double r_vir, const double redshift, const std::string author="BryanNorman", const bool unit1=false) const
	the virial mass, given the virial radius and the redshift More...

double	r_vir (const double M_vir, const double redshift, const std::string author="BryanNorman", const bool unit1=false) const
	the virial radius, given the virial mass and the redshift More...

double	w_CPL (const double redshift=0.) const
	the DE equation of state in the CPL parameterisation, as a function of redshift More...

double	f_DE (const double redshift=0.) const
	auxiliary function used to compute the Hubble function More...

double	EE (const double redshift=0.) const
	auxiliary function used to compute the Hubble function More...

double	EE_inv (const double redshift=0.) const
	inverse of the auxiliary function used to compute the Hubble function integrand of the comoving distance More...

double	EE_inv2 (const double redshift=0.) const
	inverse of the auxiliary function used to compute the Hubble function, integrand of the lookback time More...

double	EE_inv3 (const double aa) const
	inverse of the auxiliary function used to compute the Hubble function integrand of the cosmic time More...

double	HH (const double redshift=0.) const
	the Hubble function More...

double	DN (const double redshift, const double redshift_norm=0., const double prec=1.e-4) const
	the normalised amplitude of the growing mode at a given redshift, \(D(z)/D(0)\) More...

double	DD (const double redshift) const
	the amplitude of the growing mode at a given redshift, \(D(z)\) More...

double	gg (const double redshift=0.) const
	the linear growth factor at a given redshift, \(g(z)\) More...

double	sigma8 (const double redshift) const
	σ₈ at a given redshift More...

double	lookback_time (const double redshift=0.) const
	lookback time at a given redshift More...

double	cosmic_time (const double redshift=0.) const
	cosmic time at a given redshift More...

double	EE2 (const double redshift=0.) const
	auxiliary function used to compute the deceleration parameter More...

double	qq (const double redshift=0.) const
	the deceleration parameter at a given redshift More...

double	Hdot (const double redshift=0.) const
	derivative of the Hubble function at a given redshift More...

double	z_decoupling () const
	redshift at wich occurs baryon photon decoupling More...

double	z_drag () const
	redshift of drag epoch More...

double	z_acc () const
	redshift at which the Universe begins to accelerate More...

double	z_eq () const
	redshift of matter-dark energy equality More...

double	z_eq_rad (const double T_CMB=2.7255) const
	redshift of matter-radiation equality More...

double	sound_speed (const double redshift, const double T_CMB=2.7255) const
	the sound speed More...

double	rs_integrand (const double redshift, const double T_CMB=2.7255) const
	the sound horizon integrand More...

double	rs (const double redshift, const double T_CMB=2.7255) const
	the sound horizon More...

double	Mag_Volume_limited (const double z_max=1., const double mag_lim=-20.) const
	maximum absolute magnitude to have a volume-limited catalogue More...

double	Lum_bol (const double redshift=0., const double flux=1.) const
	bolometric luminosity More...

double	Redshift (const double d_c=1., const double z1_guess=0., const double z2_guess=10., const double prec=0.0001) const
	redshift at a given comoving distance More...

double	Redshift_LCDM (const double d_c=1., const double z1_guess=0., const double z2_guess=10., const bool go_fast=1, const double prec=0.0001) const
	redshift at a given comoving distance More...

double	Redshift (const double mm, const double redshift, const double ff, const std::string method_SS, const double wwf, const bool store_output=true, const std::string output_root="test") const
	redshift at a given wf More...

double	Redshift_time (const double time, const double z1_guess, const double z2_guess) const
	redshift at a given cosmic time More...

double	deltac (const double redshift) const
	spherical collapse density threshold at a given redshift More...

double	deltav_L (const double deltav_NL, const double b_eff, double slope=0.854, double offset=0.420) const
	Linear (under)density contrast. More...

double	deltav_NL (const double deltav=-2.71) const
	Non-Linear (under)density contrast. More...

double	r_rL (const double deltav=-2.71) const
	expansion factor More...

Functions to estimate cosmological distances and volumes
double	D_C (const double redshift) const
	the comoving line-of-sight distance at a given redshift More...

double	D_C_LCDM (const double redshift) const
	the comoving line-of-sight distance at a given redshift More...

void	D_C_table (const std::string file_table, const double z_min, const double z_max, const int step, std::vector< double > &Redshift, std::vector< double > &dc) const
	create a table of [redshift, comoving line-of-sight distance] More...

double	D_M (const double redshift) const
	the comoving transverse distance at a given redshift More...

double	D_A (const double redshift) const
	the angular diameter distance at a given redshift More...

double	D_A (const double z1, const double z2) const
	the angular diameter distance between objects at two redshifts More...

double	D_L (const double redshift) const
	the luminosity distance at a given redshift More...

double	D_V (const double redshift) const
	the average distance at a given redshift, used to rescale the correlation function More...

double	F_AP (const double redshift) const
	F_AP, the ALCOCK-PACZYNSKI distortion parameter. More...

double	Distance (const double redshift, const std::string distance_type) const
	the distance at a given redshift More...

double	Volume (const double z1, const double z2, const double Area) const
	comoving volume for a given redshift range and sky area More...

double	Volume (const double z1, const double z2, const double RA_min, const double RA_max, const double Dec_min, const double Dec_max) const
	comoving volume for a given redshift range and R.A.-Dec limits More...

double	Volume (const double zz) const
	total comoving volume from z=0 to z More...

double	max_redshift (const double Volume, const double Area, const double z_min) const
	maximum redshift for a given volume, sky area and minimum redshift More...

double	dV_dZdOmega (const double redshift, const bool angle_rad) const
	the derivative of the comoving volume, d²V/(dz*dΩ) at a given redshift More...

Functions to estimate the halo mass function and related quantities
std::string	create_grid_sigmaM (const std::string method_SS, const double redshift, const bool store_output=true, const std::string output_root="test", const std::string interpType="Linear", const double k_max=100., const std::string input_file=par::defaultString, const bool is_parameter_file=true) const
	auxiliary function to create a grid file with σ(M) More...

double	mass_function (const double Mass, const double redshift, const std::string model_MF, const std::string method_SS, const bool store_output=true, const std::string output_root="test", const double Delta=200., const std::string interpType="Linear", const int norm=-1, const double k_min=0.001, const double k_max=100., const double prec=1.e-2, const std::string input_file=par::defaultString, const bool is_parameter_file=true, const bool default_delta=true, const double delta_t=1.686)
	the mass function of dark matter haloes (filaments and sheets) More...

double	mass_function_fR (const double Mass, const double redshift, const std::string model_MF, const double f_R0=0., const bool store_output=true, const double Delta=200., const std::string interpType="Linear", const int norm=-1, const double k_min=0.001, const double k_max=100., const double prec=1.e-2, const std::string input_file=par::defaultString, const bool is_parameter_file=true, const bool default_delta=true, const double delta_t=1.686)
	the mass function of dark matter haloes in f(R) cosmologies (see Hu & Sawicki 2007) computed with the Boltzmann solver MGCAMB More...

double	mass_function_fast (const double Mass, const double redshift, const std::string model_MF, const std::string method_SS, const bool store_output=true, const std::string output_root="test", const double Delta=200., const std::string interpType="Linear", const int norm=-1, const double k_min=0.001, const double k_max=100., const double prec=1.e-2, const std::string input_file=par::defaultString, const bool is_parameter_file=true)
	the mass function of dark matter haloes (filaments and sheets) computed quickly using a grid More...

double	mass_function (const double Mass, const double Sigma, const double Dln_Sigma, const double redshift, const std::string model_MF, const bool store_output=true, const std::string output_root="test", const double Delta=200., const std::string interpType="Linear", const int norm=-1, const double k_min=0.001, const double k_max=100., const double prec=1.e-2, const std::string method_SS="CAMB", const std::string input_file=par::defaultString, const bool is_parameter_file=true)
	the mass function of dark matter haloes (filaments and sheets) computed quickly passing directly the mass variance and its derivative as inputs More...

double	mass_function (const double Mass, const double Sigma, const double Dln_Sigma, const double redshift, const double D_N, const std::string model_MF, const bool store_output=true, const std::string output_root="test", const double Delta=200., const std::string interpType="Linear", const int norm=-1, const double k_min=0.001, const double k_max=100., const double prec=1.e-2, const std::string method_SS="CAMB", const std::string input_file=par::defaultString, const bool is_parameter_file=true)
	the mass function of dark matter haloes (filaments and sheets) computed quickly passing directly the mass variance and its derivative as inputs More...

std::vector< double >	mass_function (const std::vector< double > Mass, const std::vector< double > Sigma, const std::vector< double > Dln_Sigma, const double redshift, const std::string model_MF, const bool store_output=true, const std::string output_root="test", const double Delta=200., const std::string interpType="Linear", const int norm=-1, const double k_min=0.001, const double k_max=100., const double prec=1.e-2, const std::string method_SS="CAMB", const std::string input_file=par::defaultString, const bool is_parameter_file=true)
	the mass function of dark matter haloes (filaments and sheets) computed quickly passing directly the mass variance and its derivative as inputs. This function takes vector in input and compute the mass function for the input masses More...

double	n_haloes (const double Mass_min, const double Mass_max, const double z_min, const double z_max, const bool angle_rad, const std::string model_MF, const std::string method_SS, const bool store_output=true, const std::string output_root="test", const double Delta=200, const std::string interpType="Linear", const double k_max=100., const std::string input_file=par::defaultString, const bool is_parameter_file=true)
	number of dark matter haloes per steradian or square degree, for a given redshift range More...

double	n_haloes (const double Mass_min, const double Mass_max, const double Volume, const double redshift, const std::string model_MF, const std::string method_SS, const int nbin_mass=0, const bool store_output=true, const std::string output_root="test", const double Delta=200., const std::string interpType="Linear", const int norm=-1, const double k_min=0.001, const double k_max=100., const double prec=1.e-2, const std::string input_file=par::defaultString, const bool is_parameter_file=true, const bool default_delta=true, const double delta_t=1.686)
	number of dark matter haloes per volume at fixed redshift More...

double	n_haloes_selection_function (const double Mass_min, const double Mass_max, const double z_min, const double z_max, const bool angle_rad, const std::string model_MF, const std::string method_SS, const std::string selection_function_file, const std::vector< int > column={}, const bool store_output=true, const std::string output_root="test", const double Delta=200, const bool isDelta_critical=false, const std::string interpType="Linear", const double k_max=100., const std::string input_file=par::defaultString, const bool is_parameter_file=true)
	number of dark matter haloes per steradian or square degree, for a given redshift range and with selection function defined on a grid More...

std::vector< double >	mass_function (const std::vector< double > mass, const double z_min, const double z_max, const std::string model_MF, const std::string method_SS, const bool store_output=true, const std::string output_root="test", const double Delta=200, const bool isDelta_critical=false, const std::string interpType="Linear", const double k_max=100., const std::string input_file=par::defaultString, const bool is_parameter_file=true)
	mass function for a range of masses More...

std::vector< double >	mass_function_selection_function_vector (const std::vector< double > mass, const double z_min, const double z_max, const std::string model_MF, const std::string method_SS, const std::string selection_function_file, const std::vector< int > column={}, const bool store_output=true, const std::string output_root="test", const double Delta=200, const bool isDelta_critical=false, const std::string interpType="Linear", const double k_max=100., const std::string input_file=par::defaultString, const bool is_parameter_file=true)
	mass function given a selection function More...

std::vector< double >	redshift_distribution_haloes (const double z_min, const double z_max, const int step_z, const double Area_degrees, const double Mass_min, const double Mass_max, const std::string model_MF, const std::string method_SS, const bool store_output=true, const std::string output_root="test", const double Delta=200, const bool isDelta_critical=false, const std::string interpType="Linear", const double k_max=100., const std::string input_file=par::defaultString, const bool is_parameter_file=true)
	redshift distribution of dark matter haloes More...

std::vector< double >	redshift_distribution_haloes_selection_function (const std::vector< double > redshift, const double Area_degrees, const double Mass_min, const double Mass_max, const std::string model_MF, const std::string method_SS, const std::string selection_function_file, const std::vector< int > column={}, const bool store_output=true, const std::string output_root="test", const double Delta=200, const bool isDelta_critical=false, const std::string interpType="Linear", const double k_max=100., const std::string input_file=par::defaultString, const bool is_parameter_file=true)
	redshift distribution of dark matter haloes, given a selection function More...

double	mean_redshift_haloes_selection_function (const double z_min, const double z_max, const double Mass_min, const double Mass_max, const std::string model_MF, const std::string method_SS, const std::string selection_function_file, const std::vector< int > column={}, const bool store_output=true, const std::string output_root="test", const double Delta=200, const bool isDelta_critical=false, const std::string interpType="Linear", const double k_max=100., const std::string input_file=par::defaultString, const bool is_parameter_file=true)
	the mean redshift of a dark matter haloe sample, given a selection function More...

double	MhaloMin (const int n_halo, const double Area, const bool angle_rad, const double z_min, const double z_max, const double Mmax, const double lgM1_guess, const double lgM2_guess, const std::string model_MF, const std::string method_SS, const bool store_output=true, const std::string output_root="test", const double Delta=200, const std::string interpType="Linear", const double k_max=100., const std::string input_file=par::defaultString, const bool is_parameter_file=true) const
	minimum halo mass, given the number of haloes in a given region of sky More...

double	converted_mass (const double mass, const cosmology::Cosmology cosmology, const double redshift, const double redshift_source=-1.) const
	convert a cluster mass estimated in a different cosmology More...

Functions to estimate the cosmic mass accretion history
double	pw (const double ww, const double ff, const std::string author) const
	differential distribution More...

double	pz (const double m0, const double z0, const double frac, const double redshift, const std::string model_model, const std::string method_SS, const bool store_output=true, const std::string output_root="test") const
	formation probability More...

double	cumPw (const double ww, const double ff, const std::string author) const
	cumulative distribution More...

void	medianwf (const double ff, const std::string model_model, std::vector< double > &wf) const
	median formation w More...

void	medianzf (const double ff, const double mass, const double z0, const std::string model_model, const std::string method_SS, std::vector< double > &zf, const bool store_output=true, const std::string output_root="test") const
	median formation z More...

double	wf (const double mm, const double redshift, const double ff, const double zf, const std::string method_SS, const bool store_output=true, const std::string output_root="test") const
	rescaled variable w as in Lacey and Coles 1993 More...

double	unevolved_mass_function (const double mass_accr) const
	the unevolved mass function More...

Functions to estimate the power spectrum and related quantities
double	As (const double sigma8) const
	amplitude of the curvature perturbations More...

double	sigma8_interpolated (const double redshift) const
	σ₈ More...

std::string	Pk_output_file (const std::string code, const bool NL, const double redshift, const bool run=0, const bool store_output=true, const std::string output_root="test", const double k_max=100., const std::string file_par=par::defaultString)
	return the path to the power spectrum output More...

void	run_CAMB (const bool NL, const double redshift, const std::string output_root=par::defaultString, const std::string output_dir=par::defaultString, const double k_max=100., const std::string file_par=par::defaultString) const
	run CAMB [http://camb.info/] More...

void	run_CAMB (std::vector< double > &lgkk, std::vector< double > &lgPk, const bool NL, const double redshift, const std::string output_root="test", const std::string output_dir=par::defaultString, const double k_max=100., const std::string file_par=par::defaultString) const
	run CAMB [http://camb.info/] and read the matter power spectrum More...

void	Table_PkCodes (const std::string code, const bool NL, std::vector< double > &lgkk, std::vector< double > &lgPk, const double redshift, const bool store_output=true, const std::string output_root="test", const double k_max=100., const std::string file_par=par::defaultString) const
	write or read the table where the dark matter power spectrum is stored More...

void	Table_PkCodes (const std::string code, const bool NL, std::vector< std::vector< double >> &lgkk, std::vector< std::vector< double >> &lgPk, const std::vector< double > redshift, const bool store_output=true, const std::string output_root="test", const double k_max=100., const std::string file_par=par::defaultString) const
	write or read the table where the dark matter power spectrum is stored More...

void	Table_XiCodes (const std::string code, const bool NL, std::vector< double > &rr, std::vector< double > &xi, const double redshift, const bool store_output, const std::string output_root, const double k_max, std::string file_par) const
	write or read the table where the dark matter two-point correlation function is stored More...

void	Pk_0 (const std::string method_Pk, const double redshift, const bool store_output=true, const std::string output_root="test", const double k_min=0.001, const double k_max=100., const double prec=1.e-2, const std::string file_par=par::defaultString)
	normalisation of the power spectrum More...

std::vector< double >	Pk_matter (const std::vector< double > kk, const std::string method_Pk, const bool NL, const double redshift, const bool store_output=true, const std::string output_root="test", const int norm=-1, const double k_min=0.001, const double k_max=100., const double prec=1.e-2, const std::string file_par=par::defaultString, const bool unit1=false)
	the dark matter power spectrum More...

std::vector< std::vector< double > >	Pk_matter (const std::vector< double > kk, const std::string method_Pk, const bool NL, const std::vector< double > redshift, const bool store_output=true, const std::string output_root="test", const int norm=-1, const double k_min=0.001, const double k_max=100., const double prec=1.e-2, const std::string file_par=par::defaultString, const bool unit1=false)
	the dark matter power spectrum More...

std::vector< double >	Pk_matter_Linear (const std::string method, const std::vector< double > kk, const double redshift, const bool store_output=true, const std::string output_root="test", const bool norm=1, const double prec=1.e-4)
	the dark matter linear power spectrum. More...

std::vector< double >	Pk_matter_NoWiggles_gaussian (const std::vector< double > kk, const std::vector< double > PkLin, const std::vector< double > PkApprox, const double lambda, const std::string method)
	the dark matter power spectrum without BAO wiggles. More...

std::vector< double >	Pk_matter_NoWiggles_bspline (const std::vector< double > kk, const std::vector< double > PkLin, const std::vector< double > PkApprox, const int order, const int nknots)
	the dark matter power spectrum without BAO wiggles. More...

std::vector< double >	Pk_matter_NoWiggles (const std::string method, const std::vector< double > kk, const double redshift, const std::string linear_method="CAMB", const int order=4, const int nknots=10, const double lambda=0.25, const bool store_output=true, const std::string output_root="test", const bool norm=1, const double prec=1.e-4)
	the dark matter power spectrum without BAO wiggles More...

std::vector< double >	Pk_matter_DeWiggled (const std::string linear_method, const std::string nowiggles_method, const std::vector< double > kk, const double redshift, const double sigma_NL, const int order=4, const int nknots=10, const double lambda=0.25, const bool store_output=true, const std::string output_root="test", const bool norm=1, const double prec=1.e-4)
	the dark matter power spectrum, de-wiggled (see e.g. Anderson et al 2014) More...

void	remove_output_Pk_tables (const std::string code, const bool NL, const double redshift, const std::string output_root="test") const
	remove the output generated by the methods CAMB, MPTbreeze or CLASS More...

double	sigma2R (const double radius, const std::string method_Pk, const double redshift, const bool store_output=true, const std::string output_root="test", const std::string interpType="Linear", const double k_max=100., const std::string input_file=par::defaultString, const bool is_parameter_file=true, const bool unit1=false) const
	the mass variance, \(\sigma^2(R)\) More...

double	sigma2M (const double mass, const std::string method_Pk, const double redshift, const bool store_output=true, const std::string output_root="test", const std::string interpType="Linear", const double k_max=100., const std::string input_file=par::defaultString, const bool is_parameter_file=true, const bool unit1=false) const
	the mass variance, \(\sigma^2(M)\) More...

double	dnsigma2R (const int nd, const double radius, const std::string method_Pk, const double redshift, const bool store_output=true, const std::string output_root="test", const std::string interpType="Linear", const double k_max=100., const std::string input_file=par::defaultString, const bool is_parameter_file=true, const bool unit1=false) const
	the nth-order derivative of the mass variance, \({\rm d}^n\sigma^2(R)/{\rm d}R^n\) More...

double	dnsigma2M (const int nd, const double mass, const std::string method_Pk, const double redshift, const bool store_output=true, const std::string output_root="test", const std::string interpType="Linear", const double k_max=100., const std::string input_file=par::defaultString, const bool is_parameter_file=true, const bool unit1=false) const
	the first derivative of the mass variance, \({\rm d}^n\sigma^2(M)/{\rm d}M^n\) More...

Functions to estimate the halo density profile
double	concentration_NFW_Duffy (const double Mass, const double redshift, const std::string halo_def="vir") const
	the halo concentration-mass relation for NFW prfile and Duffy model More...

double	c_vir (const double c200, const double redshift, const std::string author="BryanNorman") const
	virial halo concentration given \(c_{200}\) More...

Functions to estimate the two-point correlation function, bias and related quantities
double	xi_matter (const double rr, const std::string method_Pk, const bool NL, const double redshift, const bool store_output=true, const std::string output_root="test", const int norm=-1, const double k_min=0.001, const double k_max=100., const double aa=0., const bool GSL=false, const double prec=1.e-2, const std::string file_par=par::defaultString)
	the dark matter two-point correlation function More...

double	wtheta_DM (const double theta, const std::vector< double > zz, const std::vector< double > phiz, const std::string interpolationMethod, const CoordinateUnits coordUnits=CoordinateUnits::_degrees_, const bool GSL=false, const std::string method_Pk="CAMB", const bool NL=false, const bool store_output=true, const std::string output_root="test", const int norm=-1, const double k_min=1.e-4, const double k_max=100, const double prec=1.e-2, const std::string file_par=par::defaultString)
	the dark matter angular two-point correlation function More...

double	wtheta_DM (const double theta, const std::vector< double > kk, const std::vector< double > Pk, const std::vector< double > zz, const std::vector< double > nz, const std::vector< double > phiz, const std::string interpolationType="Spline", const CoordinateUnits coordUnits=CoordinateUnits::_degrees_, const bool GSL=false, const double redshift_Pk=0)
	the dark matter angular two-point correlation function More...

std::vector< double >	C_l_DM (const int lmax, const std::vector< double > zz, const std::vector< double > phiz, const std::string interpolationMethod, const std::string method_Pk="CAMB", const bool store_output=true, const std::string output_root="test", const int norm=-1, const double k_min=1.e-4, const double k_max=100, const double prec=1.e-2, const std::string file_par=par::defaultString)
	the dark matter angular linear power spectrum \(C_l\). More...

double	xi_matter_DeWiggle (const double rr, const double redshift, const double sigma_NL, const bool store_output=true, const std::string output_root="test", const bool norm=1, const double k_min=0.001, const double k_max=100., const double aa=1., const double prec=1.e-2)
	the dark matter two-point correlation function, de-wiggled (see e.g. Anderson et al 2014) More...

void	get_xi (std::vector< double > &rr, std::vector< double > &Xi, const std::string method_Pk, const double redshift, const bool store_output=true, const std::string output_root="test", const bool xiType=0, const double k_star=-1., const bool xiNL=0, const int norm=-1, const double r_min=0.1, const double r_max=150., const double k_min=0.001, const double k_max=100., const double aa=0., const bool GSL=false, const double prec=1.e-2, const std::string file_par=par::defaultString)
	get the dark matter two-point correlation function More...

void	get_barred_xi (std::vector< double > rr, std::vector< double > Xi, std::vector< double > &Xi_, std::vector< double > &Xi__, const std::string method_Pk, const double redshift, const bool xiType=0, const double k_star=-1., const bool xiNL=0, const int norm=-1, const double r_min=0.1, const double r_max=150., const double k_min=0.001, const double k_max=100., const double aa=0., const double prec=1.e-2, const std::string file_par=par::defaultString) const
	get the barred dark matter correlation functions More...

double	wp_DM (const double rp, const std::string method_Pk, const bool NL, const double redshift, const double pimax, const bool store_output=true, const std::string output_root="test", const int norm=-1, const double r_min=1.e-3, const double r_max=350., const double k_min=0.001, const double k_max=100., const double aa=0., const bool GSL=false, const double prec=1.e-2, const std::string file_par=cbl::par::defaultString)
	the dark matter projected correlation function More...

double	k_star (const std::string method_Pk, const double redshift, const bool store_output=true, const std::string output_root="test", const double k_max=100., const std::string file_par=par::defaultString) const
	the k_* parameter More...

double	sigmaR_DM (const double RR, const int corrType, const std::string method_Pk, const double redshift, const double pimax=40, const bool store_output=true, const std::string output_root="test", const bool NL=1, const int norm=-1, const double r_min=1.e-3, const double r_max=350., const double k_min=0.001, const double k_max=100., const double aa=0., const bool GSL=false, const double prec=1.e-2, const std::string file_par=par::defaultString)
	the dark matter rms mass fluctuation More...

double	sigma8_Pk (const std::string method_Pk, const double redshift, const bool store_output=true, const std::string output_root="test", const bool NL=0, const double k_min=0.001, const double k_max=100., const double prec=1.e-2, const std::string file_par=par::defaultString) const
	the dark matter rms mass fluctuation within 8 Mpc/h More...

double	bias_halo (const double Mass, const double redshift, const std::string author, const std::string method_SS, const bool store_output=true, const std::string output_root="test", const std::string interpType="Linear", const double Delta=200., const double kk=-1., const int norm=-1, const double k_min=0.001, const double k_max=100., const double prec=1.e-2, const std::string input_file=par::defaultString, const bool is_parameter_file=true)
	bias of dark matter haloes More...

double	bias_halo (const double Mass, const double Sigma, const double redshift, const std::string model_bias, const bool store_output=true, const std::string output_root="test", const std::string interpType="Linear", const double Delta=200., const double kk=-1., const int norm=-1, const double k_min=0.001, const double k_max=100., const double prec=1.e-2, const std::string method_SS="CAMB", const std::string input_file=par::defaultString, const bool is_parameter_file=true)
	bias of dark matter haloes More...

double	bias_halo (const double Mass, const double Sigma, const double redshift, const double DN, const std::string model_bias, const bool store_output=true, const std::string output_root="test", const std::string interpType="Linear", const double Delta=200., const double kk=-1., const int norm=-1, const double k_min=0.001, const double k_max=100., const double prec=1.e-2, const std::string method_SS="CAMB", const std::string input_file=par::defaultString, const bool is_parameter_file=true)
	bias of dark matter haloes More...

std::vector< double >	bias_halo (const std::vector< double > Mass, const std::vector< double > Sigma, const double redshift, const std::string model_bias, const bool store_output=true, const std::string output_root="test", const std::string interpType="Linear", const double Delta=200., const double kk=-1., const int norm=-1, const double k_min=0.001, const double k_max=100., const double prec=1.e-2, const std::string method_SS="CAMB", const std::string input_file=par::defaultString, const bool is_parameter_file=true)
	bias of dark matter haloes, for a vector of masses More...

double	bias_eff (const double Mass_min, const double Mass_max, const double redshift, const std::string model_bias, const std::string model_MF, const std::string method_SS, const bool store_output=true, const std::string output_root="test", const double Delta=200., const double kk=-1., const std::string interpType="Linear", const int norm=-1, const double k_min=0.001, const double k_max=100., const double prec=1.e-2, const std::string input_file=par::defaultString, const bool is_parameter_file=true)
	the effective bias of dark matter haloes, with masses in a given range and at a given mean redshift More...

double	bias_eff (const std::vector< double > MM, const std::vector< double > MF, const double redshift, const std::string model_bias, const std::string method_SS, const bool store_output=true, const std::string output_root="test", const double Delta=200., const double kk=-1., const std::string interpType="Linear", const int norm=-1, const double k_min=0.001, const double k_max=100., const double prec=1.e-2, const std::string input_file=par::defaultString, const bool is_parameter_file=true)
	effective bias of dark matter haloes, computed by averaging over the bias of a given set of haloes More...

std::vector< double >	bias_eff_mass_grid (const std::vector< double > MM, const std::vector< double > redshift, const std::string model_bias, const std::string method_SS, const std::string meanType="mean_bias", const bool store_output=true, const std::string output_root="test", const double Delta_crit=200., const double kk=-1., const std::string interpType="Linear", const int norm=-1, const double k_min=0.001, const double k_max=100., const double prec=1.e-2, const std::string input_file=par::defaultString, const bool is_parameter_file=true)
	effective bias of dark matter haloes, computed by averaging the bias of a set of haloes, with the mass variance estimated from a grid More...

std::vector< double >	bias_eff_mass (const std::vector< double > MM, const std::vector< double > redshift, const std::string model_bias, const std::string method_SS, const std::string meanType="mean_bias", const bool store_output=true, const std::string output_root="test", const double Delta=200., const double kk=-1., const std::string interpType="Linear", const int norm=-1, const double k_min=0.001, const double k_max=100., const double prec=1.e-2, const std::string input_file=par::defaultString, const bool is_parameter_file=true)
	effective bias of dark matter haloes, computed by averaging the bias of a set of haloes More...

std::vector< double >	bias_eff_mass (const std::vector< double > mass, const std::vector< double > mass_grid, const std::vector< double > redshift, const std::string model_bias, const std::string method_SS, const std::string meanType="mean_bias", const bool store_output=true, const std::string output_root="test", const double Delta=200., const double kk=-1., const std::string interpType="Linear", const int norm=-1, const double k_min=0.001, const double k_max=100., const double prec=1.e-2, const std::string input_file=par::defaultString, const bool is_parameter_file=true)
	effective bias of dark matter haloes, computed by averaging the bias of a set of haloes, interpolating the mass variance on a grid More...

void	generate_bias_eff_grid_one_cosmopar (std::vector< double > &parameter, std::vector< double > &bias_eff, const std::string dir_output, const std::string file_bias_eff_grid, const cbl::cosmology::CosmologicalParameter cosmoPar, const double min_par, const double max_par, const int nbin_par, const std::vector< double > mass, const std::vector< double > mass_grid, const std::vector< double > redshift, const std::string model_bias, const std::string method_SS, const std::string meanType="mean_bias", const bool store_output=true, const std::string output_root="test", const double Delta_crit=200., const double kk=-1., const std::string interpType="Linear", const int norm=-1, const double k_min=0.001, const double k_max=100., const double prec=1.e-2, const std::string input_file=par::defaultString, const bool is_parameter_file=true, const cbl::cosmology::Cosmology cosmology_mass={}, const std::vector< double > redshift_source={})
	compute the effective bias of dark matter haloes, by averaging the bias of a set of haloes, interpolating the mass variance on a grid of masses and of one input cosmological parameter; this function is used when modelling the two-point correlation function More...

void	generate_bias_eff_grid_one_cosmopar (std::vector< double > &parameter, std::vector< double > &bias_eff, const std::string dir_output, const std::string file_bias_eff_grid, const cbl::cosmology::CosmologicalParameter cosmoPar, const double min_par, const double max_par, const int nbin_par, const double redshift, const double Mass_min, const double Mass_max, const std::string model_bias, const std::string model_MF, const std::string method_SS, const std::string selection_function_file, const std::vector< int > column={}, const double alpha=1., const bool store_output=true, const std::string output_root="test", const double Delta_crit=200., const double kk=-1., const std::string interpType="Linear", const int norm=-1, const double k_min=0.001, const double k_max=100., const double prec=1.e-2, const std::string input_file=par::defaultString, const bool is_parameter_file=true)
	effective bias of dark matter haloes, computed by weighting on the selection function on a grid of one input cosmological parameter; this function is used when modelling the two-point correlation function More...

void	generate_bias_eff_grid_two_cosmopars (std::vector< double > &parameter1, std::vector< double > &parameter2, std::vector< std::vector< double >> &bias_eff, const std::string dir_output, const std::string file_bias_eff_grid, const cbl::cosmology::CosmologicalParameter cosmoPar1, const double min_par1, const double max_par1, const int nbin_par1, const cbl::cosmology::CosmologicalParameter cosmoPar2, const double min_par2, const double max_par2, const int nbin_par2, const std::vector< double > mass, const std::vector< double > mass_grid, const std::vector< double > redshift, const std::string model_bias, const std::string method_SS, const std::string meanType="mean_bias", const bool store_output=true, const std::string output_root="test", const double Delta=200., const double kk=-1., const std::string interpType="Linear", const int norm=-1, const double k_min=0.001, const double k_max=100., const double prec=1.e-2, const std::string input_file=par::defaultString, const bool is_parameter_file=true, const cbl::cosmology::Cosmology cosmology_mass={}, const std::vector< double > redshift_source={})
	effective bias of dark matter haloes, computed by averaging the bias of a set of haloes, interpolating the mass variance on a grid of masses and two input cosmological parameters; this function is used when modelling the two-point correlation function More...

std::vector< double >	bias_eff_selection_function (const glob::FuncGrid interp_sigma, const glob::FuncGrid interp_DnSigma, const glob::FuncGrid interp_SF, const double Mass_min, const double Mass_max, const std::vector< double > redshift, const std::string model_bias, const std::string model_MF, const std::string method_SS, const double alpha=1., const bool store_output=true, const std::string output_root="test", const double Delta_crit=200., const double kk=-1., const std::string interpType="Linear", const int norm=-1, const double k_min=0.001, const double k_max=100., const double prec=1.e-2, const std::string input_file=par::defaultString, const bool is_parameter_file=true)
	effective bias of dark matter haloes, computed using a given selection function; σ(mass) and dlnσ/dM are provided in input More...

std::vector< double >	bias_eff_selection_function (const glob::FuncGrid interp_sigma, const glob::FuncGrid interp_DnSigma, const glob::FuncGrid2D interp_SF, const double Mass_min, const double Mass_max, const std::vector< double > redshift, const std::string model_bias, const std::string model_MF, const std::string method_SS, const double alpha=1., const bool store_output=true, const std::string output_root="test", const double Delta_crit=200., const double kk=-1., const std::string interpType="Linear", const int norm=-1, const double k_min=0.001, const double k_max=100., const double prec=1.e-2, const std::string input_file=par::defaultString, const bool is_parameter_file=true)
	effective bias of dark matter haloes, computed using a given selection function; σ(mass) and dlnσ/dM are provided in input More...

std::vector< double >	bias_eff_selection_function (const double Mass_min, const double Mass_max, const std::vector< double > redshift, const std::string model_bias, const std::string model_MF, const std::string method_SS, const std::string selection_function_file, const std::vector< int > column={}, const double alpha=1., const bool store_output=true, const std::string output_root="test", const double Delta_crit=200., const double kk=-1., const std::string interpType="Linear", const int norm=-1, const double k_min=0.001, const double k_max=100., const double prec=1.e-2, const std::string input_file=par::defaultString, const bool is_parameter_file=true)
	effective bias of dark matter haloes, computed using a given selection function More...

Functions to model redshift-space distortions
double	linear_growth_rate (const double redshift, const double prec=1.e-4) const
	the linear growth rate at a given redshift, \(f(z)\) More...

double	fsigma8 (const double redshift, const std::string method_Pk, const bool store_output=true, const std::string output_root="test", const bool NL=false, const double k_min=0.001, const double k_max=100., const double prec=1.e-2, const std::string file_par=par::defaultString) const
	f*σ₈: the linear growth rate times the dark matter rms mass fluctuation within 8 Mpc/h More...

double	beta (const double redshift, const double bias) const
	the specific growth rate β More...

double	error_beta (const double redshift, const double bias, const double err_bias) const
	the error on the specific growth rate β More...

double	beta (const double Mass_min, const double Mass_max, const double redshift, const std::string model_bias, const std::string model_MF, const std::string method_SS, const bool store_output=true, const std::string output_root="test", const double Delta=200., const double kk=-1., const std::string interpType="Linear", const int norm=-1, const double k_min=0.001, const double k_max=100., const double prec=1.e-2, const std::string input_file=par::defaultString, const bool is_parameter_file=true)
	the error on the specific growth rate β More...

double	error_beta (const double Mass_min, const double Mass_max, const double redshift, const std::string model_bias, const std::string model_MF, const std::string method_SS, const double err_bias, const bool store_output=true, const std::string output_root="test", const double Delta=200., const double kk=-1., const std::string interpType="Linear", const int norm=-1, const double k_min=0.001, const double k_max=100., const double prec=1.e-2, const std::string input_file=par::defaultString, const bool is_parameter_file=true)
	the specific growth rate β More...

double	beta (const std::vector< double > MM, const std::vector< double > MF, const double redshift, const std::string model_bias, const std::string method_SS, const bool store_output=true, const std::string output_root="test", const double Delta=200., const double kk=-1., const std::string interpType="Linear", const int norm=-1, const double k_min=0.001, const double k_max=100., const double prec=1.e-2, const std::string input_file=par::defaultString, const bool is_parameter_file=true)
	the specific growth rate β More...

double	error_beta (const std::vector< double > MM, const std::vector< double > MF, const double redshift, const std::string model_bias, const std::string method_SS, const double err_bias, const bool store_output=true, const std::string output_root="test", const double Delta=200., const double kk=-1., const std::string interpType="Linear", const int norm=-1, const double k_min=0.001, const double k_max=100., const double prec=1.e-2, const std::string input_file=par::defaultString, const bool is_parameter_file=true)
	the error on the specific growth rate β More...

double	error_beta_measured (const double Volume, const double density, const double Mass_min, const double Mass_max, const double redshift, const std::string model_bias, const std::string model_MF, const std::string method_SS, const bool store_output=true, const std::string output_root="test", const double Delta=200., const double kk=-1., const std::string interpType="Linear", const int norm=-1, const double k_min=0.001, const double k_max=100., const double prec=1.e-2, const std::string input_file=par::defaultString, const bool is_parameter_file=true)
	the error on the specific growth rate β from Bianchi et al. 2012 More...

double	quadrupole (const double Mass_min, const double Mass_max, const double redshift, const std::string model_bias, const std::string model_MF, const std::string method_SS, const bool store_output=true, const std::string output_root="test", const double Delta=200., const double kk=-1., const std::string interpType="Linear", const int norm=-1, const double k_min=0.001, const double k_max=100., const double prec=1.e-2, const std::string input_file=par::defaultString, const bool is_parameter_file=true)
	the normalised quadrupole Q More...

double	quadrupole (const std::vector< double > MM, const std::vector< double > MF, const double redshift, const std::string model_bias, const std::string method_SS, const bool store_output=true, const std::string output_root="test", const double Delta=200., const double kk=-1., const std::string interpType="Linear", const int norm=-1, const double k_min=0.001, const double k_max=100., const double prec=1.e-2, const std::string input_file=par::defaultString, const bool is_parameter_file=true)
	the normalised quadrupole Q More...

double	square_bulk_flow (const double rr, const double k_int_min, const std::string method_Pk, const double redshift, const bool store_output=true, const std::string output_root="test", const double k_min=0.001, const double k_max=100., const double prec=1.e-2, const std::string file_par=par::defaultString)
	the mean square bulk flow More...

double	square_bulk_flow_Table (const double rr, const double k_int_min, const std::vector< double > lgkk, const std::vector< double > lgPk, const double redshift) const
	the mean square bulk flow More...

double	square_velocity_dispersion (const double rr, const double k_int_min, const std::string method_Pk, const double redshift, const bool store_output=true, const std::string output_root="test", const double k_min=0.001, const double k_max=100., const double prec=1.e-2, const std::string file_par=par::defaultString)
	the mean square velocity dispersion More...

double	CMN (const double rr, const double k_int_min, const std::string method_Pk, const double redshift, const bool store_output=true, const std::string output_root="test", const double k_max=100., const std::string file_par=par::defaultString) const
	the Cosmic Mach Number More...

double	Sn_PT (const int nn, const double RR, const std::string method_SS, const bool store_output=true, const std::string output_root="test", const std::string interpType="Linear", const double k_max=100., const std::string input_file=par::defaultString, const bool is_parameter_file=true) const
	the hierarchical moments S_n More...

double	Sigman_PT (const int nn, const double RR, const std::string method_SS, const bool store_output=true, const std::string output_root="test", const std::string interpType="Linear", const double k_max=100., const std::string input_file=par::defaultString, const bool is_parameter_file=true) const
	the deprojected hierarchical moments Σ_n More...

double	xi0_Kaiser (const double rad, const double f_sigma8, const double bias_sigma8, const std::string method_Pk, const double redshift, const bool store_output=true, const std::string output_root="test", const bool xiType=0, const double k_star=-1., const bool NL=false, const int norm=-1, const double r_min=0.1, const double r_max=150., const double k_min=0.001, const double k_max=100., const double aa=0., const bool GSL=false, const double prec=1.e-2, const std::string file_par=par::defaultString)
	monopole of the redshift-space two-point correlation function in the Kaiser limit More...

std::vector< double >	xi0_Kaiser (const std::vector< double > rad, const double bias, const std::string method_Pk, const double redshift, const bool store_output=true, const std::string output_root="test", const bool NL=false, const int norm=-1, const double k_min=0.001, const double k_max=100., const double prec=1.e-2, const std::string file_par=par::defaultString)
	monopole of the redshift-space two-point correlation function in the Kaiser limit More...

double	xi2D_dispersionModel (const double rp, const double pi, const double f_sigma8, const double bias_sigma8, const double sigmav, const std::string method_Pk, const double redshift, const int FV, const bool NL, std::vector< double > rr, std::vector< double > &Xi, std::vector< double > &Xi_, std::vector< double > &Xi__, const bool store_output=true, const std::string output_root="test", const int index=-1, const bool bias_nl=0, const double bA=-1., const bool xiType=0, const double k_star=-1., const bool xiNL=0, const double v_min=-3000., const double v_max=3000., const int step_v=500, const int norm=-1, const double r_min=0.1, const double r_max=150., const double k_min=0.001, const double k_max=100., const double aa=0., const bool GSL=false, const double prec=1.e-2, const std::string file_par=par::defaultString)
	2D correlation function, ξ(r_p,π), predicted by the dispersion model More...

double	xi_star (const double rr, const double redshift, const bool store_output=true, const std::string output_root="test", const double k_star=-1., const double k_min=0.001, const double k_max=100., const double prec=1.e-2, const std::string file_par=par::defaultString)
	the function ξ_* of the Chuang & Wang 2012 model More...

double	xisnl_gnw (const double rp, const double pi, const double f_sigma8, const double bias_sigma8, const double bA, const double redshift, std::vector< double > rr, std::vector< double > Xi, std::vector< double > &Xi_, std::vector< double > &Xi__, const bool store_output=true, const std::string output_root="test")
	the function ξ_g,nw(s) of the Chuang & Wang 2012 model More...

double	xis_gBAO (const double rp, const double pi, const double f_sigma8, const double bias_sigma8, const double redshift, std::vector< double > rr, std::vector< double > Xi, std::vector< double > &Xi_, std::vector< double > &Xi__, const bool store_output=true, const std::string output_root="test", const double k_star=-1., const double x_min=-3000., const double x_max=3000., const int step_x=500)
	the function ξ_g,BAO(s) of the Chuang & Wang 2012 model More...

double	xi2D_CW (const double rp, const double pi, const double beta, const double bias_lin, const double bA, const double sigmav0, const double cmu, const double cs1, const double cs2, const double redshift, std::vector< double > rr1, std::vector< double > Xi1, std::vector< double > rr2, std::vector< double > Xi2, std::vector< double > &Xi1_, std::vector< double > &Xi1__, std::vector< double > &Xi2_, std::vector< double > &Xi2__, const bool store_output=true, const std::string output_root="test", const bool BAO=1, const bool xiType=0, const double k_star=-1, const bool xiNL=0, const double r_min=0.1, const double r_max=150., const double v_min=-3000., const double v_max=3000., const int step_v=500, const double k_min=0.001, const double k_max=100., const double x_min=-3000., const double x_max=3000., const int step_x=500, const double aa=0., const bool GSL=false, const double prec=1.e-2, const std::string file_par=par::defaultString)
	2D correlation function, ξ(r_p,π), predicted by the Chuang & Wang model More...

Functions to model baryon acoustic oscillations
double	rs (const std::string method_Pk, const double T_CMB=par::TCMB) const
	the sound horizon at the drag epoch r_s(z_d), valid choices for method_Pk are: EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html], CAMB [http://camb.info/] More...

double	rs_EH (const double T_CMB=par::TCMB) const
	the sound horizon at the drag epoch predicted by Eisentein & Hu 1998 More...

double	rs_CAMB () const
	the sound horizon at the drag epoch estimated with CAMB [http://camb.info/], analytical formula by Aubourg et al. 2014 More...

double	ys (const double redshift, const std::string method_Pk, const double T_CMB=par::TCMB) const
	the fiducial cosmology independent ratio r_s/D_V, valid choices for method_Pk are: EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html], CAMB [http://camb.info/] More...

double	Az (const double redshift) const
	the acoustic parameter More...

std::vector< double >	linear_point (const double redshift, const double rmin=60., const double rmax=150., const int nbinr=100, const std::string interpType="Spline")
	the linear point More...

Functions to model cosmological quantities in non-Gaussian cosmologies
double	Am (const std::string method_Pk, const bool store_output=true, const std::string output_root="test", const int norm=-1, const double k_min=0.001, const double k_max=100., const double prec=1.e-2, const std::string file_par=par::defaultString)
	the amplitude of the matter power spectrum More...

double	potential_spectral_amplitude (const std::string method_Pk, const bool store_output=true, const std::string output_root="test", const int norm=-1, const double k_min=0.001, const double k_max=100., const double prec=1.e-2, const std::string file_par=par::defaultString)
	the potential spectral amplitude More...

double	bispectrum (const std::vector< double > kk, const std::string method_Pk, const bool store_output=true, const std::string output_root="test", const int norm=-1, const double k_min=0.001, const double k_max=100., const double prec=1.e-2, const std::string file_par=par::defaultString)
	the bispectrum More...

double	mrk (const double kk, const double mass, const std::string method_Pk, const bool store_output=true, const std::string output_root="test", const int norm=-1, const double k_min=0.001, const double k_max=100., const double prec=1.e-2, const std::string file_par=par::defaultString)
	auxiliary function to estimate cosmological quantities in non-Gaussian cosmologies More...

double	frk (const double kk, const double mass, const std::string method_Pk, const bool store_output=true, const std::string output_root="test", const std::string interpType="Linear", const int norm=-1, const double k_min=0.001, const double k_max=100., const double prec=1.e-2, const std::string input_file=par::defaultString, const bool is_parameter_file=true)
	auxiliary function to estimate cosmological quantities in non-Gaussian cosmologies More...

double	bias_correction (const double kk, const double mass, const std::string method_Pk, const bool store_output=true, const std::string output_root="test", const std::string interpType="Linear", const int norm=-1, const double k_min=0.001, const double k_max=100., const double prec=1.e-2, const std::string input_file=par::defaultString, const bool is_parameter_file=true)
	correction to the halo bias in non-Gaussian cosmologies More...

double	skewness (const double mass, const std::string method_Pk, const bool store_output=true, const std::string output_root="test", const std::string interpType="Linear", const int norm=-1, const double k_min=0.001, const double k_max=100., const double prec=1.e-2, const std::string input_file=par::defaultString, const bool is_parameter_file=true)
	the skewness More...

double	dskewnessdM (const double mass, const std::string method_Pk, const bool store_output=true, const std::string output_root="test", const std::string interpType="Linear", const int norm=-1, const double k_min=0.001, const double k_max=100., const double prec=1.e-2, const std::string input_file=par::defaultString, const bool is_parameter_file=true)
	the derivative of the skewness, ds/dM More...

double	MF_correction (const double mass, const double redshift, const std::string method_Pk, const bool store_output=true, const std::string output_root="test", const std::string interpType="Linear", const int norm=-1, const double k_min=0.001, const double k_max=100., const double prec=1.e-2, const std::string input_file=par::defaultString, const bool is_parameter_file=true)
	correction to the halo mass in non-Gaussian cosmologies More...

Functions to estimate the void size function
double	f_nu (const double SS, const double del_v, const double del_c) const
	\(f_{\ln \sigma}(\sigma)\) (approximation) More...

double	size_function (const double RV, const double redshift, const std::string model, const double b_eff, double slope=0.854, double offset=0.420, const double deltav_NL=-0.795, const double del_c=1.69, const std::string method_Pk="EisensteinHu", const bool store_output=true, const std::string output_root="test", const std::string interpType="Linear", const double k_max=100., const std::string input_file=par::defaultString, const bool is_parameter_file=true) const
	the void size function More...

std::vector< double >	size_function (const std::vector< double > RV, const double redshift, const std::string model, const double b_eff, double slope=0.854, double offset=0.420, const double deltav_NL=-0.795, const double del_c=1.69, const std::string method_Pk="EisensteinHu", const bool store_output=true, const std::string output_root="test", const std::string interpType="Linear", const double k_max=100., const std::string input_file=par::defaultString, const bool is_parameter_file=true) const
	the void size function More...

std::vector< std::vector< double > >	Nvoids (const double min_r, const double max_r, const int num_bins, const double mean_z, const double Volume, const std::string model, const double b_eff, double slope=0.854, double offset=0.420, const double deltav_NL=-0.795, const double del_c=1.69, const std::string method_Pk="EisensteinHu", const bool store_output=true, const std::string output_root="test", const std::string interpType="Linear", const double k_max=100., const std::string input_file=par::defaultString, const bool is_parameter_file=true) const
	number of voids computed from the void size function model for bins of radii spaced in log scale and for a specified survey/simulation volume More...

std::vector< std::vector< double > >	Nvoids (const double min_r, const double max_r, const int num_bins, const double min_z, const double max_z, const double mean_z, const double Area, const std::string model, const double b_eff, double slope=0.854, double offset=0.420, const double deltav_NL=-0.795, const double del_c=1.69, const std::string method_Pk="EisensteinHu", const bool store_output=true, const std::string output_root="test", const std::string interpType="Linear", const double k_max=100., const std::string input_file=par::defaultString, const bool is_parameter_file=true) const
	number of voids computed from the void size function model for bins of radii spaced in log scale. The considered volume is computed from a (fraction of) a sphere shell, included in between two different redshifts More...

double	size_function (const double RV, const double redshift, const std::string model_mf, const double del_v, const std::string model_sf, const std::string method_Pk="EisensteinHu", const bool store_output=true, const std::string output_root="test", const double Delta=200., const std::string interpType="Linear", const int norm=-1, const double k_min=0.001, const double k_max=100., const double prec=1.e-2, const std::string input_file=par::defaultString, const bool is_parameter_file=true)
	the void size function More...

std::vector< double >	AP_corr (const cbl::cosmology::Cosmology cosm_true, const std::vector< double > redshift)
	Supplementary function to compute a correction factor to apply to the void size function, to predict the measured abundance of voids affected by geometrical distortions (Alcock-Paczyński change of volume). These are caused by the assumption of a fiducial cosmology different from the true one, see Correa et al. 2020 (https://arxiv.org/pdf/2007.12064.pdf) More...

Functions to estimate the multipoles/wedges covariance matrix
std::vector< std::vector< double > >	XiMultipoles (const int nbins, const double rMin, const double rMax, const std::vector< double > kk, const std::vector< double > Pk0, const std::vector< double > Pk2, const std::vector< double > Pk4, const int IntegrationMethod=1)
	the first three non-null multipoles of the two-point correlation function More...

std::vector< std::vector< double > >	XiMonopole_covariance (const int nbins, const double rMin, const double rMax, const double nn, const double Volume, const std::vector< double > kk, const std::vector< double > Pk0, const int IntegrationMethod=1)
	the covariance matrix of the first three non-null multipoles of the two-point correlation function More...

std::vector< std::vector< double > >	XiMultipoles_covariance (const int nbins, const double rMin, const double rMax, const double nn, const double Volume, const std::vector< double > kk, const std::vector< double > Pk0, const std::vector< double > Pk2, const std::vector< double > Pk4, const int IntegrationMethod=1)
	the covariance matrix of the first three non-null multipole moments of the two-point correlation function More...

Functions to estimate the non-linear power spectrum
double	F2 (const double k, const double q, const double kq)
	function used to estimate the non-linear power spectrum More...

double	G2 (const double k, const double q, const double kq)
	function used to estimate the non-linear power spectrum More...

double	f_k (const double k, const std::shared_ptr< cbl::glob::FuncGrid > PkLin, const double qmin, const double qmax, const double prec=1.e-3)
	function used to estimate the non-linear power spectrum More...

double	g_k (const double k, const std::shared_ptr< cbl::glob::FuncGrid > PkLin, const double qmin, const double qmax, const double prec=1.e-3)
	function used to estimate the non-linear power spectrum More...

double	Pk_1loop (const double kk, const std::shared_ptr< cbl::glob::FuncGrid > PkLin, const int corrtype, const double qmin, const double qmax, const double prec=1.e-3)
	the one-loop power spectrum More...

double	Pk_DeltaDelta (const double kk, const std::shared_ptr< cbl::glob::FuncGrid > Pk, const double qmin, const double qmax, const double prec=1.e-3)
	the real-space matter non-linear power spectrum \(P_{\delta\delta}(k)\), computed at 1-loop More...

std::vector< double >	Pk_DeltaDelta (const std::vector< double > kk, const double redshift, const std::string method_Pk, const bool store_output=true, const std::string output_root="test", const int norm=-1, const double k_min=0.001, const double k_max=100., const double prec=1.e-2, const std::string file_par=par::defaultString, const bool unit1=false)
	the real-space matter non-linear power spectrum \(P_{\delta\delta}(k)\), computed at 1-loop More...

double	Pk_DeltaTheta (const double kk, const std::shared_ptr< cbl::glob::FuncGrid > Pk, const double qmin, const double qmax, const double prec=1.e-3)
	the real-space matter non-linear power spectrum \(P_{\delta\theta}(k)\), computed at 1-loop More...

std::vector< double >	Pk_DeltaTheta (const std::vector< double > kk, const double redshift, const std::string method_Pk, const bool store_output=true, const std::string output_root="test", const int norm=-1, const double k_min=0.001, const double k_max=100., const double prec=1.e-2, const std::string file_par=par::defaultString, const bool unit1=false)
	the real-space matter non-linear power spectrum \(P_{\delta\theta}(k)\), computed at 1-loop More...

double	Pk_ThetaTheta (const double kk, const std::shared_ptr< cbl::glob::FuncGrid > Pk, const double qmin, const double qmax, const double prec=1.e-3)
	the real-space matter non-linear power spectrum \(P_{\theta\theta}(k)\), computed at 1-loop More...

std::vector< double >	Pk_ThetaTheta (const std::vector< double > kk, const double redshift, const std::string method_Pk, const bool store_output=true, const std::string output_root="test", const int norm=-1, const double k_min=0.001, const double k_max=100., const double prec=1.e-2, const std::string file_par=par::defaultString, const bool unit1=false)
	the real-space matter non-linear power spectrum \(P_{\theta\theta}(k)\), computed at 1-loop More...

double	Pk_DeltaDelta_fitting_function (const double kk, const std::string method_Pk, const double redshift, const std::string author, const bool store_output, const std::string output_root, const int norm, double k_min, double k_max, const double prec, const std::string file_par, const bool unit1)
	the non-linear dark matter power spectrum using fitting functions given by Bel et. al (2019) More...

double	Pk_DeltaTheta_fitting_function (const double kk, const std::string method_Pk, const double redshift, const std::string author, const bool store_output, const std::string output_root, const bool NL, const int norm, double k_min, double k_max, const double prec, const std::string file_par, const bool unit1)
	the dark matter cross power spectrum More...

double	Pk_ThetaTheta_fitting_function (const double kk, const std::string method_Pk, const double redshift, const std::string author, const bool store_output, const std::string output_root, const bool NL, const int norm, double k_min, double k_max, const double prec, const std::string file_par, const bool unit1)
	the dark matter velocity divergence power spectrum More...

double	sigma_v (const double redshift=0., const std::string method_Pk="CAMB", const bool store_output=true, const std::string output_root="test", const int norm=-1, const double k_min=0.001, const double k_max=100., const int bin_k=512, const double prec=1.e-2, const std::string file_par=par::defaultString, const bool unit1=false)
	the linear-order one-dimensional pairwise velocity dispersion, \(\sigma_{\mathrm{v}, \mathrm{lin}}\) More...

std::vector< std::vector< double > >	Pk_TNS_AB_multipoles (std::vector< double > kk, const std::string method, const double redshift, const bool store_output, const std::string output_root, const int norm, const double k_min, const double k_max, const double prec)
	the multipoles of the A and B correction terms for the TNS model More...

std::vector< std::vector< double > >	Pk_TNS_AB_1loop (std::vector< double > kk, const double mu, const std::string method, const double redshift, const bool store_output, const std::string output_root, const int norm, const double k_min, const double k_max, const double prec)
	the A and B correction terms for the TNS model at 1-loop from the multipole expansion More...

std::vector< std::vector< double > >	Pk_TNS_AB_terms_1loop (std::vector< double > kk, const std::string method, const double redshift, const bool store_output, const std::string output_root, const int norm, const double k_min=0.001, const double k_max=100., const double prec=1.e-2)
	the expanded A and B correction terms for the TNS model More...

std::vector< std::vector< double > >	Pk_eTNS_terms_1loop (std::vector< double > kk, const std::string method, const double redshift, const bool store_output, const std::string output_root, const int norm, const double k_min=0.001, const double k_max=100., const double prec=1.e-2)
	The expanded correction terms for the extended TNS model (eTNS) More...

std::vector< std::vector< double > >	Pk_TNS_AB_1loop (std::vector< double > kk, const double mu, const double linear_growth_rate, const double bias, const std::string method, const double redshift, const bool store_output, const std::string output_root, const int norm, const double k_min=0.001, const double k_max=100., const double prec=1.e-2)
	the expanded A and B correction terms for the TNS model More...

std::vector< std::vector< double > >	Pk_TNS_dd_dt_tt (std::vector< double > kk, const std::string method, const double redshift, const bool store_output, const std::string output_root, const int norm, const double k_min=0.001, const double k_max=100., const double prec=1.e-2)
	the non-linear \(\delta-\delta\), \(\delta-\theta\), \(\theta-\theta\) matter power spectra More...

Functions to estimate the three-point correlation function
double	denominator_Q (const double r1, const double r2, const double theta, const std::vector< double > rr, const std::vector< double > xi_matter) const
	the normalization factor for reduced three-point correlation function More...

void	integrals_Q_nonLocal (std::vector< double > &xi_matter, std::vector< double > &Phi, const std::vector< double > rr, const std::vector< double > kk, const std::vector< double > Pk_matter, const double prec) const
	integral functions for the three-point correlation model More...

double	Gamma_3PCF (const double r1, const double r2, const double theta, const std::vector< double > xi, const std::vector< double > dPhi) const
	function to compute non-local contribution to three-point correlation function; specifically, it implements Eq. 20 of Bel el et al. 2015, MNRAS, 453, 259: More...

double	Q_nonLocal (const double r1, const double r2, const double theta, std::vector< double > &rr, std::vector< double > &xi_matter, std::vector< double > &Phi, const std::vector< double > kk, const std::vector< double > Pk_matter) const
	the non-local contribution to the reduced dark matter three-point correlation function More...

std::vector< double >	Q_nonLocal (const double r1, const double r2, const std::vector< double > theta, const std::vector< double > kk, const std::vector< double > Pk_matter) const
	all the non-local contribution terms of the reduced dark matter three-point correlation function More...

void	integrals_zeta_Slepian (std::vector< double > &xi_matter, std::vector< double > &xi_matter_m1, std::vector< double > &xi_matter_p1, std::vector< double > &xi_matter_2, const std::vector< double > rr, const std::vector< double > kk, const std::vector< double > Pk_matter) const
	integrals used to compute the Slepian et al. 2015 three-point correlation function model More...

double	zeta_precyclic_Slepian (const double r1, const double r2, const double mu, const double b1, const double b2, const glob::FuncGrid interp_xi_matter, const glob::FuncGrid interp_xi_matter_m1, const glob::FuncGrid interp_xi_matter_p1, const glob::FuncGrid interp_xi_matter_2) const
	the pre-cyclic three-point correlation function as described in Slepian et al. 2015 More...

double	zeta_precyclic_Slepian (const double r1, const double r2, const double r3, const double deltaR, const double b1, const double b2, const glob::FuncGrid interp_xi_matter, const glob::FuncGrid interp_xi_matter_m1, const glob::FuncGrid interp_xi_matter_p1, const glob::FuncGrid interp_xi_matter_2) const
	the pre-cyclic three-point correlation function as described in Slepian et al. 2015, for a triangle averaging in the bin More...

std::vector< double >	zeta_expansion_Slepian (const double r1, const double r2, const double b1, const double b2, std::vector< double > &rr, std::vector< double > &xi_matter, std::vector< double > &xi_matter_m1, std::vector< double > &xi_matter_p1, std::vector< double > &xi_matter_2, const int norders=9, const double prec=1.e-3) const
	the terms of the \(\zeta(r_1, r_2)\) expansion More...

double	zeta_DM_Slepian (const double r1, const double r2, const double theta, std::vector< double > &rr, std::vector< double > &xi_matter, std::vector< double > &xi_matter_m1, std::vector< double > &xi_matter_p1, std::vector< double > &xi_matter_2, const std::vector< double > kk, const std::vector< double > Pk_matter, const int norders=9, const double prec=1.e-3) const
	the dark matter three-point correlation function model by Slepian et al. 2015 More...

double	Q_DM_Slepian (const double r1, const double r2, const double theta, std::vector< double > &rr, std::vector< double > &xi_matter, std::vector< double > &xi_matter_m1, std::vector< double > &xi_matter_p1, std::vector< double > &xi_matter_2, const std::vector< double > kk, const std::vector< double > Pk_matter, const int norders=9, const double prec=1.e-3) const
	the dark matter reduced three-point correlation function model by Slepian et al. 2015 More...

void	integrals_zeta_BarrigaGatzanaga (std::vector< double > &xi_matter, std::vector< double > &Phi, const std::vector< double > rr, const std::vector< double > kk, const std::vector< double > Pk_matter) const
	integrals used to compute the Barriga & Gatzanaga al. 2002 three-point correlation function model More...

double	zeta_single_BarrigaGatzanaga (const double r1, const double r2, const double theta, const std::vector< double > xi, const std::vector< double > dxi, const std::vector< double > dPhi) const
	the single term of the dark matter three-point correlation function model by Barriga & Gatzanaga et al. 2002 More...

double	zeta_DM_BarrigaGatzanaga (const double r1, const double r2, const double theta, std::vector< double > &rr, std::vector< double > &xi_matter, std::vector< double > &Phi, const std::vector< double > kk, const std::vector< double > Pk_matter) const
	the dark matter three-point correlation function model by Barriga & Gatzanaga et al. 2002 More...

double	Q_DM_BarrigaGatzanaga (const double r1, const double r2, const double theta, std::vector< double > &rr, std::vector< double > &xi_matter, std::vector< double > &Phi, const std::vector< double > kk, const std::vector< double > Pk_matter) const
	the dark matter reduced three-point correlation function model by Barriga & Gatzanaga et al. 2002 More...

std::vector< double >	zeta_DM (const double r1, const double r2, const std::vector< double > theta, const std::string model, const std::vector< double > kk, const std::vector< double > Pk_matter) const
	the dark matter three-point correlation function More...

std::vector< double >	Q_DM (const double r1, const double r2, const std::vector< double > theta, const std::string model, const std::vector< double > kk, const std::vector< double > Pk_matter) const
	the dark matter reduced three-point correlation function More...

std::vector< double >	zeta_halo (const double r1, const double r2, const std::vector< double > theta, const double b1, const double b2, const std::string model, const std::vector< double > kk, const std::vector< double > Pk_matter) const
	the local-bias model of the three-point correlation function of dark matter haloes More...

std::vector< double >	Q_halo (const double r1, const double r2, const std::vector< double > theta, const double b1, const double b2, const std::string model, const std::vector< double > kk, const std::vector< double > Pk_matter) const
	the local-bias model of the reduced three-point correlation function of dark matter haloes More...

std::vector< double >	Q_halo (const double r1, const double r2, const std::vector< double > theta, const double b1, const double b2, const double g2, const std::string model, const std::vector< double > kk, const std::vector< double > Pk_matter) const
	the non-local-bias model of the three-point correlation function of dark matter haloes More...

std::vector< double >	zeta_DM_eq (const std::vector< double > rr, const std::string model, const std::vector< double > kk, const std::vector< double > Pk_matter) const
	the dark matter equilateral three-point correlation function More...

std::vector< double >	Q_DM_eq (const std::vector< double > rr, const std::string model, const std::vector< double > kk, const std::vector< double > Pk_matter) const
	the dark matter equilateral reduced three-point correlation function More...

double	zeta_multipoles_covariance (const double Volume, const double nObjects, const int l, const int l_prime, const double r1, const double r2, const double r1_prime, const double r2_prime, const double deltaR, const std::vector< double > kk, const std::vector< double > Pk, const std::vector< double > rr, const std::vector< double > Xi, const double prec=1.e-3)
	the dark matter three-point correlation function multipoles covariance model, by Slepian et al. 2015 More...

std::vector< std::vector< double > >	zeta_covariance (const double Volume, const double nObjects, const std::vector< double > theta, const double r1, const double r2, const double deltaR, const std::vector< double > kk, const std::vector< double > Pk, const int norders=10, const double prec=1.e-3, const bool method=false, const int nExtractions=10000, const std::vector< double > mean={}, const int seed=543)
	the dark matter three-point correlation function covariance model More...

void	xi_r_n (std::vector< double > &xi_n, const std::vector< double > rr, const int nn, const std::vector< double > kk, const std::vector< double > Pk)
	compute the power spectrum integral transform More...

void	xi_r_n_pm (std::vector< double > &xi_n_p, std::vector< double > &xi_n_m, const std::vector< double > rr, const int nn, const std::vector< double > kk, const std::vector< double > Pk)
	compute the power spectrum integral transform More...

void	eff_l_l1 (std::vector< std::vector< double >> &eff, const std::vector< double > rr, const int l, const int l1, const std::vector< double > kk, const std::vector< double > Pk)
	compute the power spectrum integral transform More...

void	I_ELL_ell (std::vector< std::vector< double >> &II, const std::vector< double > rr, const int ll, const int LL, const std::vector< double > kk, const std::vector< double > Pk)
	compute the quantity \( I_{\mathcal{L} l} (r_1, r_2)\) More...

void	k_ell (std::vector< std::vector< double >> &KK, const std::vector< double > rr, const int ll, const std::vector< double > kk, const std::vector< double > Pk)
	compute the quantity \( k_l (r_1, r_2) \) More...

double	zeta_ell_0_factor (const double b1, const double gamma, const double beta)
	the multiplicative factor for \( \zeta_0 \), with local bias More...

double	zeta_ell_1_factor (const double b1, const double beta)
	the multiplicative factor for \( \zeta_1 \), with local bias More...

double	zeta_ell_2_factor (const double b1, const double gamma, const double beta)
	the multiplicative factor for \( \zeta_2 \), with local bias More...

double	zeta_ell_3_factor (const double b1, const double beta)
	the multiplicative factor for \( \zeta_3 \), with local bias More...

double	zeta_ell_4_factor (const double b1, const double beta)
	the multiplicative factor for \( \zeta_4 \), with local bias More...

double	zeta_ell_k_factor (const double b1, const double beta)
	the multiplicative factor for \( \zeta_l, l>4 \), with local bias More...

double	zeta_ell_0_factor_tidal (const double gamma_t, const double beta)
	the multiplicative factor for \( \zeta_l, l=0 \), with non-local bias More...

double	zeta_ell_2_factor_tidal (const double gamma_t, const double beta)
	the multiplicative factor for \( \zeta_l, l=2 \), with non-local bias More...

double	zeta_ell_4_factor_tidal (const double gamma_t, const double beta)
	the multiplicative factor for \( \zeta_l, l=4 \), with non-local bias More...

double	zeta_ell_precyclic (const double r1, const double r2, const int ell, const double b1, const double b2, const double bt, const double beta, std::vector< std::shared_ptr< glob::FuncGrid >> interp_xi_ell, const bool use_k, std::shared_ptr< glob::FuncGrid2D > interp_k_ell)
	the pre-cyclic \( \zeta_l \) More...

std::vector< double >	zeta_RSD (const double r1, const double r2, const int ntheta, const double b1, const double b2, const double bt, const double beta, const std::vector< double > rr, const std::vector< double > kk, const std::vector< double > Pk, const bool include_limits=false, const int max_ll=4, const bool use_k=false)
	the \( \zeta (r_1, r_2, \theta) \) More...

std::vector< double >	zeta_RSD (const double r1, const double r2, const int ntheta, const double b1, const double b2, const double bt, const double redshift, const std::string method_Pk, const int step_r, const int step_k, const bool store_output=true, const std::string output_root="test", const bool force_RealSpace=false, const bool include_limits=false, const int max_ll=4, const bool use_k=false)
	the \( \zeta (r_1, r_2, \theta) \) More...

Private Member Functions
Auxiliary functions of internal usage
void	set_default ()
	internal function to set default values

double	m_func_sigma (const std::string method_Pk, const double redshift, const bool store_output=true, const std::string output_root="test", const std::string interpType="Linear", const double k_max=100., const std::string input_file=par::defaultString, const bool is_parameter_file=true, std::function< double(double)> filter={}, const bool unit1=false) const
	function to compute the not-yet-normalised mass variances and their derivatives More...

double	m_sigma2R_notNormalised (const double radius, const std::string method_Pk, const double redshift, const bool store_output=true, const std::string output_root="test", const std::string interpType="Linear", const double k_max=100., const std::string input_file=par::defaultString, const bool is_parameter_file=true, const bool unit1=false) const
	the not-yet-normalised mass variance, \(\sigma^2(R)\) More...

double	m_sigma2M_notNormalised (const double mass, const std::string method_Pk, const double redshift, const bool store_output=true, const std::string output_root="test", const std::string interpType="Linear", const double k_max=100., const std::string input_file=par::defaultString, const bool is_parameter_file=true, const bool unit1=false) const
	the not-yet-normalised mass variance, \(\sigma^2(M)\) More...

double	m_mass_function (const double Mass, std::shared_ptr< void > mass_function_params)
	auxiliary function to compute the mass function of dark matter haloes (filaments and sheets) More...

double	m_MF_generator (const double Mass, const double Sigma, const double Dln_Sigma, const double redshift, const std::string model_MF, const double Delta=200., const bool default_delta=true, const double delta_t=1.686)
	auxiliary function to compute the mass function More...

double	m_MF_generator (const double Mass, const double Sigma, const double Dln_Sigma, const double redshift, const double D_N, const std::string model_MF, const double Delta=200., const bool default_delta=true, const double delta_t=1.686)
	auxiliary function to compute the mass function More...

double	m_bias_halo_generator (const double Sigma, const double redshift, const std::string author, const double Delta=200.) const
	auxiliary function to compute the halo bias More...

double	m_bias_halo_generator (const double Sigma, const double redshift, const double D_N, const std::string author, const double Delta=200.) const
	auxiliary function to compute the halo bias More...

double	m_elf_dz (const double phi) const
	the incomplete elliptic integral More...

double	m_acn_dz (const double cc) const
	the inverse cosine amplitude of the Jacobian elliptic function More...

double	m_asn_dz (const double ss) const
	the inverse sine amplitude of the Jacobian elliptic function More...

double	m_serf_dz (const double yy) const
	the inverse truncated series necessary to compute sn^-1(s\|m) in ASN_DZ More...

void	m_Table_Pk_CAMB_MPTbreeze (const std::string code, const bool NL, std::vector< double > &lgkk, std::vector< double > &lgPk, const double redshift, const bool store_output=true, const std::string output_root="test", const double k_max=100.) const
	write and read the table where the dark matter power spectrum, computed with either CAMB or MPTbreeze, is stored More...

void	m_Table_Pk_CAMB_MPTbreeze (const std::string code, const bool NL, std::vector< std::vector< double >> &lgkk, std::vector< std::vector< double >> &lgPk, const std::vector< double > redshift, const bool store_output=true, const std::string output_root="test", const double k_max=100.) const
	write and read the table where the dark matter power spectrum, computed with either CAMB or MPTbreeze, is stored More...

void	m_Table_Pk_CLASS (const bool NL, std::vector< double > &lgkk, std::vector< double > &lgPk, const double redshift, const bool store_output=true, const std::string output_root="test", const double k_max=100.) const
	write and read the table where the dark matter power spectrum computed with CLASS is stored More...

void	m_Table_Pk_CLASS (const bool NL, std::vector< std::vector< double >> &lgkk, std::vector< std::vector< double >> &lgPk, const std::vector< double > redshift, const bool store_output=true, const std::string output_root="test", const double k_max=100.) const
	write and read the table where the dark matter power spectrum computed with CLASS is stored More...

void	m_Table_Pk_parameterFile (const std::string code, const std::string file_par, const bool NL, std::vector< double > &lgkk, std::vector< double > &lgPk, const double redshift, const std::string output_root="test") const
	write and read the table where the dark matter power spectrum is stored; it is used when a parameter file is provided in input More...

Private Attributes
double	m_Omega_matter
	\(\Omega_M\): the density of baryons, cold dark matter and massive neutrinos (in units of the critical density) at z=0 in the LCDM case

double	m_Omega_baryon
	\(\Omega_b\): the baryon density at z=0

double	m_Omega_neutrinos
	\(\Omega_\nu\): the density of massive neutrinos at z=0

double	m_massless_neutrinos
	\(N_{eff}\): the effective number (for QED + non-instantaneous decoupling)

int	m_massive_neutrinos
	the number of degenerate massive neutrino species

double	m_Omega_DE
	\(\Omega_{DE}\): the dark energy density at z=0

double	m_Omega_radiation
	\(\Omega_{rad}\): the radiation density at z=0

double	m_Omega_k
	\(\Omega_k\): the density of curvature energy

double	m_Omega_CDM
	\(Omega_{CDM}\): the cold dark matter density at z=0

double	m_H0
	\(H_0\): the Hubble constant at z=0 [km/sec/Mpc]

double	m_hh
	\(h\): the Hubble parameter, \(H_0/100\)

double	m_t_H
	\(t_H\): the Hubble time

double	m_D_H
	\(D_H\): the Hubble distance

double	m_sigma8
	\(sigma_8\): the power spectrum normalisation

double	m_scalar_amp
	\(A_s\): the initial scalar amplitude of the power spectrum

double	m_scalar_pivot
	the scalar pivot k in \(Mpc^{-1}\)

double	m_n_spec
	\(n_{spec}\): the primordial spectral index

double	m_w0
	\(w_0\): the parameter of the dark energy equation of state (CPL parameterisation)

double	m_wa
	\(w_a\): the parameter of the dark energy equation of state (CPL parameterisation)

double	m_RhoZero
	\(\rho_0\): the mean density of the Universe at z=0 [Msun*Mpc^-3]

double	m_fNL
	\(f_{NL}\): the non-Gaussian amplitude

int	m_type_NG
	the non-Gaussian shape (type=1 local, type=2 equilateral, type=3 enfolded, type=4 orthogonal)

double	m_tau
	\(\tau\): Thomson scattering optical depth due to reionization

double	m_rs
	\(r_s\) the sound horizon

double	m_Pk0_EH
	the normalisation of the power spectrum for Eisenstein & Hu [http://background.uchicago.edu/~whu/transfer/transferpage.html]

double	m_Pk0_CAMB
	the normalisation of the power spectrum for CAMB [http://camb.info/]

double	m_Pk0_MPTbreeze
	the normalisation of the power spectrum for MPTbreeze [http://arxiv.org/abs/1207.1465]

double	m_Pk0_CLASS
	the normalisation of the power spectrum for CLASS [http://class-code.net/]

std::string	m_model
	the cosmologial model used to compute distances

bool	m_unit
	false \(\rightarrow\) quantities are provided in phyical units; true \(\rightarrow\) quantities are provided in cosmological units (i.e. in units of h, e.g. Mpc/h)

Detailed Description

The class Cosmology.

This class is used to handle objects of type cosmology . It can be used to estimate i) any kind of cosmic distances and volumes, ii) the halo mass function and bias, iii) the real-space and redshift-space dark matter power spectrum and correlation function (with both CAMB, CLASS, MPTbreeze and the analytic fitting forms by Eisenstein & Hu), iv) the accreted mass function, v) several BAO parameters, and vi) the halo mass function and bias in different non-Gaussian cosmological frameworks.

Definition at line 277 of file Cosmology.h.

Constructor & Destructor Documentation

◆ Cosmology() [1/2]

cbl::cosmology::Cosmology::Cosmology	(	const double	Omega_matter = `0.27`,
		const double	Omega_baryon = `0.046`,
		const double	Omega_neutrinos = `0.`,
		const double	massless_neutrinos = `3.04`,
		const int	massive_neutrinos = `0`,
		const double	Omega_DE = `0.73`,
		const double	Omega_radiation = `0.`,
		const double	hh = `0.7`,
		const double	scalar_amp = `2.46e-9`,
		const double	scalar_pivot = `0.05`,
		const double	n_spec = `0.96`,
		const double	w0 = `-1.`,
		const double	wa = `0.`,
		const double	fNL = `0.`,
		const int	type_NG = `1`,
		const double	tau = `0.09`,
		const std::string	model = `"LCDM"`,
		const bool	unit = `true`
	)

constructor

Parameters

Omega_matter	\(\Omega_M\): the density of baryons, cold dark matter and massive neutrinos (in units of the critical density) at z=0
Omega_baryon	\(\Omega_b\): the density of baryons at z=0
Omega_neutrinos	\(\Omega_\nu\): the density of massive neutrinos at z=0
massless_neutrinos	the effective number (for QED + non-instantaneous decoupling)
massive_neutrinos	the number of degenerate massive neutrino species
Omega_DE	\(\Omega_{DE}\): the density of dark energy at z=0
Omega_radiation	\(\Omega_{rad}\): the density of radiation at z=0
hh	h: the Hubble parameter, \(H_0/100\)
scalar_amp	\(A_s\): the initial scalar amplitude of the power spectrum
scalar_pivot	the scalar pivot k in \(Mpc^{-1}\)
n_spec	\(n_{spec}\): the primordial spectral index
w0	\(w_0\): one of the two parameters of the dark energy equation of state (CPL parameterisation)
wa	\(w_a\): one of the two parameters of the dark energy equation of state (CPL parameterisation)
fNL	\(f_{NL}\): the non-Gaussian amplitude
type_NG	the non-Gaussian shape (type=1 local, type=2 equilateral, type=3 enfolded, type=4 orthogonal)
tau	\(\tau\): Thomson scattering optical depth due to reionization
model	the cosmologial model used to compute distances
unit	false \(\rightarrow\) quantities are provided in phyical units; true \(\rightarrow\) quantities are provided in cosmological units (i.e. in units of h, e.g. Mpc/h)

Warning: by default: \(\Omega_k = 1-\Omega_M-\Omega_{rad}-\Omega_{DM}\), \(\Omega_{CDM} = \Omega_M-\Omega_b-\Omega_\nu\), \(t_H = 1-H_0\), \(D_H = c/t_H\), \(\rho_0 = \rho_0(\Omega_M, \Omega_\nu)\)

Definition at line 165 of file Cosmology.cpp.

◆ Cosmology() [2/2]

cbl::cosmology::Cosmology::Cosmology	(	const CosmologicalModel	cosmoModel,
		const std::string	model = `"LCDM"`,
		const bool	unit = `true`
	)

constructor using built-in cosmological models

by default: \(\Omega_k = 1-\Omega_M-\Omega_{rad}-\Omega_{DM}\), \(\Omega_{CDM} = \Omega_M-\Omega_b-\Omega_\nu\), \(t_H = 1-H_0\) \(D_H = c/t_H\) \(\rho_0 = \rho_0(\Omega_M, \Omega_nu)\)

Parameters

cosmoModel	the built-in cosmological model
model	the cosmologial model used to compute distances
unit	false \(\rightarrow\) quantities are provided in phyical units; true \(\rightarrow\) quantities are provided in cosmological units (i.e. in units of h, e.g. Mpc/h)

Definition at line 173 of file Cosmology.cpp.

Member Function Documentation

◆ Am()

double cbl::cosmology::Cosmology::Am	(	const std::string	method_Pk,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const int	norm = `-1`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`,
		const std::string	file_par = `par::defaultString`
	)

the amplitude of the matter power spectrum

Author: Cosimo Fedeli; cosim.nosp@m.o.fe.nosp@m.deli@.nosp@m.oabo.nosp@m..inaf.nosp@m..it

Parameters

method_Pk	method used to compute the power spectrum (i.e. the Boltzmann solver); valid choices for method_Pk are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	the output_root parameter of the parameter file used to compute the power spectrum; it can be any name. If this parameter is different from the default value it will be used also in the output directory name
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
prec	accuracy of the integration
file_par	name of the parameter file; if a parameter file is provided (i.e. file_par!=NULL), it will use be used, ignoring the cosmological parameters of the object

Returns: A_m

Definition at line 47 of file NG.cpp.

◆ AP_corr()

vector< double > cbl::cosmology::Cosmology::AP_corr	(	const cbl::cosmology::Cosmology	cosm_true,
		const std::vector< double >	redshift
	)

Supplementary function to compute a correction factor to apply to the void size function, to predict the measured abundance of voids affected by geometrical distortions (Alcock-Paczyński change of volume). These are caused by the assumption of a fiducial cosmology different from the true one, see Correa et al. 2020 (https://arxiv.org/pdf/2007.12064.pdf)

Author: Sofia Contarini; sofia.nosp@m..con.nosp@m.tarin.nosp@m.i3@u.nosp@m.nibo..nosp@m.it

Parameters

cosm_true	the true cosmology of the catalogue
redshift	the vector of redshifts of different samples of voids

Returns: a vector with the correction factors relative to the void samples at different redshifts

Definition at line 96 of file SizeFunction.cpp.

◆ As()

double cbl::cosmology::Cosmology::As ( const double sigma8 ) const

amplitude of the curvature perturbations

this function provides an approximate value of A_s, for a fiven value of σ₈, from Eq.(3) by Vikhlinin et al. 2009, ApJ, 692, 1060; it is valid only without massive neutrinos! (see also Hu & Jain 2004)

Parameters

sigma8 σ₈ the power spectrum normalisation

Returns: A_s

Definition at line 49 of file PkXi.cpp.

◆ Az()

double cbl::cosmology::Cosmology::Az ( const double redshift ) const

the acoustic parameter

see Eisenstein 2005

Author: Alfonso Veropalumbo; alfon.nosp@m.so.v.nosp@m.eropa.nosp@m.lumb.nosp@m.o@uni.nosp@m.bo.i.nosp@m.t

Parameters

redshift the redshift

Returns: the acoustic parameter

Definition at line 206 of file BAO.cpp.

◆ beta() [1/3]

double cbl::cosmology::Cosmology::beta	(	const double	Mass_min,
		const double	Mass_max,
		const double	redshift,
		const std::string	model_bias,
		const std::string	model_MF,
		const std::string	method_SS,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const double	Delta = `200.`,
		const double	kk = `-1.`,
		const std::string	interpType = `"Linear"`,
		const int	norm = `-1`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`
	)

the error on the specific growth rate β

Parameters

Mass_min	minimum halo mass
Mass_max	maximum halo mass
redshift	the redshift
model_bias	author(s) who proposed the bias; valid authors are: ST99 (Sheth & Tormen 1999), SMT01 (Sheth, Mo & Tormen 2001), SMT01_WL04 (Sheth, Mo & Tormen 2001 with the correction of Warren 2004), Tinker (Tinker et al. 2010)
model_MF	author(s) who proposed the mass function; valid authors are: PS (Press & Schechter), ST (Sheth & Tormen), Jenkins (Jenkins et al. 2001), Warren (Warren et al. 2006), ShenH (halo MF, Shen et al. 2006), ShenF (filament MF, Shen et al. 2006), ShenS (sheet MF, Shen et al. 2006), Pan (Pan 2007), Peacock (Peacock at al. 2007), Reed (Reed et al. 2007), Tinker (Tinker et al. 2008), Crocce (Crocce et al. 2010), Manera (Manera et al. 2010), Courtin (Courtin et al. 2010), Bhattacharya (Bhattacharya et al. 2011), Angulo_FOF (FoF MF, Angulo et al. 2012), Angulo_Sub (SUBFIND MF, Angulo et al. 2012), Watson_FOF (FoF MF, Watson et al. 2012), Watson_SOH (Spherical Overdensity halo MF, Watson et al. 2012), Despali_Z0, Despali_AllZ, Despali_AllZAllCosmo, Despali_HighM (Despali et al. 2016)
method_SS	method used to compute the power spectrum and σ(mass); valid method_SS are: CAMB [http://camb.info/], CLASS [http://class-code.net/], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
Delta	\(\Delta\), the overdensity
kk	wave vector module
interpType	method to interpolate the power spectrum
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed
prec	accuracy of the integration
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum

Returns: β=f/b, where f is the linear growth rate and b is the bias

Warning: the input parameter \(\Delta\) is the background overdensity, not the critical overdensity \(\Delta_{crit}\); divide \(\Delta_{crit}\) by \(\Omega_M(z)\) (see cbl::cosmology::Cosmology::OmegaM) to obtain the background overdensity; the mass function by Manera et al. (2010) has been tested only for z=0 and z=0.5; the mass function by Despali et al. (2016) is currently implemented only for virial masses and at \(z<1.25\)

Definition at line 73 of file RSD.cpp.

◆ beta() [2/3]

double cbl::cosmology::Cosmology::beta	(	const double	redshift,
		const double	bias
	)		const

the specific growth rate β

Parameters

redshift	the redshift
bias	bias

Returns: β=f/b, where f is the linear growth rate and b is the bias

Definition at line 55 of file RSD.cpp.

◆ beta() [3/3]

double cbl::cosmology::Cosmology::beta	(	const std::vector< double >	MM,
		const std::vector< double >	MF,
		const double	redshift,
		const std::string	model_bias,
		const std::string	method_SS,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const double	Delta = `200.`,
		const double	kk = `-1.`,
		const std::string	interpType = `"Linear"`,
		const int	norm = `-1`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`
	)

the specific growth rate β

Parameters

MM	vector of halo masses
MF	vector of mass function values, dΦ/dM=dn(M)/dM
redshift	the redshift
model_bias	author(s) who proposed the bias; valid authors are: ST99 (Sheth & Tormen 1999), SMT01 (Sheth, Mo & Tormen 2001), SMT01_WL04 (Sheth, Mo & Tormen 2001 with the correction of Warren 2004), Tinker (Tinker et al. 2010)
method_SS	method used to compute the power spectrum and σ(mass); valid method_SS are: CAMB [http://camb.info/], CLASS [http://class-code.net/], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
Delta	\(\Delta\), the overdensity
kk	wave vector module
interpType	method to interpolate the power spectrum
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed
prec	accuracy of the integration
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum

Returns: β=f/b, where f is the linear growth rate and b is the bias

Warning: the input parameter \(\Delta\) is the background overdensity, not the critical overdensity \(\Delta_{crit}\); divide \(\Delta_{crit}\) by \(\Omega_M(z)\) (see cbl::cosmology::Cosmology::OmegaM) to obtain the background overdensity; the mass function by Manera et al. (2010) has been tested only for z=0 and z=0.5; the mass function by Despali et al. (2016) is currently implemented only for virial masses and at \(z<1.25\)

Definition at line 91 of file RSD.cpp.

◆ bias_correction()

double cbl::cosmology::Cosmology::bias_correction	(	const double	kk,
		const double	mass,
		const std::string	method_Pk,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const std::string	interpType = `"Linear"`,
		const int	norm = `-1`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`
	)

correction to the halo bias in non-Gaussian cosmologies

Author: Cosimo Fedeli; cosim.nosp@m.o.fe.nosp@m.deli@.nosp@m.oabo.nosp@m..inaf.nosp@m..it

Parameters

kk	wave vector module
mass	halo mass
method_Pk	method used to compute the power spectrum (i.e. the Boltzmann solver); valid choices for method_Pk are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	the output_root parameter of the parameter file used to compute the power spectrum; it can be any name. If this parameter is different from the default value it will be used also in the output directory name
interpType	method to interpolate the power spectrum
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
prec	accuracy of the integration
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum

Returns: bias correction

Definition at line 356 of file NG.cpp.

◆ bias_eff() [1/2]

double cbl::cosmology::Cosmology::bias_eff	(	const double	Mass_min,
		const double	Mass_max,
		const double	redshift,
		const std::string	model_bias,
		const std::string	model_MF,
		const std::string	method_SS,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const double	Delta = `200.`,
		const double	kk = `-1.`,
		const std::string	interpType = `"Linear"`,
		const int	norm = `-1`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`
	)

the effective bias of dark matter haloes, with masses in a given range and at a given mean redshift

this function computes the effective bias of dark matter haloes:

\[ b_{eff}(z) = \frac{\int_{M_{min}}^{M_{max}} {\rm d}M\, b(M, z) \Phi(M, z)}{\int_{M_{min}}^{M_{max}} {\rm d}M\,\Phi(M, z)} \]

in the current implementation, the integral is actually replaced by the Riemann sum, as follows:

\[ b_{eff}(z) \simeq \frac{\sum_{i_{min}}^{i_{max}} b(M, z) \Phi(M, z) (M_{i+1}-M_i)}{\sum_{i_{min}}^{i_{max}} \Phi(M, z) (M_{i+1}-M_i)} \]

where the halo mass function, \(\Phi(M, z)\), is computed by cbl::cosmology::Cosmology::mass_function and the linear bias, \(b(M, z)\), is computed by cbl::cosmology::Cosmology::bias_halo

Parameters

Mass_min	minimum halo mass
Mass_max	maximum halo mass
redshift	the redshift
model_bias	author(s) who proposed the bias; valid authors are: ST99 (Sheth & Tormen 1999), SMT01 (Sheth, Mo & Tormen 2001), SMT01_WL04 (Sheth, Mo & Tormen 2001 with the correction of Warren 2004), Tinker (Tinker et al. 2010)
model_MF	author(s) who proposed the mass function; valid authors are: PS (Press & Schechter), ST (Sheth & Tormen), Jenkins (Jenkins et al. 2001), Warren (Warren et al. 2006), ShenH (halo MF, Shen et al. 2006), ShenF (filament MF, Shen et al. 2006), ShenS (sheet MF, Shen et al. 2006), Pan (Pan 2007), Peacock (Peacock at al. 2007), Reed (Reed et al. 2007), Tinker (Tinker et al. 2008), Crocce (Crocce et al. 2010), Manera (Manera et al. 2010), Courtin (Courtin et al. 2010), Bhattacharya (Bhattacharya et al. 2011), Angulo_FOF (FoF MF, Angulo et al. 2012), Angulo_Sub (SUBFIND MF, Angulo et al. 2012), Watson_FOF (FoF MF, Watson et al. 2012), Watson_SOH (Spherical Overdensity halo MF, Watson et al. 2012), Despali_Z0, Despali_AllZ, Despali_AllZAllCosmo, Despali_HighM (Despali et al. 2016)
method_SS	method used to compute the power spectrum and σ(mass); valid method_SS are: CAMB [http://camb.info/], CLASS [http://class-code.net/], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
Delta	\(\Delta\), the overdensity
kk	wave vector module
interpType	method to interpolate the power spectrum
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed
prec	accuracy of the integration
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum

Returns: b_eff: the effective dark matter bias

Warning: the input parameter \(\Delta\) is the background overdensity, not the critical overdensity \(\Delta_{crit}\); divide \(\Delta_{crit}\) by \(\Omega_M(z)\) (see cbl::cosmology::Cosmology::OmegaM) to obtain the background overdensity; the mass function by Manera et al. (2010) has been tested only for z=0 and z=0.5; the mass function by Despali et al. (2016) is currently implemented only for virial masses and at \(z<1.25\)

Definition at line 153 of file Bias.cpp.

◆ bias_eff() [2/2]

double cbl::cosmology::Cosmology::bias_eff	(	const std::vector< double >	MM,
		const std::vector< double >	MF,
		const double	redshift,
		const std::string	model_bias,
		const std::string	method_SS,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const double	Delta = `200.`,
		const double	kk = `-1.`,
		const std::string	interpType = `"Linear"`,
		const int	norm = `-1`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`
	)

effective bias of dark matter haloes, computed by averaging over the bias of a given set of haloes

this function computes the effective bias of dark matter haloes as follows:

\[ b_{eff}(z) = \frac{\int_{M_{min}}^{M_{max}} {\rm d}M\, b(M, z) \Phi(M, z)}{\int_{M_{min}}^{M_{max}} {\rm d}M\,\Phi(M, z)} \]

in the current implementation, the integral is actually replaced by the Riemann sum, as follows:

\[ b_{eff}(z) \simeq \frac{\sum_{i_{min}}^{i_{max}} b(M, z) \Phi(M, z) (M_{i+1}-M_i)}{\sum_{i_{min}}^{i_{max}} \Phi(M, z) (M_{i+1}-M_i)} \]

where the halo mass function is provided in input and the linear bias, \(b(M, z)\), is computed by cbl::cosmology::Cosmology::bias_halo

Parameters

MM	vector of halo masses
MF	vector of mass function values, dΦ/dM=dn(M)/dM
redshift	the redshift
model_bias	author(s) who proposed the bias; valid authors are: ST99 (Sheth & Tormen 1999), SMT01 (Sheth, Mo & Tormen 2001), SMT01_WL04 (Sheth, Mo & Tormen 2001 with the correction of Warren 2004), Tinker (Tinker et al. 2010)
method_SS	method used to compute the power spectrum and σ(mass); valid method_SS are: CAMB [http://camb.info/], CLASS [http://class-code.net/], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
Delta	\(\Delta\), the overdensity
kk	wave vector module
interpType	method to interpolate the power spectrum
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed
prec	accuracy of the integration
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum

Returns: b_eff: the effective dark matter bias

Warning: the input parameter \(\Delta\) is the background overdensity, not the critical overdensity \(\Delta_{crit}\); divide \(\Delta_{crit}\) by \(\Omega_M(z)\) (see cbl::cosmology::Cosmology::OmegaM) to obtain the background overdensity

Definition at line 196 of file Bias.cpp.

◆ bias_eff_mass() [1/2]

vector< double > cbl::cosmology::Cosmology::bias_eff_mass	(	const std::vector< double >	mass,
		const std::vector< double >	mass_grid,
		const std::vector< double >	redshift,
		const std::string	model_bias,
		const std::string	method_SS,
		const std::string	meanType = `"mean_bias"`,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const double	Delta = `200.`,
		const double	kk = `-1.`,
		const std::string	interpType = `"Linear"`,
		const int	norm = `-1`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`
	)

effective bias of dark matter haloes, computed by averaging the bias of a set of haloes, interpolating the mass variance on a grid

this function computes the effective bias of dark matter haloes by either averaging the bias of a set of haloes with a given mass:

\[b_{eff}(z) = \frac{1}{N_{halo}}\sum_{i=1}^{N_{halo}} b(M_i, z_i) \; , \; (1)\]

or by averaging over halo pairs:

\[b_{eff}(z) = \sqrt{ \frac{2}{N_{halo}(N_{halo}-1)} \sum_{i=1}^{N_{halo}}\sum_{j=i+1}^{N_{halo}} b(M_i, z_i)b(M_j, z_j)} \; , \; (2)\]

where the linear bias of the \(i\)-th halo, \(b^{i}(M, z)\), is computed by cbl::cosmology::Cosmology::bias_halo; the mass variance is computed by cbl::cosmology::Cosmology::sigma2M

Parameters

mass	vector containing the halo masses
mass_grid	vector containing the halo masses on the grid used to interpolate the mass variance
redshift	vector containing the redshifts; if it has size=1, it will be considered as the main redshift
model_bias	author(s) who proposed the bias; valid authors are: ST99 (Sheth & Tormen 1999), SMT01 (Sheth, Mo & Tormen 2001), SMT01_WL04 (Sheth, Mo & Tormen 2001 with the correction of Warren 2004), Tinker (Tinker et al. 2010)
method_SS	method used to compute the power spectrum and σ(mass); valid method_SS are: CAMB [http://camb.info/], CLASS [http://class-code.net/], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
meanType	meanType="mean_bias" \(\rightarrow\) the effective bias is computed with Eq.(1); meanType="mean_pair_bias" \(\rightarrow\) the effective bias is computed with Eq.(2)
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
Delta	\(\Delta\): the background overdensity
kk	wave vector module
interpType	method to interpolate the power spectrum
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed
prec	accuracy of the integration
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum

Returns: a vector containing the mean and standard deviation of the effective dark matter bias

Definition at line 349 of file Bias.cpp.

◆ bias_eff_mass() [2/2]

vector< double > cbl::cosmology::Cosmology::bias_eff_mass	(	const std::vector< double >	MM,
		const std::vector< double >	redshift,
		const std::string	model_bias,
		const std::string	method_SS,
		const std::string	meanType = `"mean_bias"`,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const double	Delta = `200.`,
		const double	kk = `-1.`,
		const std::string	interpType = `"Linear"`,
		const int	norm = `-1`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`
	)

effective bias of dark matter haloes, computed by averaging the bias of a set of haloes

this function computes the effective bias of dark matter haloes by either averaging the bias of a set of haloes with a given mass:

\[b_{eff}(z) = \frac{1}{N_{halo}}\sum_{i=1}^{N_{halo}} b(M_i, z_i) \; , \; (1)\]

or by averaging over halo pairs:

\[b_{eff}(z) = \sqrt{ \frac{2}{N_{halo}(N_{halo}-1)} \sum_{i=1}^{N_{halo}}\sum_{j=i+1}^{N_{halo}} b(M_i, z_i)b(M_j, z_j)} \; , \; (2)\]

where the linear bias of the \(i\)-th halo, \(b^{i}(M, z)\), is computed by cbl::cosmology::Cosmology::bias_halo; the mass variance is computed by cbl::cosmology::Cosmology::sigma2M

Parameters

MM	vector containing the halo masses
redshift	vector containing the redshifts; if it has size=1, it will be considered as the main redshift
model_bias	author(s) who proposed the bias; valid authors are: ST99 (Sheth & Tormen 1999), SMT01 (Sheth, Mo & Tormen 2001), SMT01_WL04 (Sheth, Mo & Tormen 2001 with the correction of Warren 2004), Tinker (Tinker et al. 2010)
method_SS	method used to compute the power spectrum and σ(mass); valid method_SS are: CAMB [http://camb.info/], CLASS [http://class-code.net/], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
meanType	meanType="mean_bias" \(\rightarrow\) the effective bias is computed with Eq.(1); meanType="mean_pair_bias" \(\rightarrow\) the effective bias is computed with Eq.(2)
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
Delta	\(\Delta\): the background overdensity
kk	wave vector module
interpType	method to interpolate the power spectrum
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed
prec	accuracy of the integration
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum

Returns: a vector containing the mean and standard deviation of the effective dark matter bias

Definition at line 298 of file Bias.cpp.

◆ bias_eff_mass_grid()

vector< double > cbl::cosmology::Cosmology::bias_eff_mass_grid	(	const std::vector< double >	MM,
		const std::vector< double >	redshift,
		const std::string	model_bias,
		const std::string	method_SS,
		const std::string	meanType = `"mean_bias"`,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const double	Delta_crit = `200.`,
		const double	kk = `-1.`,
		const std::string	interpType = `"Linear"`,
		const int	norm = `-1`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`
	)

effective bias of dark matter haloes, computed by averaging the bias of a set of haloes, with the mass variance estimated from a grid

this function computes the effective bias of dark matter haloes by either averaging the bias of a set of haloes with a given mass:

\[b_{eff}(z) = \frac{1}{N_{halo}}\sum_{i=1}^{N_{halo}} b(M_i, z_i) \; , \; (1)\]

or by averaging over halo pairs:

\[b_{eff}(z) = \sqrt{ \frac{2}{N_{halo}(N_{halo}-1)} \sum_{i=1}^{N_{halo}}\sum_{j=i+1}^{N_{halo}} b(M_i, z_i)b(M_j, z_j)} \; , \; (2)\]

where the linear bias of the \(i\)-th halo, \(b^{i}(M, z)\), is computed by cbl::cosmology::Cosmology::bias_halo; the mass variance is estimated from a grid by cbl::cosmology::Cosmology::create_grid_sigmaM

Parameters

MM	vector containing the halo masses
redshift	vector containing the redshifts; if it has size=1, it will be considered as the main redshift
model_bias	author(s) who proposed the bias; valid authors are: ST99 (Sheth & Tormen 1999), SMT01 (Sheth, Mo & Tormen 2001), SMT01_WL04 (Sheth, Mo & Tormen 2001 with the correction of Warren 2004), Tinker (Tinker et al. 2010)
method_SS	method used to compute the power spectrum and σ(mass); valid method_SS are: CAMB [http://camb.info/], CLASS [http://class-code.net/], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
meanType	meanType="mean_bias" \(\rightarrow\) the effective bias is computed with Eq.(1); meanType="mean_pair_bias" \(\rightarrow\) the effective bias is computed with Eq.(2)
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
Delta_crit	\(\Delta_{crit}\): the critical overdensity
kk	wave vector module
interpType	method to interpolate the power spectrum
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed
prec	accuracy of the integration
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum

Returns: a vector containing the mean and standard deviation of the effective dark matter bias

Definition at line 241 of file Bias.cpp.

◆ bias_eff_selection_function() [1/3]

vector< double > cbl::cosmology::Cosmology::bias_eff_selection_function	(	const double	Mass_min,
		const double	Mass_max,
		const std::vector< double >	redshift,
		const std::string	model_bias,
		const std::string	model_MF,
		const std::string	method_SS,
		const std::string	selection_function_file,
		const std::vector< int >	column = `{}`,
		const double	alpha = `1.`,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const double	Delta_crit = `200.`,
		const double	kk = `-1.`,
		const std::string	interpType = `"Linear"`,
		const int	norm = `-1`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`
	)

effective bias of dark matter haloes, computed using a given selection function

this function computes the effective bias of dark matter haloes:

\[ b_{eff}(z) = \frac{\int_{M_{min}}^{M_{max}} {\rm d}M\, b(M, z) \Phi(M, z) f(M, z)}{\int_{M_{min}}^{M_{max}} {\rm d}M\,\Phi(M, z) f(M, z)} \]

in the current implementation, the integral is actually replaced by the Riemann sum, as follows:

\[ b_{eff}(z) \simeq \frac{\sum_{i_{min}}^{i_{max}} b(M, z) \Phi(M, z) f(M, z) (M_{i+1}-M_i)}{\sum_{i_{min}}^{i_{max}} \Phi(M, z) f(M, z) (M_{i+1}-M_i)} \]

where the halo mass function, \(\Phi(M, z)\), is computed by cbl::cosmology::Cosmology::mass_function, the linear bias, \(b(M, z)\), is computed by cbl::cosmology::Cosmology::bias_halo, and f(M, z) is the selection function

Parameters

Mass_min	minimum halo mass
Mass_max	maximum halo mass
redshift	vector containing the input redshifts
model_bias	author(s) who proposed the bias; valid authors are: ST99 (Sheth & Tormen 1999), SMT01 (Sheth, Mo & Tormen 2001), SMT01_WL04 (Sheth, Mo & Tormen 2001 with the correction of Warren 2004), Tinker (Tinker et al. 2010)
model_MF	author(s) who proposed the mass function; valid authors are: PS (Press & Schechter), ST (Sheth & Tormen), Jenkins (Jenkins et al. 2001), Warren (Warren et al. 2006), ShenH (halo MF, Shen et al. 2006), ShenF (filament MF, Shen et al. 2006), ShenS (sheet MF, Shen et al. 2006), Pan (Pan 2007), Peacock (Peacock at al. 2007), Reed (Reed et al. 2007), Tinker (Tinker et al. 2008), Crocce (Crocce et al. 2010), Manera (Manera et al. 2010), Courtin (Courtin et al. 2010), Bhattacharya (Bhattacharya et al. 2011), Angulo_FOF (FoF MF, Angulo et al. 2012), Angulo_Sub (SUBFIND MF, Angulo et al. 2012), Watson_FOF (FoF MF, Watson et al. 2012), Watson_SOH (Spherical Overdensity halo MF, Watson et al. 2012), Despali_Z0, Despali_AllZ, Despali_AllZAllCosmo, Despali_HighM (Despali et al. 2016)
method_SS	method used to compute the power spectrum and σ(mass); valid method_SS are: CAMB [http://camb.info/], CLASS [http://class-code.net/], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
selection_function_file	input file with the selection functon
column	vector containing the three columns of the selection function file to be read
alpha	the \(\alpha\) parameter of the cluster mass scaling relation
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
Delta_crit	\(\Delta_{crit}\): the critical overdensity
kk	wave vector module
interpType	method to interpolate the power spectrum
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed
prec	accuracy of the integration
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum

Returns: b_eff: the effective dark matter bias

Definition at line 483 of file Bias.cpp.

◆ bias_eff_selection_function() [2/3]

vector< double > cbl::cosmology::Cosmology::bias_eff_selection_function	(	const glob::FuncGrid	interp_sigma,
		const glob::FuncGrid	interp_DnSigma,
		const glob::FuncGrid	interp_SF,
		const double	Mass_min,
		const double	Mass_max,
		const std::vector< double >	redshift,
		const std::string	model_bias,
		const std::string	model_MF,
		const std::string	method_SS,
		const double	alpha = `1.`,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const double	Delta_crit = `200.`,
		const double	kk = `-1.`,
		const std::string	interpType = `"Linear"`,
		const int	norm = `-1`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`
	)

effective bias of dark matter haloes, computed using a given selection function; σ(mass) and dlnσ/dM are provided in input

this function computes the effective bias of dark matter haloes:

\[ b_{eff}(z) = \frac{\int_{M_{min}}^{M_{max}} {\rm d}M\, b(M, z) \Phi(M, z) f(M, z)}{\int_{M_{min}}^{M_{max}} {\rm d}M\,\Phi(M, z) f(M, z)} \]

in the current implementation, the integral is actually replaced by the Riemann sum, as follows:

\[ b_{eff}(z) \simeq \frac{\sum_{i_{min}}^{i_{max}} b(M, z) \Phi(M, z) f(M, z) (M_{i+1}-M_i)}{\sum_{i_{min}}^{i_{max}} \Phi(M, z) f(M, z) (M_{i+1}-M_i)} \]

where the halo mass function, \(\Phi(M, z)\), is computed by cbl::cosmology::Cosmology::mass_function, the linear bias, \(b(M, z)\), is computed by cbl::cosmology::Cosmology::bias_halo, and f(M, z) is the selection function

Parameters

interp_sigma	FuncGrid object containing the values of σ(mass) computed on a grid, used by interpolation
interp_DnSigma	FuncGrid object containing the values of dlnσ/dM computed on a grid, used by interpolation
interp_SF	FuncGrid object containing the values of the selection function computed on a grid in mass, at the mean redshift, used by interpolation
Mass_min	minimum halo mass
Mass_max	maximum halo mass
redshift	vector containing the input redshifts
model_bias	author(s) who proposed the bias; valid authors are: ST99 (Sheth & Tormen 1999), SMT01 (Sheth, Mo & Tormen 2001), SMT01_WL04 (Sheth, Mo & Tormen 2001 with the correction of Warren 2004), Tinker (Tinker et al. 2010)
model_MF	author(s) who proposed the mass function; valid authors are: PS (Press & Schechter), ST (Sheth & Tormen), Jenkins (Jenkins et al. 2001), Warren (Warren et al. 2006), ShenH (halo MF, Shen et al. 2006), ShenF (filament MF, Shen et al. 2006), ShenS (sheet MF, Shen et al. 2006), Pan (Pan 2007), Peacock (Peacock at al. 2007), Reed (Reed et al. 2007), Tinker (Tinker et al. 2008), Crocce (Crocce et al. 2010), Manera (Manera et al. 2010), Courtin (Courtin et al. 2010), Bhattacharya (Bhattacharya et al. 2011), Angulo_FOF (FoF MF, Angulo et al. 2012), Angulo_Sub (SUBFIND MF, Angulo et al. 2012), Watson_FOF (FoF MF, Watson et al. 2012), Watson_SOH (Spherical Overdensity halo MF, Watson et al. 2012), Despali_Z0, Despali_AllZ, Despali_AllZAllCosmo, Despali_HighM (Despali et al. 2016)
method_SS	method used to compute the power spectrum and σ(mass); valid method_SS are: CAMB [http://camb.info/], CLASS [http://class-code.net/], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
alpha	the \(\alpha\) parameter of the cluster mass scaling relation
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
Delta_crit	\(\Delta_{crit}\): the critical overdensity
kk	wave vector module
interpType	method to interpolate the power spectrum
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed
prec	accuracy of the integration
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum

Returns: b_eff: the effective dark matter bias

Warning: interp_sigma and interp_DnSigma have to be computed at the same cosmology of the object. They are provided as an input just to improve the performances in some applications (e.g. MCMC) where these quantities can be computed once

Definition at line 385 of file Bias.cpp.

◆ bias_eff_selection_function() [3/3]

vector< double > cbl::cosmology::Cosmology::bias_eff_selection_function	(	const glob::FuncGrid	interp_sigma,
		const glob::FuncGrid	interp_DnSigma,
		const glob::FuncGrid2D	interp_SF,
		const double	Mass_min,
		const double	Mass_max,
		const std::vector< double >	redshift,
		const std::string	model_bias,
		const std::string	model_MF,
		const std::string	method_SS,
		const double	alpha = `1.`,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const double	Delta_crit = `200.`,
		const double	kk = `-1.`,
		const std::string	interpType = `"Linear"`,
		const int	norm = `-1`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`
	)

effective bias of dark matter haloes, computed using a given selection function; σ(mass) and dlnσ/dM are provided in input

this function computes the effective bias of dark matter haloes:

\[ b_{eff}(z) = \frac{\int_{M_{min}}^{M_{max}} {\rm d}M\, b(M, z) \Phi(M, z) f(M, z)}{\int_{M_{min}}^{M_{max}} {\rm d}M\,\Phi(M, z) f(M, z)} \]

in the current implementation, the integral is actually replaced by the Riemann sum, as follows:

\[ b_{eff}(z) \simeq \frac{\sum_{i_{min}}^{i_{max}} b(M, z) \Phi(M, z) f(M, z) (M_{i+1}-M_i)}{\sum_{i_{min}}^{i_{max}} \Phi(M, z) f(M, z) (M_{i+1}-M_i)} \]

where the halo mass function, \(\Phi(M, z)\), is computed by cbl::cosmology::Cosmology::mass_function, the linear bias, \(b(M, z)\), is computed by cbl::cosmology::Cosmology::bias_halo, and f(M, z) is the selection function

Parameters

interp_sigma	FuncGrid object containing the values of σ(mass) computed on a grid, used by interpolation
interp_DnSigma	FuncGrid object containing the values of dlnσ/dM computed on a grid, used by interpolation
interp_SF	FuncGrid2D object containing the values of the selection function computed on a grid in mass and redshift, used by interpolation
Mass_min	minimum halo mass
Mass_max	maximum halo mass
redshift	vector containing the input redshifts
model_bias	author(s) who proposed the bias; valid authors are: ST99 (Sheth & Tormen 1999), SMT01 (Sheth, Mo & Tormen 2001), SMT01_WL04 (Sheth, Mo & Tormen 2001 with the correction of Warren 2004), Tinker (Tinker et al. 2010)
model_MF	author(s) who proposed the mass function; valid authors are: PS (Press & Schechter), ST (Sheth & Tormen), Jenkins (Jenkins et al. 2001), Warren (Warren et al. 2006), ShenH (halo MF, Shen et al. 2006), ShenF (filament MF, Shen et al. 2006), ShenS (sheet MF, Shen et al. 2006), Pan (Pan 2007), Peacock (Peacock at al. 2007), Reed (Reed et al. 2007), Tinker (Tinker et al. 2008), Crocce (Crocce et al. 2010), Manera (Manera et al. 2010), Courtin (Courtin et al. 2010), Bhattacharya (Bhattacharya et al. 2011), Angulo_FOF (FoF MF, Angulo et al. 2012), Angulo_Sub (SUBFIND MF, Angulo et al. 2012), Watson_FOF (FoF MF, Watson et al. 2012), Watson_SOH (Spherical Overdensity halo MF, Watson et al. 2012), Despali_Z0, Despali_AllZ, Despali_AllZAllCosmo, Despali_HighM (Despali et al. 2016)
method_SS	method used to compute the power spectrum and σ(mass); valid method_SS are: CAMB [http://camb.info/], CLASS [http://class-code.net/], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
alpha	the \(\alpha\) parameter of the cluster mass scaling relation
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
Delta_crit	\(\Delta_{crit}\): the critical overdensity
kk	wave vector module
interpType	method to interpolate the power spectrum
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed
prec	accuracy of the integration
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum

Returns: b_eff: the effective dark matter bias

Warning: interp_sigma and interp_DnSigma have to be computed at the same cosmology of the object. They are provided as an input just to improve the performances in some applications (e.g. MCMC) where these quantities can be computed once

Definition at line 438 of file Bias.cpp.

◆ bias_halo() [1/4]

double cbl::cosmology::Cosmology::bias_halo	(	const double	Mass,
		const double	redshift,
		const std::string	author,
		const std::string	method_SS,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const std::string	interpType = `"Linear"`,
		const double	Delta = `200.`,
		const double	kk = `-1.`,
		const int	norm = `-1`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`
	)

bias of dark matter haloes

Parameters

Mass	halo mass
redshift	the redshift
author	author(s) who proposed the bias; valid authors are: ST99 (Sheth & Tormen 1999), SMT01 (Sheth, Mo & Tormen 2001), SMT01_WL04 (Sheth, Mo & Tormen 2001 with the correction of Warren 2004), Tinker (Tinker et al. 2010)
method_SS	method used to compute the power spectrum and σ(mass); valid method_SS are: CAMB [http://camb.info/], CLASS [http://class-code.net/], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
interpType	method to interpolate the power spectrum
Delta	\(\Delta\), the overdensity
kk	wave vector module
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed
prec	accuracy of the integration
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum

Returns: b_halo: the dark matter bias

Warning: the input parameter \(\Delta\) is the background overdensity, not the critical overdensity \(\Delta_{crit}\); divide \(\Delta_{crit}\) by \(\Omega_M(z)\) (see cbl::cosmology::Cosmology::OmegaM) to obtain the background overdensity

Definition at line 44 of file Bias.cpp.

◆ bias_halo() [2/4]

double cbl::cosmology::Cosmology::bias_halo	(	const double	Mass,
		const double	Sigma,
		const double	redshift,
		const double	DN,
		const std::string	model_bias,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const std::string	interpType = `"Linear"`,
		const double	Delta = `200.`,
		const double	kk = `-1.`,
		const int	norm = `-1`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`,
		const std::string	method_SS = `"CAMB"`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`
	)

bias of dark matter haloes

Parameters

Mass	halo mass
Sigma	σ(mass, z=0): the mass variance at z=0
redshift	the redshift
DN	normalised amplitude of the growing mode at a given redshift
model_bias	author(s) who proposed the bias; valid authors are: ST99 (Sheth & Tormen 1999), SMT01 (Sheth, Mo & Tormen 2001), SMT01_WL04 (Sheth, Mo & Tormen 2001 with the correction of Warren 2004), Tinker (Tinker et al. 2010)
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
interpType	method to interpolate the power spectrum
Delta	\(\Delta\), the overdensity
kk	wave vector module
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed
prec	accuracy of the integration
method_SS	method used to compute the power spectrum and σ(mass); valid method_SS are: CAMB [http://camb.info/], CLASS [http://class-code.net/], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum

Returns: b_halo: the dark matter bias

Warning: the input parameter \(\Delta\) is the background overdensity, not the critical overdensity \(\Delta_{crit}\); divide \(\Delta_{crit}\) by \(\Omega_M(z)\) (see cbl::cosmology::Cosmology::OmegaM) to obtain the background overdensity

Definition at line 75 of file Bias.cpp.

◆ bias_halo() [3/4]

double cbl::cosmology::Cosmology::bias_halo	(	const double	Mass,
		const double	Sigma,
		const double	redshift,
		const std::string	model_bias,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const std::string	interpType = `"Linear"`,
		const double	Delta = `200.`,
		const double	kk = `-1.`,
		const int	norm = `-1`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`,
		const std::string	method_SS = `"CAMB"`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`
	)

bias of dark matter haloes

Parameters

Mass	halo mass
Sigma	σ(mass, z=0): the mass variance at z=0
redshift	the redshift
model_bias	author(s) who proposed the bias; valid authors are: ST99 (Sheth & Tormen 1999), SMT01 (Sheth, Mo & Tormen 2001), SMT01_WL04 (Sheth, Mo & Tormen 2001 with the correction of Warren 2004), Tinker (Tinker et al. 2010)
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
interpType	method to interpolate the power spectrum
Delta	\(\Delta\), the overdensity
kk	wave vector module
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed
prec	accuracy of the integration
method_SS	method used to compute the power spectrum and σ(mass); valid method_SS are: CAMB [http://camb.info/], CLASS [http://class-code.net/], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum

Returns: b_halo: the dark matter bias

Warning: the input parameter \(\Delta\) is the background overdensity, not the critical overdensity \(\Delta_{crit}\); divide \(\Delta_{crit}\) by \(\Omega_M(z)\) (see cbl::cosmology::Cosmology::OmegaM) to obtain the background overdensity

Definition at line 61 of file Bias.cpp.

◆ bias_halo() [4/4]

vector< double > cbl::cosmology::Cosmology::bias_halo	(	const std::vector< double >	Mass,
		const std::vector< double >	Sigma,
		const double	redshift,
		const std::string	model_bias,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const std::string	interpType = `"Linear"`,
		const double	Delta = `200.`,
		const double	kk = `-1.`,
		const int	norm = `-1`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`,
		const std::string	method_SS = `"CAMB"`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`
	)

bias of dark matter haloes, for a vector of masses

Parameters

Mass	halo mass
Sigma	σ(mass, z=0): the mass variance at z=0
redshift	the redshift
model_bias	author(s) who proposed the bias; valid authors are: ST99 (Sheth & Tormen 1999), SMT01 (Sheth, Mo & Tormen 2001), SMT01_WL04 (Sheth, Mo & Tormen 2001 with the correction of Warren 2004), Tinker (Tinker et al. 2010)
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
interpType	method to interpolate the power spectrum
Delta	\(\Delta\), the overdensity
kk	wave vector module
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed
prec	accuracy of the integration
method_SS	method used to compute the power spectrum and σ(mass); valid method_SS are: CAMB [http://camb.info/], CLASS [http://class-code.net/], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum

Returns: b_halo: the dark matter bias

Warning: the input parameter \(\Delta\) is the background overdensity, not the critical overdensity \(\Delta_{crit}\); divide \(\Delta_{crit}\) by \(\Omega_M(z)\) (see cbl::cosmology::Cosmology::OmegaM) to obtain the background overdensity

Definition at line 44 of file Bias_vector.cpp.

◆ bispectrum()

double cbl::cosmology::Cosmology::bispectrum	(	const std::vector< double >	kk,
		const std::string	method_Pk,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const int	norm = `-1`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`,
		const std::string	file_par = `par::defaultString`
	)

the bispectrum

Author: Cosimo Fedeli; cosim.nosp@m.o.fe.nosp@m.deli@.nosp@m.oabo.nosp@m..inaf.nosp@m..it

Parameters

kk	wave vector module
method_Pk	method used to compute the power spectrum (i.e. the Boltzmann solver); valid choices for method_Pk are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	the output_root parameter of the parameter file used to compute the power spectrum; it can be any name. If this parameter is different from the default value it will be used also in the output directory name
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
prec	accuracy of the integration
file_par	name of the parameter file; if a parameter file is provided (i.e. file_par!=NULL), it will use be used, ignoring the cosmological parameters of the object

Returns: the potential spectral amplitude

Definition at line 68 of file NG.cpp.

◆ C_l_DM()

std::vector< double > cbl::cosmology::Cosmology::C_l_DM	(	const int	lmax,
		const std::vector< double >	zz,
		const std::vector< double >	phiz,
		const std::string	interpolationMethod,
		const std::string	method_Pk = `"CAMB"`,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const int	norm = `-1`,
		const double	k_min = `1.e-4`,
		const double	k_max = `100`,
		const double	prec = `1.e-2`,
		const std::string	file_par = `par::defaultString`
	)

the dark matter angular linear power spectrum \(C_l\).

this function provides the angular linear power spectrum using the Limber approximation up to a given \(l_{max}\):

\[ C_l = \int_{z_{min}}^{z_{max}}\phi^2(z) D^2(z) P(\frac{l}{D_C(z)}) \frac{H(z)}{c \cdot D_c(z)} dz \]

where l is the multipole order, \(\phi(z)\) is the tracers redshift distribution, \(P\) is the \(z=0\) power spectrum and \(D(z)\) is the growth factor. \(D_C(z)\) and \(H(z)\) are respectively the comoving function and the Hubble parameter.

Parameters

lmax	the maximum multipole order
zz	the redshift range
phiz	the number density
interpolationMethod	the method in interpolation
method_Pk	method used to compute the power spectrum (i.e. the Boltzmann solver); valid choices for method_Pk are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
norm	0 \(\rightarrow\) don't normalize the power spectrum; 1 \(\rightarrow\) normalize the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed
k_max	maximum wave vector module up to which the power spectrum is computed
prec	accuracy of the integration
file_par	name of the parameter file; if a parameter file is provided (i.e. file_par!=NULL), it will be used, ignoring the cosmological parameters of the object

Returns: vector containing the angular linear power spectrum up to \(l_{max}\)

Definition at line 2636 of file PkXi.cpp.

◆ c_vir()

double cbl::cosmology::Cosmology::c_vir	(	const double	c200,
		const double	redshift,
		const std::string	author = `"BryanNorman"`
	)		const

virial halo concentration given \(c_{200}\)

this function provides an approximate conversion to compute \(c_{vir}\) from \(c_{200}\) (from Coe 2010):

\[c_{vir}\simeq a\,c_{200}+b\]

\[a\simeq-1.119\log\Delta_c(z)+3.537\]

\[b\simeq-0.967\log\Delta_c(z)+2.181\]

where \(\Delta_c(z)\) is computed by cbl::cosmology::Cosmology::Delta_c

Parameters

c200	\(c_{200}\)
redshift	the redshift
author	the author of the \(\Delta_c(z)\) equation (see cbl::cosmology::Cosmology::Delta_c)

Returns: \(c_{vir}\)

Definition at line 1340 of file Cosmology.cpp.

◆ CMN()

double cbl::cosmology::Cosmology::CMN	(	const double	rr,
		const double	k_int_min,
		const std::string	method_Pk,
		const double	redshift,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const double	k_max = `100.`,
		const std::string	file_par = `par::defaultString`
	)		const

the Cosmic Mach Number

Parameters

rr	comoving radius
k_int_min	minimum wave vector module up to which the integral is computed
method_Pk	method used to compute the power spectrum and σ(mass) (i.e. the Boltzmann solver); valid choices for method_Pk are: CAMB [http://camb.info/], CLASS [http://class-code.net/], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
redshift	the redshift
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
k_max	maximum wave vector module up to which the power spectrum is computed
file_par	name of the parameter file; if a parameter file is provided (i.e. file_par!=NULL), it will be used, ignoring the cosmological parameters of the object

Returns: the Cosmic Mach Number

Definition at line 132 of file Velocities.cpp.

◆ concentration_NFW_Duffy()

double cbl::cosmology::Cosmology::concentration_NFW_Duffy	(	const double	Mass,
		const double	redshift,
		const std::string	halo_def = `"vir"`
	)		const

the halo concentration-mass relation for NFW prfile and Duffy model

This function computes the concentration of a dark matter halo of a given a mass, at a given redshift following Duffy et al. 2008 model:

\[c(M_h, z) = A(M_h/M_{pivot})^B\,(1+z)^C\]

Parameters

Mass	the halo mass.
redshift	the redshift (must be < 2).
halo_def	the halo definition; available options are: "vir" \(\rightarrow\) all matter withing the radius \(r_{vir}\) for which the mean internal density is \(\Delta\) times the critical density \(\rho_{crit}=3H^2/8\pi G\); "200" \(\rightarrow\) all matter withing the radius \(r_{200}\) for which the mean internal density is 200 times the critical density; "mean" \(\rightarrow\) all matter withing the radius \(r_{200}\) for which the mean internal density is 200 times the critical mean background density.

Returns: the halo concentration for NFW profile and Duffy model.

Warning: the Duffy et al. concentrantion-mass relation refers to the 0<z<2 redshift range, obtained from their full samples (see Table 1 of Duffy et al. 2008); actually, the current implementation does not depend on cosmology.

Definition at line 1461 of file Cosmology.cpp.

◆ converted_mass()

double cbl::cosmology::Cosmology::converted_mass	(	const double	mass,
		const cosmology::Cosmology	cosmology,
		const double	redshift,
		const double	redshift_source = `-1.`
	)		const

convert a cluster mass estimated in a different cosmology

this function converts a cluster mass estimated assuming a different cosmology, following Eq.C4 of Sereno & Ettori 2015 (https://arxiv.org/abs/1407.7868)

\[ M^{(2)} = M^{(1)} \left( \frac{D_{ds}^{(1)}}{D_s^{(1)}} \right)^{3/2} H^{(1)} \left( \frac{D_{ds}^{(2)}}{D_s^{(2)}}\right)^{-3/2} H^{(2) -1} \]

where and \(D_s\) and \(D_{ds}\) are the source and the lens-source angular diameter distances, respectively

Parameters

mass	the cluster mass to be converted (since estimated in a different cosmology), \(M^{(1)}\)
cosmology	the cosmology assumed to measure the cluster mass
redshift	redshift of the cluster
redshift_source	redshift of the source, if the cluster mass is estimated from weak lensing, -1 otherwise

Returns: the cluster mass converted in this cosmology, \(M^{(2)}\)

Definition at line 962 of file MassFunction.cpp.

◆ cosmic_time()

double cbl::cosmology::Cosmology::cosmic_time ( const double redshift = 0. ) const

cosmic time at a given redshift

Parameters

redshift the redshift

Returns: t_cosmic [Gyr]

Definition at line 947 of file Cosmology.cpp.

◆ create_grid_sigmaM()

std::string cbl::cosmology::Cosmology::create_grid_sigmaM	(	const std::string	method_SS,
		const double	redshift,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const std::string	interpType = `"Linear"`,
		const double	k_max = `100.`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`
	)		const

auxiliary function to create a grid file with σ(M)

Parameters

method_SS	method used to compute the power spectrum and σ(mass); valid method_SS are: CAMB [http://camb.info/], CLASS [http://class-code.net/], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
redshift	the redshift
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
interpType	method to interpolate the power spectrum
k_max	maximum wave vector module up to which the power spectrum is computed
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum

Returns: file_grid name of the file where the grid is stored

Definition at line 298 of file Sigma.cpp.

◆ cumPw()

double cbl::cosmology::Cosmology::cumPw	(	const double	ww,
		const double	ff,
		const std::string	author
	)		const

cumulative distribution

this function provides the cumulative rescaled and generalized formation redshift distribution

Author: Carlo Giocoli; cgioc.nosp@m.oli@.nosp@m.gmail.nosp@m..com

Parameters

ww	rescaled variable w as in Lacey and Coles 1993
ff	assembled fraction
author	valid authors are: NS (Nusser and Sheth), GTS (Giocoli et al. 2012)

Returns: P(w): cumulative distribution

Definition at line 97 of file MassGrowth.cpp.

◆ D_A() [1/2]

double cbl::cosmology::Cosmology::D_A ( const double redshift ) const

the angular diameter distance at a given redshift

Parameters

redshift the redshift

Returns: D_A

Definition at line 848 of file Cosmology.cpp.

◆ D_A() [2/2]

double cbl::cosmology::Cosmology::D_A	(	const double	z1,
		const double	z2
	)		const

the angular diameter distance between objects at two redshifts

this function provides the angular diameter distance \(D_{A,12}\) between two objects at redshifts \(z_1\) and \(z_2\), as follows:

\[ D_{A,12} = \frac{1}{1+z_2} \left[ D_M(z_2)\sqrt{1+\Omega_k\frac{D_M^2(z_1)}{D_H^2}} - D_M(z_1)\sqrt{1+\Omega_k\frac{D_M^2(z_2)}{D_H^2}} \right] \]

(e.g. Eq.19 of Hogg 2000)

Parameters

z1	the redshift of the first object
z2	the redshift of the second object

Returns: D_A between z1 and z2

Warning: the implemented formula is not correct for \(\Omega_k<0\)

Definition at line 857 of file Cosmology.cpp.

◆ D_C()

double cbl::cosmology::Cosmology::D_C ( const double redshift ) const

the comoving line-of-sight distance at a given redshift

for demonstration, see distances.cpp

Parameters

redshift the redshift

Returns: D_C

Definition at line 741 of file Cosmology.cpp.

◆ D_C_LCDM()

double cbl::cosmology::Cosmology::D_C_LCDM ( const double redshift ) const

the comoving line-of-sight distance at a given redshift

this method provides the comoving distance for a given redshift using elliptic integrals (see Numer. Math. (2010) 116:687–719, T. Fukushima "Fast computation of incomplete elliptic integral of first kind by half argument transformation")

d(z) is computed using the following formula, taken from A. Meszaros & J. Ripa 2013, arXiv:1306.4736,

d(z) = C*[F(φ₀,m)-F(φ₁,m)]

where

C = 3^-1/4 / (Ω_M^1/3*Ω_Λ^1/6)

φ₀ = arccos( [1+(1-3^0.5)*(Ω_Λ/Ω_M)^1/3] / [1+(1+3^0.5)*(Ω_Λ/Ω_M)^1/3] )

φ₁ = arccos( [1+(1-3^0.5)*(Ω_Λ/Ω_M)^1/3*(1+z)] / [1+(1+3^0.5)*(Ω_Λ/Ω_M)^1/3*(1+z)] )

F(φ, m) is the incomplete elliptic integral of the first kind, with argument φ

m = (2+3^0.5)/4 is the elliptic integral shape parameter

for demonstration, see distances.cpp

Author: Mauro Roncarelli; mauro.nosp@m..ron.nosp@m.carel.nosp@m.li@u.nosp@m.nibo..nosp@m.it

Parameters

redshift the redshift

Returns: D_C

Warning: this method works only for a flat ΛCDM universe at low enough redshifts where Ω_r is negligible; it does not work for non-standard dark energy or non-flat models

Definition at line 1351 of file Cosmology.cpp.

◆ D_C_table()

void cbl::cosmology::Cosmology::D_C_table	(	const std::string	file_table,
		const double	z_min,
		const double	z_max,
		const int	step,
		std::vector< double > &	Redshift,
		std::vector< double > &	dc
	)		const

create a table of [redshift, comoving line-of-sight distance]

this function is used to create a table of [redshift, comoving line-of-sight distance], useful to speed up the analysis

Parameters

[in]	file_table	name of the file where the table is stored
[in]	z_min	minimum redshift of the table
[in]	z_max	maximum redshift of the table
[in]	step	redshift step
[out]	Redshift	vector of redshifts
[out]	dc	vector of comoving line-of-sight distances

Definition at line 794 of file Cosmology.cpp.

◆ D_H()

double cbl::cosmology::Cosmology::D_H ( ) const

inline

get the private member Cosmology::m_D_H

Returns: D_H: the Hubble distance

Definition at line 1205 of file Cosmology.h.

◆ D_L()

double cbl::cosmology::Cosmology::D_L ( const double redshift ) const

the luminosity distance at a given redshift

Parameters

redshift the redshift

Returns: D_L

Definition at line 875 of file Cosmology.cpp.

◆ D_M()

double cbl::cosmology::Cosmology::D_M ( const double redshift ) const

the comoving transverse distance at a given redshift

Parameters

redshift the redshift

Returns: D_M

Definition at line 832 of file Cosmology.cpp.

◆ D_V()

double cbl::cosmology::Cosmology::D_V ( const double redshift ) const

the average distance at a given redshift, used to rescale the correlation function

Parameters

redshift the redshift

Returns: D_V

Definition at line 884 of file Cosmology.cpp.

◆ DD()

double cbl::cosmology::Cosmology::DD ( const double redshift ) const

the amplitude of the growing mode at a given redshift, \(D(z)\)

this function computes the following quantity (see Eq.(15) by Percival (2005), A&A 443, 819):

\[ D(z) = \frac{5 \Omega_{M,0} }{2} E(a) \int_0^a \frac{{\rm d}\,a'}{[a' E(a')]^3} \]

where \(a=1/(1+z)\)

Parameters

redshift the redshift

Returns: the amplitude of the growing mode

Warning: the current implementation is valid only for ΛCDM cosmologies (e.g. Percival (2005) A&A 443, 819, and references therein)

Definition at line 702 of file Cosmology.cpp.

◆ Delta_c()

double cbl::cosmology::Cosmology::Delta_c	(	const double	redshift,
		const std::string	author = `"BryanNorman"`
	)		const

the critical overdensity

this function computes the critical overdensity, \(\Delta_c(z)\equiv\Delta^{vir}_c(z)\), using approximated equations valid only for a flat Universe (see e.g. Coe 2010), where \(\rho_{vir} = \Delta^{vir}_c\rho_c = \Delta^{vir}_b\rho_m = \Delta^{vir}_b\Omega_M\rho_c\):

Bryan & Norman (1998)

\[\Delta_c\simeq18\pi^2+60x-32x^2\, \mbox{for}\, \Omega_\Lambda=0\]

\[\Delta_c\simeq18\pi^2+82x-39x^2\, \mbox{for}\, \Omega_k=0\]

\[x=\Omega_M(z)-1\]
Eke et al. (1998)

\[\Delta_c\simeq178\Omega_M(z)^{0.3}\, \mbox{for}\, \Omega_\Lambda=0\]

\[\Delta_c\simeq178\Omega_M(z)^{0.45}\, \mbox{for}\, \Omega_k=0\]
Nakamura & Suto (1998)

\[\Delta_c\simeq18\pi^2(1+0.4093x^{2.7152})\Omega_M(z)\]

\[x=(1-\Omega_{M,0})^{1/3}(1+z)^{-1}\]

Parameters

redshift	the redshift
author	the author of the equation implemented; available options are: "BryanNorman", "Eke", "NakamuraSuto"

Returns: \(\Delta_c\)

Warning: The implemented functions are approximated, and valid only for a restricted range of cosmological parameters (see the reported references)

Definition at line 1283 of file Cosmology.cpp.

◆ deltac()

double cbl::cosmology::Cosmology::deltac ( const double redshift ) const

spherical collapse density threshold at a given redshift

this function computes the spherical collapse density threshold, \(\delta_c\), by using the approximated equation (C.28) provided by Nakamura & Suto (1997)

\[\delta_c(z) \simeq \frac{3}{20}(12\pi)^{2/3} \{1.+0.012299\log[\Omega_M(z)]\}\]

Parameters

redshift the redshift

Returns: \(\delta_c\)

Examples: modelling_VoidAbundances.cpp.

Definition at line 1248 of file Cosmology.cpp.

◆ deltav_L()

double cbl::cosmology::Cosmology::deltav_L	(	const double	deltav_NL,
		const double	b_eff,
		double	slope = `0.854`,
		double	offset = `0.420`
	)		const

Linear (under)density contrast.

Author: Tommaso Ronconi; tomma.nosp@m.so.r.nosp@m.oncon.nosp@m.i@st.nosp@m.udio..nosp@m.unib.nosp@m.o.it

Parameters

deltav_NL	the non linear density contrast: \(\rho_v/\rho_m\) (default value set to \(-0.795\))
b_eff	the effective bias of the sample
slope	first coefficent to convert the effective bias (default value set to \(0.854\))
offset	second coefficent to convert the effective bias (default value set to \(0.420\))

Returns: The linear density contrast used as second barrier in the excursion set formalism for voids, based on the fit by Bernardeu (1994): \(\delta_v^L \equiv \frac{\rho_v - \rho_m}{\rho_m} \approx C [1 - (\rho_v/\rho_m)^{- 1/C}]\) where \(\rho_v =\ \) average void density, \(\rho_m =\ \) average density of the surrounding Universe and \(C = 1.594\), a costant.

Definition at line 44 of file SizeFunction.cpp.

◆ deltav_NL()

double cbl::cosmology::Cosmology::deltav_NL ( const double deltav = -2.71 ) const

Non-Linear (under)density contrast.

Author: Tommaso Ronconi; tomma.nosp@m.so.r.nosp@m.oncon.nosp@m.i@st.nosp@m.udio..nosp@m.unib.nosp@m.o.it

Parameters

deltav the linear density contrast: \(\delta_v\) (default value set to \(-2.71\))

Returns: The non linear density contrast to be used in samples of tracers, independently of the bias value, based on the fit by Bernardeu (1994): \( \delta_v^{NL} \equiv \frac{\rho_v}{\rho_m} - 1 \approx \bigl(1 - C^{-1}\delta_v^L\bigr)^{-C} - 1\) where \(\rho_v =\ \) average void density, \(\rho_m =\ \) average density of the surrounding Universe and \(C = 1.594\), a costant.

Definition at line 56 of file SizeFunction.cpp.

◆ denominator_Q()

double cbl::cosmology::Cosmology::denominator_Q	(	const double	r1,
		const double	r2,
		const double	theta,
		const std::vector< double >	rr,
		const std::vector< double >	xi_matter
	)		const

the normalization factor for reduced three-point correlation function

this function computes the normalization factor for reduced three-point correlation function:

\[ \xi(r_1)\cdot\xi(r_2) + \xi(r_2)\cdot\xi(r_3) + \xi(r_3)\cdot\xi(r_1) \]

with \( r_3 = \sqrt{r_1^2+r_2^2-2 r_1 r_2 \cos(\theta)} \)

Parameters

r1	the first side of the triangle
r2	the second side of the triangle
theta	the angle between r1 and r2
rr	vector containing the scales at which the two-point correlation function is computed
xi_matter	vector containing the dark matter two-point correlation function values, estimated at the scales given in rr

Returns: the normalization factor for reduced three-point correlation function

Definition at line 47 of file 3PCF.cpp.

◆ Distance()

double cbl::cosmology::Cosmology::Distance	(	const double	redshift,
		const std::string	distance_type
	)		const

the distance at a given redshift

The distances available are: D_C,D_L,D_A,D_V, D_V/r_s, r_s/D_V

Author: Alfonso Veropalumbo; alfon.nosp@m.so.v.nosp@m.eropa.nosp@m.lumb.nosp@m.o@uni.nosp@m.bo.i.nosp@m.t

Parameters

redshift	the redshift
distance_type	the type of distance to return

Returns: Distance

Definition at line 902 of file Cosmology.cpp.

◆ DN()

double cbl::cosmology::Cosmology::DN	(	const double	redshift,
		const double	redshift_norm = `0.`,
		const double	prec = `1.e-4`
	)		const

the normalised amplitude of the growing mode at a given redshift, \(D(z)/D(0)\)

this function computes the following quantity:

\[ \frac{D(z)}{D(z_{norm})} = \exp{\int_{a_{norm}}^{a} \frac{f}{a'} {\rm d}a'} \]

where \(a=1/(1+z)\), \(a_{norm}=1/(1+z_{norm})\), and \(f\) is the linear growth rate computed by cbl::cosmology::Cosmology::linear_growth_rate

Parameters

redshift	the redshift
redshift_norm	the redshift at with the amplitude of the growing mode is normalised
prec	precision used for the resolution of the differential equation when the the normalised growth factor is computed

Returns: the amplitude of the growing mode

Definition at line 691 of file Cosmology.cpp.

◆ dnsigma2M()

double cbl::cosmology::Cosmology::dnsigma2M	(	const int	nd,
		const double	mass,
		const std::string	method_Pk,
		const double	redshift,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const std::string	interpType = `"Linear"`,
		const double	k_max = `100.`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`,
		const bool	unit1 = `false`
	)		const

the first derivative of the mass variance, \({\rm d}^n\sigma^2(M)/{\rm d}M^n\)

Parameters

nd	the derivative order, \(n\)
mass	the mass, \(M\)
method_Pk	method used to compute the power spectrum (i.e. the Boltzmann solver); valid choices for method_Pk are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
redshift	the redshift
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	the output_root parameter of the parameter file used to compute the power spectrum; it can be any name. If this parameter is different from the default value it will be used also in the output directory name
interpType	method to interpolate the power spectrum
k_max	maximum wave vector module up to which the power spectrum is computed
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum
unit1	true \(\rightarrow\) force cosmological units

Returns: the first derivative of the mass variance

Warning: the current implementation computes the derivative using the simplest numerical approximation, with fixed incremental step; it is computationally efficient, but the accuracy might be low

Definition at line 254 of file Sigma.cpp.

◆ dnsigma2R()

double cbl::cosmology::Cosmology::dnsigma2R	(	const int	nd,
		const double	radius,
		const std::string	method_Pk,
		const double	redshift,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const std::string	interpType = `"Linear"`,
		const double	k_max = `100.`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`,
		const bool	unit1 = `false`
	)		const

the nth-order derivative of the mass variance, \({\rm d}^n\sigma^2(R)/{\rm d}R^n\)

Parameters

nd	the derivative order, \(n\)
radius	the radius, \(R\)
method_Pk	method used to compute the power spectrum (i.e. the Boltzmann solver); valid choices for method_Pk are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
redshift	the redshift
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	the output_root parameter of the parameter file used to compute the power spectrum; it can be any name. If this parameter is different from the default value it will be used also in the output directory name
interpType	method to interpolate the power spectrum
k_max	maximum wave vector module up to which the power spectrum is computed
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum
unit1	true \(\rightarrow\) force cosmological units

Returns: the nth-order derivative of the mass variance

Warning: the current implementation computes the derivative using the simplest numerical approximation, with fixed incremental step; it is computationally efficient, but the accuracy might be lowt

Definition at line 176 of file Sigma.cpp.

◆ dskewnessdM()

double cbl::cosmology::Cosmology::dskewnessdM	(	const double	mass,
		const std::string	method_Pk,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const std::string	interpType = `"Linear"`,
		const int	norm = `-1`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`
	)

the derivative of the skewness, ds/dM

Author: Cosimo Fedeli; cosim.nosp@m.o.fe.nosp@m.deli@.nosp@m.oabo.nosp@m..inaf.nosp@m..it

Parameters

mass	halo mass
method_Pk	method used to compute the power spectrum (i.e. the Boltzmann solver); valid choices for method_Pk are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	the output_root parameter of the parameter file used to compute the power spectrum; it can be any name. If this parameter is different from the default value it will be used also in the output directory name
interpType	method to interpolate the power spectrum
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
prec	accuracy of the integration
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum

Returns: derivative of the skewness

Definition at line 509 of file NG.cpp.

◆ dV_dZdOmega()

double cbl::cosmology::Cosmology::dV_dZdOmega	(	const double	redshift,
		const bool	angle_rad
	)		const

the derivative of the comoving volume, d²V/(dz*dΩ) at a given redshift

Parameters

redshift	the redshift
angle_rad	false \(\rightarrow\) Ω in square degrees; true \(\rightarrow\) Ω in steradians

Returns: d²V/(dz*dΩ)

Definition at line 1236 of file Cosmology.cpp.

◆ EE()

double cbl::cosmology::Cosmology::EE ( const double redshift = 0. ) const

auxiliary function used to compute the Hubble function

Parameters

redshift the redshift

Returns: E=H/H₀

Definition at line 561 of file Cosmology.cpp.

◆ EE2()

double cbl::cosmology::Cosmology::EE2 ( const double redshift = 0. ) const

auxiliary function used to compute the deceleration parameter

Parameters

redshift the redshift

Returns: E²

Definition at line 964 of file Cosmology.cpp.

◆ EE_inv()

double cbl::cosmology::Cosmology::EE_inv ( const double redshift = 0. ) const

inline

inverse of the auxiliary function used to compute the Hubble function integrand of the comoving distance

Parameters

redshift the redshift

Returns: 1./E=H₀/H

Definition at line 1910 of file Cosmology.h.

◆ EE_inv2()

double cbl::cosmology::Cosmology::EE_inv2 ( const double redshift = 0. ) const

inline

inverse of the auxiliary function used to compute the Hubble function, integrand of the lookback time

Parameters

redshift the redshift

Returns: 1/(1+z)/E=H₀/H

Definition at line 1919 of file Cosmology.h.

◆ EE_inv3()

double cbl::cosmology::Cosmology::EE_inv3 ( const double aa ) const

inline

inverse of the auxiliary function used to compute the Hubble function integrand of the cosmic time

Parameters

aa 1/(1+z)

Returns: (1+z)/E=H₀/H

Definition at line 1928 of file Cosmology.h.

◆ eff_l_l1()

void cbl::cosmology::Cosmology::eff_l_l1	(	std::vector< std::vector< double >> &	eff,
		const std::vector< double >	rr,
		const int	l,
		const int	l1,
		const std::vector< double >	kk,
		const std::vector< double >	Pk
	)

compute the power spectrum integral transform

this function computes the power spectrum integral transform:

\[ f_{l, l_1} (r_i;r)= \int \frac{k^2\mathrm{d}k}{2\pi^2} j_l(kr_i) j_{l_1} (kr) k P(k) \]

where \(l, l_1\) are the orders of the transform.

Parameters

eff	the power spectrum transform \( f_{l, l_1} (r_i;r) \)
rr	vector of scales
l	the order \(l\)
l1	the order \(l_1\)
kk	vector of wavevector modules
Pk	dark matter power spectrum

Definition at line 819 of file 3PCF.cpp.

◆ error_beta() [1/3]

double cbl::cosmology::Cosmology::error_beta	(	const double	Mass_min,
		const double	Mass_max,
		const double	redshift,
		const std::string	model_bias,
		const std::string	model_MF,
		const std::string	method_SS,
		const double	err_bias,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const double	Delta = `200.`,
		const double	kk = `-1.`,
		const std::string	interpType = `"Linear"`,
		const int	norm = `-1`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`
	)

the specific growth rate β

Parameters

Mass_min	minimum halo mass
Mass_max	maximum halo mass
redshift	the redshift
model_bias	author(s) who proposed the bias; valid authors are: ST99 (Sheth & Tormen 1999), SMT01 (Sheth, Mo & Tormen 2001), SMT01_WL04 (Sheth, Mo & Tormen 2001 with the correction of Warren 2004), Tinker (Tinker et al. 2010)
model_MF	author(s) who proposed the mass function; valid authors are: PS (Press & Schechter), ST (Sheth & Tormen), Jenkins (Jenkins et al. 2001), Warren (Warren et al. 2006), ShenH (halo MF, Shen et al. 2006), ShenF (filament MF, Shen et al. 2006), ShenS (sheet MF, Shen et al. 2006), Pan (Pan 2007), Peacock (Peacock at al. 2007), Reed (Reed et al. 2007), Tinker (Tinker et al. 2008), Crocce (Crocce et al. 2010), Manera (Manera et al. 2010), Courtin (Courtin et al. 2010), Bhattacharya (Bhattacharya et al. 2011), Angulo_FOF (FoF MF, Angulo et al. 2012), Angulo_Sub (SUBFIND MF, Angulo et al. 2012), Watson_FOF (FoF MF, Watson et al. 2012), Watson_SOH (Spherical Overdensity halo MF, Watson et al. 2012), Despali_Z0, Despali_AllZ, Despali_AllZAllCosmo, Despali_HighM (Despali et al. 2016)
method_SS	method used to compute the power spectrum and σ(mass); valid method_SS are: CAMB [http://camb.info/], CLASS [http://class-code.net/], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
err_bias	error on the bias
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
Delta	\(\Delta\), the overdensity
kk	wave vector module
interpType	method to interpolate the power spectrum
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed
prec	accuracy of the integration
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum

Returns: error on β=f/b, where f is the linear growth rate and b is the bias

Warning: the input parameter \(\Delta\) is the background overdensity, not the critical overdensity \(\Delta_{crit}\); divide \(\Delta_{crit}\) by \(\Omega_M(z)\) (see cbl::cosmology::Cosmology::OmegaM) to obtain the background overdensity; the mass function by Manera et al. (2010) has been tested only for z=0 and z=0.5; the mass function by Despali et al. (2016) is currently implemented only for virial masses and at \(z<1.25\)

Definition at line 82 of file RSD.cpp.

◆ error_beta() [2/3]

double cbl::cosmology::Cosmology::error_beta	(	const double	redshift,
		const double	bias,
		const double	err_bias
	)		const

the error on the specific growth rate β

Parameters

redshift	the redshift
bias	bias
err_bias	error on the bias

Returns: error on β=f/b, where f is the linear growth rate and b is the bias

Definition at line 64 of file RSD.cpp.

◆ error_beta() [3/3]

double cbl::cosmology::Cosmology::error_beta	(	const std::vector< double >	MM,
		const std::vector< double >	MF,
		const double	redshift,
		const std::string	model_bias,
		const std::string	method_SS,
		const double	err_bias,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const double	Delta = `200.`,
		const double	kk = `-1.`,
		const std::string	interpType = `"Linear"`,
		const int	norm = `-1`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`
	)

the error on the specific growth rate β

Parameters

MM	vector of halo masses
MF	vector of mass function values, dΦ/dM=dn(M)/dM
redshift	the redshift
model_bias	author(s) who proposed the bias; valid authors are: ST99 (Sheth & Tormen 1999), SMT01 (Sheth, Mo & Tormen 2001), SMT01_WL04 (Sheth, Mo & Tormen 2001 with the correction of Warren 2004), Tinker (Tinker et al. 2010)
method_SS	method used to compute the power spectrum and σ(mass); valid method_SS are: CAMB [http://camb.info/], CLASS [http://class-code.net/], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
err_bias	error on the bias
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
Delta	\(\Delta\), the overdensity
kk	wave vector module
interpType	method to interpolate the power spectrum
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed
prec	accuracy of the integration
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum

Returns: error on β=f/b, where f is the linear growth rate and b is the bias

Warning: the input parameter \(\Delta\) is the background overdensity, not the critical overdensity \(\Delta_{crit}\); divide \(\Delta_{crit}\) by \(\Omega_M(z)\) (see cbl::cosmology::Cosmology::OmegaM) to obtain the background overdensity; the mass function by Manera et al. (2010) has been tested only for z=0 and z=0.5; the mass function by Despali et al. (2016) is currently implemented only for virial masses and at \(z<1.25\)

Definition at line 100 of file RSD.cpp.

◆ error_beta_measured()

double cbl::cosmology::Cosmology::error_beta_measured	(	const double	Volume,
		const double	density,
		const double	Mass_min,
		const double	Mass_max,
		const double	redshift,
		const std::string	model_bias,
		const std::string	model_MF,
		const std::string	method_SS,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const double	Delta = `200.`,
		const double	kk = `-1.`,
		const std::string	interpType = `"Linear"`,
		const int	norm = `-1`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`
	)

the error on the specific growth rate β from Bianchi et al. 2012

Parameters

Volume	comoving volume
density	comoving density
Mass_min	minimum halo mass
Mass_max	maximum halo mass
redshift	the redshift
model_bias	author(s) who proposed the bias; valid authors are: ST99 (Sheth & Tormen 1999), SMT01 (Sheth, Mo & Tormen 2001), SMT01_WL04 (Sheth, Mo & Tormen 2001 with the correction of Warren 2004), Tinker (Tinker et al. 2010)
model_MF	author(s) who proposed the mass function; valid authors are: PS (Press & Schechter), ST (Sheth & Tormen), Jenkins (Jenkins et al. 2001), Warren (Warren et al. 2006), ShenH (halo MF, Shen et al. 2006), ShenF (filament MF, Shen et al. 2006), ShenS (sheet MF, Shen et al. 2006), Pan (Pan 2007), Peacock (Peacock at al. 2007), Reed (Reed et al. 2007), Tinker (Tinker et al. 2008), Crocce (Crocce et al. 2010), Manera (Manera et al. 2010), Courtin (Courtin et al. 2010), Bhattacharya (Bhattacharya et al. 2011), Angulo_FOF (FoF MF, Angulo et al. 2012), Angulo_Sub (SUBFIND MF, Angulo et al. 2012), Watson_FOF (FoF MF, Watson et al. 2012), Watson_SOH (Spherical Overdensity halo MF, Watson et al. 2012), Despali_Z0, Despali_AllZ, Despali_AllZAllCosmo, Despali_HighM (Despali et al. 2016)
method_SS	method used to compute the power spectrum and σ(mass); valid method_SS are: CAMB [http://camb.info/], CLASS [http://class-code.net/], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
Delta	\(\Delta\), the overdensity
kk	wave vector module
interpType	method to interpolate the power spectrum
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed
prec	accuracy of the integration
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum

Returns: error on β=f/b, where f is the linear growth rate and b is the bias

Warning: the input parameter \(\Delta\) is the background overdensity, not the critical overdensity \(\Delta_{crit}\); divide \(\Delta_{crit}\) by \(\Omega_M(z)\) (see cbl::cosmology::Cosmology::OmegaM) to obtain the background overdensity; the mass function by Manera et al. (2010) has been tested only for z=0 and z=0.5; the mass function by Despali et al. (2016) is currently implemented only for virial masses and at \(z<1.25\)

Definition at line 109 of file RSD.cpp.

◆ F2()

double cbl::cosmology::Cosmology::F2	(	const double	k,
		const double	q,
		const double	kq
	)

function used to estimate the non-linear power spectrum

this function computes the following equation, which is used to estimate the non-linear power spectrum estimate the non-linear power spectrum following the MPTbreeze scheme (Crocce et al. 2012, https://arxiv.org/pdf/1207.1465.pdf):

\[ F_2 = \frac{5}{7} + \frac{kq}{2}\left(\frac{k}{q} + \frac{q}{k}\right) + \frac{2}{7}(kq)^2 \]

Parameters

k	the wavevector module
q
kq

Returns: \(F_2\)

Definition at line 77 of file PkXiNonLinear.cpp.

◆ F_AP()

double cbl::cosmology::Cosmology::F_AP ( const double redshift ) const

F_AP, the ALCOCK-PACZYNSKI distortion parameter.

Parameters

redshift the redshift

Returns: return F_AP

Definition at line 893 of file Cosmology.cpp.

◆ f_DE()

double cbl::cosmology::Cosmology::f_DE ( const double redshift = 0. ) const

auxiliary function used to compute the Hubble function

this function returns f_DE(z), a parameter that multiplies Ω_DE in the Hubble function (see e.g. Bassett & Hlozek 2010)

Parameters

redshift the redshift

Returns: f_DE

Definition at line 544 of file Cosmology.cpp.

◆ f_k()

double cbl::cosmology::Cosmology::f_k	(	const double	k,
		const std::shared_ptr< cbl::glob::FuncGrid >	PkLin,
		const double	qmin,
		const double	qmax,
		const double	prec = `1.e-3`
	)

function used to estimate the non-linear power spectrum

this function computes the following integral, which is used to estimate the non-linear power spectrum estimate the non-linear power spectrum following the MPTbreeze scheme (Crocce et al. 2012, https://arxiv.org/pdf/1207.1465.pdf):

\[ f(k) = \int_{q_{min}}^{q_{max}} \mathrm{d}q\, q^2P(k)\frac{1}{504k^3q^5}\left[ 6k^7q-79k^5q^3+50k^3q^5-21kq^7+\frac{3}{4}\left(k^2-q^2\right)^3 \left(2k^2+7q^2\right)\ln\left(\frac{(k-q)^2}{(k+q)^2}\right) \right] \]

Parameters

k	the wavevector module
PkLin	linear power spectrum
qmin
qmax
prec	the integral precision

Returns: \(f(k)\)

Definition at line 47 of file PkXiNonLinear.cpp.

◆ f_nu()

double cbl::cosmology::Cosmology::f_nu	(	const double	SS,
		const double	del_v,
		const double	del_c
	)		const

\(f_{\ln \sigma}(\sigma)\) (approximation)

Author: Tommaso Ronconi; tomma.nosp@m.so.r.nosp@m.oncon.nosp@m.i@st.nosp@m.udio..nosp@m.unib.nosp@m.o.it

Parameters

SS	variance of the linear density field ( \(\sigma^2(R)\))
del_v	linear density contrast defining a void
del_c	critical value of the linear density field

Returns: the fraction of trajectories that evolve into voids, as given in equation (8) of Jennings et al. (2013)

Definition at line 74 of file SizeFunction.cpp.

◆ fNL()

double cbl::cosmology::Cosmology::fNL ( ) const

inline

get the private member Cosmology::m_fNL

Returns: f_NL: the non-Gaussian amplitude

Definition at line 1265 of file Cosmology.h.

◆ frk()

double cbl::cosmology::Cosmology::frk	(	const double	kk,
		const double	mass,
		const std::string	method_Pk,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const std::string	interpType = `"Linear"`,
		const int	norm = `-1`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`
	)

auxiliary function to estimate cosmological quantities in non-Gaussian cosmologies

Author: Cosimo Fedeli; cosim.nosp@m.o.fe.nosp@m.deli@.nosp@m.oabo.nosp@m..inaf.nosp@m..it

Parameters

kk	wave vector module
mass	halo mass
method_Pk	method used to compute the power spectrum (i.e. the Boltzmann solver); valid choices for method_Pk are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	the output_root parameter of the parameter file used to compute the power spectrum; it can be any name. If this parameter is different from the default value it will be used also in the output directory name
interpType	method to interpolate the power spectrum
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
prec	accuracy of the integration
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum

Returns: frk

Definition at line 266 of file NG.cpp.

◆ fsigma8()

double cbl::cosmology::Cosmology::fsigma8	(	const double	redshift,
		const std::string	method_Pk,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const bool	NL = `false`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`,
		const std::string	file_par = `par::defaultString`
	)		const

f*σ₈: the linear growth rate times the dark matter rms mass fluctuation within 8 Mpc/h

Parameters

redshift	the redshift
method_Pk	method used to compute the power spectrum and σ(mass) (i.e. the Boltzmann solver); valid choices for method_Pk are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
NL	false \(\rightarrow\) linear power spectrum; false \(\rightarrow\) non-linear power spectrum
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
prec	accuracy of the integration
file_par	name of the parameter file; if a parameter file is provided (i.e. file_par!=NULL), it will be used, ignoring the cosmological parameters of the object

Returns: f*σ₈

Definition at line 46 of file RSD.cpp.

◆ G2()

double cbl::cosmology::Cosmology::G2	(	const double	k,
		const double	q,
		const double	kq
	)

function used to estimate the non-linear power spectrum

this function computes the following equation, which is used to estimate the non-linear power spectrum estimate the non-linear power spectrum following the MPTbreeze scheme (Crocce et al. 2012, https://arxiv.org/pdf/1207.1465.pdf):

\[ G_2 = \frac{3}{7} + \frac{kq}{2}\left(\frac{k}{q} + \frac{q}{k}\right) + \frac{4}{7}(kq)^2 \]

Parameters

k	the wavevector module
q
kq

Returns: \( G_2 \)

Definition at line 86 of file PkXiNonLinear.cpp.

◆ g_k()

double cbl::cosmology::Cosmology::g_k	(	const double	k,
		const std::shared_ptr< cbl::glob::FuncGrid >	PkLin,
		const double	qmin,
		const double	qmax,
		const double	prec = `1.e-3`
	)

function used to estimate the non-linear power spectrum

this function computes the following integral, which is used to estimate the non-linear power spectrum estimate the non-linear power spectrum following the MPTbreeze scheme (Crocce et al. 2012, https://arxiv.org/pdf/1207.1465.pdf):

\[ f(k) = \int_{q_{min}}^{q_{max}} \mathrm{d}q\, q^2P(k)\frac{1}{168k^3q^5}\left[ 6k^7q-41k^5q^3+2k^3q^5-3kq^7+\frac{3}{4}\left(k^2-q^2\right)^3 \left(2k^2+q^2\right)\ln\left(\frac{(k-q)^2}{(k+q)^2}\right) \right] \]

Parameters

k	the wavevector module
PkLin	linear power spectrum
qmin
qmax
prec	the integral precision

Returns: \(g(k)\)

Definition at line 62 of file PkXiNonLinear.cpp.

◆ Gamma_3PCF()

double cbl::cosmology::Cosmology::Gamma_3PCF	(	const double	r1,
		const double	r2,
		const double	theta,
		const std::vector< double >	xi,
		const std::vector< double >	dPhi
	)		const

function to compute non-local contribution to three-point correlation function; specifically, it implements Eq. 20 of Bel el et al. 2015, MNRAS, 453, 259:

\[ \Gamma_{123} = \left[ \xi(r_1)+3\frac{\Phi^\prime(r_1)}{r1}\right] \left[ \xi(r_2)+3\frac{\Phi^\prime(r_2)}{r_2}\right]P_2(\cos\theta) \]

where the prime indicates the derivative with respect to \(r\), \(P_2\) is the second Legandre polynomial computed by cbl::legendre_polynomial, and \(\xi(r), \Phi(r)\) are the integrals of the power spectrum computed by cbl::cosmology::Cosmology::integrals_Q_nonLocal

Parameters

r1	the first side of the triangle
r2	the second side of the triangle
theta	the angle betwee r1 and r2
xi	vector containing the value of xi at r1, r2
dPhi	vector containing the value of the derivative of Phi at r1, r2

Returns: the value of the \(\Gamma_{123}\)

Definition at line 90 of file 3PCF.cpp.

◆ generate_bias_eff_grid_one_cosmopar() [1/2]

void cbl::cosmology::Cosmology::generate_bias_eff_grid_one_cosmopar	(	std::vector< double > &	parameter,
		std::vector< double > &	bias_eff,
		const std::string	dir_output,
		const std::string	file_bias_eff_grid,
		const cbl::cosmology::CosmologicalParameter	cosmoPar,
		const double	min_par,
		const double	max_par,
		const int	nbin_par,
		const double	redshift,
		const double	Mass_min,
		const double	Mass_max,
		const std::string	model_bias,
		const std::string	model_MF,
		const std::string	method_SS,
		const std::string	selection_function_file,
		const std::vector< int >	column = `{}`,
		const double	alpha = `1.`,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const double	Delta_crit = `200.`,
		const double	kk = `-1.`,
		const std::string	interpType = `"Linear"`,
		const int	norm = `-1`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`
	)

effective bias of dark matter haloes, computed by weighting on the selection function on a grid of one input cosmological parameter; this function is used when modelling the two-point correlation function

this function computes the effective bias of dark matter haloes:

\[ b_{eff}(z) = \frac{\int_{M_{min}}^{M_{max}} {\rm d}M\, b(M, z) \Phi(M, z) f(M, z)}{\int_{M_{min}}^{M_{max}} {\rm d}M\,\Phi(M, z) f(M, z)} \]

where the linear bias of the \(i\)-th halo, \(b^{i}(M, z)\), is computed by cbl::cosmology::Cosmology::bias_halo; the mass variance is computed by cbl::cosmology::Cosmology::sigma2M

Parameters

parameter	vector containing the grid of the cosmological parameters on which the effective bias grid is computed
bias_eff	vector containing the effective bias grid
dir_output	the directory where the effective bias grid is stored
file_bias_eff_grid	the file there the effective bias grid is stored
cosmoPar	the cosmological parameter for which the effective bias grid is computed
min_par	the minimum value for the parameter where the effective bias is computed
max_par	the maximum value for the parameter where the effective bias is computed
nbin_par	the number of points for the parameter where the effective bias is computed
redshift	vector containing the redshifts; if it has size=1, it will be considered as the main redshift
Mass_min	minimum cluster mass
Mass_max	maximum cluster mass
model_bias	author(s) who proposed the bias; valid authors are: ST99 (Sheth & Tormen 1999), SMT01 (Sheth, Mo & Tormen 2001), SMT01_WL04 (Sheth, Mo & Tormen 2001 with the correction of Warren 2004), Tinker (Tinker et al. 2010)
model_MF	author(s) who proposed the mass function; valid authors are: PS (Press & Schechter), ST (Sheth & Tormen), Jenkins (Jenkins et al. 2001), Warren (Warren et al. 2006), ShenH (halo MF, Shen et al. 2006), ShenF (filament MF, Shen et al. 2006), ShenS (sheet MF, Shen et al. 2006), Pan (Pan 2007), Peacock (Peacock at al. 2007), Reed (Reed et al. 2007), Tinker (Tinker et al. 2008), Crocce (Crocce et al. 2010), Manera (Manera et al. 2010), Courtin (Courtin et al. 2010), Bhattacharya (Bhattacharya et al. 2011), Angulo_FOF (FoF MF, Angulo et al. 2012), Angulo_Sub (SUBFIND MF, Angulo et al. 2012), Watson_FOF (FoF MF, Watson et al. 2012), Watson_SOH (Spherical Overdensity halo MF, Watson et al. 2012), Despali_Z0, Despali_AllZ, Despali_AllZAllCosmo, Despali_HighM (Despali et al. 2016)
method_SS	method used to compute the power spectrum and σ(mass); valid method_SS are: CAMB [http://camb.info/], CLASS [http://class-code.net/], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
alpha	the \(\alpha\) parameter of the cluster mass scaling relation
selection_function_file	the input selection function file
column	vector containing the columns with {mass, redshift, selection function}
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
Delta_crit	\(\Delta_{crit}\): the critical overdensity
kk	wave vector module
interpType	method to interpolate the power spectrum
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed
prec	accuracy of the integration
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum

Definition at line 586 of file Bias.cpp.

◆ generate_bias_eff_grid_one_cosmopar() [2/2]

void cbl::cosmology::Cosmology::generate_bias_eff_grid_one_cosmopar	(	std::vector< double > &	parameter,
		std::vector< double > &	bias_eff,
		const std::string	dir_output,
		const std::string	file_bias_eff_grid,
		const cbl::cosmology::CosmologicalParameter	cosmoPar,
		const double	min_par,
		const double	max_par,
		const int	nbin_par,
		const std::vector< double >	mass,
		const std::vector< double >	mass_grid,
		const std::vector< double >	redshift,
		const std::string	model_bias,
		const std::string	method_SS,
		const std::string	meanType = `"mean_bias"`,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const double	Delta_crit = `200.`,
		const double	kk = `-1.`,
		const std::string	interpType = `"Linear"`,
		const int	norm = `-1`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`,
		const cbl::cosmology::Cosmology	cosmology_mass = `{}`,
		const std::vector< double >	redshift_source = `{}`
	)

compute the effective bias of dark matter haloes, by averaging the bias of a set of haloes, interpolating the mass variance on a grid of masses and of one input cosmological parameter; this function is used when modelling the two-point correlation function

this function computes the effective bias of dark matter haloes by either averaging the bias of a set of haloes with a given mass:

\[b_{eff}(z) = \frac{1}{N_{halo}}\sum_{i=1}^{N_{halo}} b(M_i, z_i) \; , \; (1)\]

or by averaging over halo pairs:

\[b_{eff}(z) = \sqrt{ \frac{2}{N_{halo}(N_{halo}-1)} \sum_{i=1}^{N_{halo}}\sum_{j=i+1}^{N_{halo}} b(M_i, z_i)b(M_j, z_j)} \; , \; (2)\]

where the linear bias of the \(i\)-th halo, \(b^{i}(M, z)\), is computed by cbl::cosmology::Cosmology::bias_halo; the mass variance is computed by cbl::cosmology::Cosmology::sigma2M

Parameters

parameter	vector containing the grid of the cosmological parameters on which the effective bias grid is computed
bias_eff	vector containing the effective bias grid
dir_output	the directory where the effective bias grid is stored
file_bias_eff_grid	the file there the effective bias grid is stored
cosmoPar	the cosmological parameter for which the effective bias grid is computed
min_par	the minimum value for the parameter where the effective bias is computed
max_par	the maximum value for the parameter where the effective bias is computed
nbin_par	the number of points for the parameter where the effective bias is computed
mass	vector containing the halo masses
mass_grid	vector containing the halo masses on the grid used to interpolate the mass variance
redshift	vector containing the redshifts; if it has size=1, it will be considered as the main redshift
model_bias	author(s) who proposed the bias; valid authors are: ST99 (Sheth & Tormen 1999), SMT01 (Sheth, Mo & Tormen 2001), SMT01_WL04 (Sheth, Mo & Tormen 2001 with the correction of Warren 2004), Tinker (Tinker et al. 2010)
method_SS	method used to compute the power spectrum and σ(mass); valid method_SS are: CAMB [http://camb.info/], CLASS [http://class-code.net/], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
meanType	meanType="mean_bias" \(\rightarrow\) the effective bias is computed with Eq.(1); meanType="mean_pair_bias" \(\rightarrow\) the effective bias is computed with Eq.(2)
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
Delta_crit	\(\Delta_{crit}\): the critical overdensity
kk	wave vector module
interpType	method to interpolate the power spectrum
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed
prec	accuracy of the integration
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum
cosmology_mass	cosmology used to measure the cluster masses
redshift_source	vector containing the redshifts of the source galaxies, in case the cluster masses are estimated from weak lensing

Definition at line 529 of file Bias.cpp.

◆ generate_bias_eff_grid_two_cosmopars()

void cbl::cosmology::Cosmology::generate_bias_eff_grid_two_cosmopars	(	std::vector< double > &	parameter1,
		std::vector< double > &	parameter2,
		std::vector< std::vector< double >> &	bias_eff,
		const std::string	dir_output,
		const std::string	file_bias_eff_grid,
		const cbl::cosmology::CosmologicalParameter	cosmoPar1,
		const double	min_par1,
		const double	max_par1,
		const int	nbin_par1,
		const cbl::cosmology::CosmologicalParameter	cosmoPar2,
		const double	min_par2,
		const double	max_par2,
		const int	nbin_par2,
		const std::vector< double >	mass,
		const std::vector< double >	mass_grid,
		const std::vector< double >	redshift,
		const std::string	model_bias,
		const std::string	method_SS,
		const std::string	meanType = `"mean_bias"`,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const double	Delta = `200.`,
		const double	kk = `-1.`,
		const std::string	interpType = `"Linear"`,
		const int	norm = `-1`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`,
		const cbl::cosmology::Cosmology	cosmology_mass = `{}`,
		const std::vector< double >	redshift_source = `{}`
	)

effective bias of dark matter haloes, computed by averaging the bias of a set of haloes, interpolating the mass variance on a grid of masses and two input cosmological parameters; this function is used when modelling the two-point correlation function

this function computes the effective bias of dark matter haloes by either averaging the bias of a set of haloes with a given mass:

\[b_{eff}(z) = \frac{1}{N_{halo}}\sum_{i=1}^{N_{halo}} b(M_i, z_i) \; , \; (1)\]

or by averaging over halo pairs:

\[b_{eff}(z) = \sqrt{ \frac{2}{N_{halo}(N_{halo}-1)} \sum_{i=1}^{N_{halo}}\sum_{j=i+1}^{N_{halo}} b(M_i, z_i)b(M_j, z_j)} \; , \; (2)\]

where the linear bias of the \(i\)-th halo, \(b^{i}(M, z)\), is computed by cbl::cosmology::Cosmology::bias_halo; the mass variance is computed by cbl::cosmology::Cosmology::sigma2M

Parameters

parameter1	vector containing the grid of the first cosmological parameters on which the effective bias grid is computed
parameter2	vector containing the grid of the second cosmological parameters on which the effective bias grid is computed
bias_eff	vector containing the effective bias grid
dir_output	the directory where the effective bias grid is stored
file_bias_eff_grid	the file there the effective bias grid is stored
cosmoPar1	the first cosmological parameter for which the effective bias grid is computed
min_par1	the minimum value for the first parameter where the effective bias is computed
max_par1	the maximum value for the first parameter where the effective bias is computed
nbin_par1	the number of points for the first parameter where the effective bias is computed
cosmoPar2	the second cosmological parameter for which the effective bias grid is computed
min_par2	the minimum value for the second parameter where the effective bias is computed
max_par2	the maximum value for the second parameter where the effective bias is computed
nbin_par2	the number of points for the second parameter where the effective bias is computed
mass	vector containing the halo masses
mass_grid	vector containing the halo masses on the grid used to interpolate the mass variance
redshift	vector containing the redshifts; if it has size=1, it will be considered as the main redshift
model_bias	author(s) who proposed the bias; valid authors are: ST99 (Sheth & Tormen 1999), SMT01 (Sheth, Mo & Tormen 2001), SMT01_WL04 (Sheth, Mo & Tormen 2001 with the correction of Warren 2004), Tinker (Tinker et al. 2010)
method_SS	method used to compute the power spectrum and σ(mass); valid method_SS are: CAMB [http://camb.info/], CLASS [http://class-code.net/], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
meanType	meanType="mean_bias" \(\rightarrow\) the effective bias is computed with Eq.(1); meanType="mean_pair_bias" \(\rightarrow\) the effective bias is computed with Eq.(2)
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
Delta	\(\Delta\), the overdensity
kk	wave vector module
interpType	method to interpolate the power spectrum
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed
prec	accuracy of the integration
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum
cosmology_mass	cosmology used to measure the cluster masses
redshift_source	vector containing the redshifts of the source galaxies, in case the cluster masses are estimated from weak lensing

Definition at line 636 of file Bias.cpp.

◆ get_barred_xi()

void cbl::cosmology::Cosmology::get_barred_xi	(	std::vector< double >	rr,
		std::vector< double >	Xi,
		std::vector< double > &	Xi_,
		std::vector< double > &	Xi__,
		const std::string	method_Pk,
		const double	redshift,
		const bool	xiType = `0`,
		const double	k_star = `-1.`,
		const bool	xiNL = `0`,
		const int	norm = `-1`,
		const double	r_min = `0.1`,
		const double	r_max = `150.`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	aa = `0.`,
		const double	prec = `1.e-2`,
		const std::string	file_par = `par::defaultString`
	)		const

get the barred dark matter correlation functions

this function provides the dark matter barred correlation functions, used to model the two-point correlation function in redshift-space

Parameters

[in]	rr	vector of r, the module of the comoving separation
[in]	Xi	vector of ξ(r), the two-point correlation function of dark matter
[out]	Xi_	vector of barred ξ(r),
[out]	Xi__	vector of double-barred ξ(r)
[in]	method_Pk	method used to compute the power spectrum (i.e. the Boltzmann solver); valid choices for method_Pk are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
[in]	redshift	redshift
[in]	xiType	0 \(\rightarrow\) standard; 1 \(\rightarrow\) Chuang & Wang model
[in]	k_star	k_* of the Chuang & Wang model
[in]	xiNL	0 \(\rightarrow\) linear power spectrum; 1 \(\rightarrow\) non-linear power spectrum
[in]	norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
[in]	r_min	minimum separation up to which the correlation function is computed
[in]	r_max	maximum separation up to which the correlation function is computed
[in]	k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
[in]	k_max	maximum wave vector module up to which the power spectrum is computed
[in]	aa	parameter a of Eq. 24 of Anderson et al. 2012
[in]	prec	accuracy of the integration
[in]	file_par	name of the parameter file; if a parameter file is provided (i.e. file_par!=NULL), it will be used, ignoring the cosmological parameters of the object

Definition at line 1981 of file PkXi.cpp.

◆ get_xi()

void cbl::cosmology::Cosmology::get_xi	(	std::vector< double > &	rr,
		std::vector< double > &	Xi,
		const std::string	method_Pk,
		const double	redshift,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const bool	xiType = `0`,
		const double	k_star = `-1.`,
		const bool	xiNL = `0`,
		const int	norm = `-1`,
		const double	r_min = `0.1`,
		const double	r_max = `150.`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	aa = `0.`,
		const bool	GSL = `false`,
		const double	prec = `1.e-2`,
		const std::string	file_par = `par::defaultString`
	)

get the dark matter two-point correlation function

this function provides the dark matter correlation function, obtained by Fourier transforming the matter power spectrum

Parameters

[out]	rr	vector of r, the module of the comoving separation
[out]	Xi	vector of ξ(r), the two-point correlation function of dark matter
[in]	method_Pk	method used to compute the power spectrum (i.e. the Boltzmann solver); valid choices for method_Pk are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
[in]	redshift	redshift
[in]	store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
[in]	output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
[in]	xiType	0 \(\rightarrow\) standard; 1 \(\rightarrow\) Chuang & Wang model
[in]	k_star	k_* of the Chuang & Wang model
[in]	xiNL	0 \(\rightarrow\) linear power spectrum; 1 \(\rightarrow\) non-linear power spectrum
[in]	norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
[in]	r_min	minimum separation up to which the correlation function is computed
[in]	r_max	maximum separation up to which the correlation function is computed
[in]	k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
[in]	k_max	maximum wave vector module up to which the power spectrum is computed
[in]	aa	parameter a of Eq. 24 of Anderson et al. 2012
[in]	GSL	false \(\rightarrow\) FFTlog is used; true \(\rightarrow\) the GSL libraries are used
[in]	prec	accuracy of the integration
[in]	file_par	name of the parameter file; if a parameter file is provided (i.e. file_par!=NULL), it will be used, const ignoring the cosmological parameters of the object

Definition at line 1909 of file PkXi.cpp.

◆ gg()

double cbl::cosmology::Cosmology::gg ( const double redshift = 0. ) const

the linear growth factor at a given redshift, \(g(z)\)

this function computes the following quantity (e.g. Eq.(1) by Hamilton 2001):

\[ g(z) \equiv \tilde{D}(z)(1+z) \]

where \(a=1/(1+z)\) and \(D(z)\) is computed by cbl::cosmology::Cosmology::DD

Parameters

redshift the redshift

Returns: the linear growth factor

Definition at line 720 of file Cosmology.cpp.

◆ H0()

double cbl::cosmology::Cosmology::H0 ( ) const

inline

get the private member Cosmology::m_H0

Returns: H₀: the Hubble constant [km/sec/Mpc]

Definition at line 1184 of file Cosmology.h.

◆ Hdot()

double cbl::cosmology::Cosmology::Hdot ( const double redshift = 0. ) const

derivative of the Hubble function at a given redshift

Parameters

redshift the redshift

Returns: dH/dz

Definition at line 985 of file Cosmology.cpp.

◆ hh()

double cbl::cosmology::Cosmology::hh ( ) const

inline

get the private member Cosmology::m_hh

Returns: h: the Hubble parameter, H₀/100

Definition at line 1191 of file Cosmology.h.

◆ HH()

double cbl::cosmology::Cosmology::HH ( const double redshift = 0. ) const

the Hubble function

Parameters

redshift the redshift

Returns: H(z)

Definition at line 570 of file Cosmology.cpp.

◆ I_ELL_ell()

void cbl::cosmology::Cosmology::I_ELL_ell	(	std::vector< std::vector< double >> &	II,
		const std::vector< double >	rr,
		const int	ll,
		const int	LL,
		const std::vector< double >	kk,
		const std::vector< double >	Pk
	)

compute the quantity \( I_{\mathcal{L} l} (r_1, r_2)\)

This function computes the quantity \( I_{\mathcal{L} l} (r_1, r_2)\):

\[ I_{\mathcal{L} l} (r_1, r_2) = \sum_{l_1} (-1)^{l_1+l}(2l_1+1)(2l+1) \begin{pmatrix} l_1 & l & \mathcal{L} \\ 0 & 0 & 0 \end{pmatrix}^2 \\ \times \int \mathrm{d} r \;r\;f_{l, l_1}(r_1;r) f_{l, l_1} (r_2; r) \]

where \( f_{l, l_1} (r_i;r) \) is computed by cbl::cosmology::Cosmology::eff_l_l1 This quantity is used the compute the tree-level theoretical prediction for the biased and redshift space the three-point correlation function, following Slepian&Eisenstein, 2017

Parameters

II	the quantity \( I_{\mathcal{L} l} (r_1, r_2) \)
rr	vector of scales
ll	the order \(l\)
LL	the order \( \mathcal{L} \)
kk	vector of wavevector modules
Pk	dark matter power spectrum

Definition at line 842 of file 3PCF.cpp.

◆ integrals_Q_nonLocal()

void cbl::cosmology::Cosmology::integrals_Q_nonLocal	(	std::vector< double > &	xi_matter,
		std::vector< double > &	Phi,
		const std::vector< double >	rr,
		const std::vector< double >	kk,
		const std::vector< double >	Pk_matter,
		const double	prec
	)		const

integral functions for the three-point correlation model

this function computes and store functons used to model the three-point correlation model; specifically, it implements Eq. 21, in polar coordinates, of Bel et al. 2015, MNRAS, 453, 259):

\[ \xi_{DM}(r) = \frac{1}{2\pi^2}\int_0^\infty \mathrm{d} k\, k^2 P_{DM}(k) j_0(k r), \\\ \Phi(r) = \frac{1}{2\pi^2}\int_0^\infty \mathrm{d} k\, P_{DM}(k) W^2(kr) j_0(k r), \\ \]

where \(j_0(k r)=\sin(k r)/(kr)\) is the l=0 spherical Bessel function, and \(W(kr)\) is the top-hat window function computed by cbl::TopHat_WF

Parameters

[out]	xi_matter	vector containing the dark matter two-point correlation function values
[out]	Phi	vector containing the \( \Phi(r)\) values, estimated at the scales given in rr
[in]	rr	vector or scales at which the dark matter two-point correlation function (xi_matter) will be computed
[in]	kk	vector of the wave vector modules at which the power spectrum is computed
[in]	Pk_matter	vector of containing the dark matter power spectrum values, estimated at the wave vector modules given in kk
	prec	the integral precision

Definition at line 63 of file 3PCF.cpp.

◆ integrals_zeta_BarrigaGatzanaga()

void cbl::cosmology::Cosmology::integrals_zeta_BarrigaGatzanaga	(	std::vector< double > &	xi_matter,
		std::vector< double > &	Phi,
		const std::vector< double >	rr,
		const std::vector< double >	kk,
		const std::vector< double >	Pk_matter
	)		const

integrals used to compute the Barriga & Gatzanaga al. 2002 three-point correlation function model

this function computes the integrals used to model the three-point correlation as described in Barriga & Gatzanaga 2002:

\[ \xi_{DM}(r) = \frac{1}{2\pi^2}\int_0^\infty \mathrm{d} k\, k^2 P_{DM}(k) j_0(k r), \]

\[ \Phi(r) = \frac{1}{2\pi^2}\int_0^\infty \mathrm{d} k\, P_{DM}(k) j_0(k r). \]

Parameters

[out]	xi_matter	vector containing the dark matter two-point correlation function
[out]	Phi	vector containing \( \Phi(r)\)
[in]	rr	vector or scales
[in]	kk	vector of the wave vector modules
[in]	Pk_matter	the dark matter power spectrum

Definition at line 346 of file 3PCF.cpp.

◆ integrals_zeta_Slepian()

void cbl::cosmology::Cosmology::integrals_zeta_Slepian	(	std::vector< double > &	xi_matter,
		std::vector< double > &	xi_matter_m1,
		std::vector< double > &	xi_matter_p1,
		std::vector< double > &	xi_matter_2,
		const std::vector< double >	rr,
		const std::vector< double >	kk,
		const std::vector< double >	Pk_matter
	)		const

integrals used to compute the Slepian et al. 2015 three-point correlation function model

this function computes the integrals used to model the three-point correlation as described in Slepian et. al 2015:

\[ \xi_{DM}(r) = \frac{1}{2\pi^2}\int_0^\infty \mathrm{d} k k^2 P_{DM}(k) j_0(k r), \\\ \xi^{[1\pm]}_{DM}(r) = \frac{1}{2\pi^2}\int_0^\infty \mathrm{d} k k^2 P_{DM}(k) k^{\pm 1} j_1(k r), \\ \xi^{[2]}_{DM}(r) = \frac{1}{2\pi^2}\int_0^\infty \mathrm{d} k k^2 P_{DM}(k) j_2(k r) . \]

Parameters

[out]	xi_matter	vector containing the dark matter two-point correlation function
[out]	xi_matter_m1	vector containing \(\xi^{[1-]}_{DM}(r)\)
[out]	xi_matter_p1	vector containing \(\xi^{[1+]}_{DM}(r)\)
[out]	xi_matter_2	vector containing \(\xi^{[2]}_{DM}(r)\)
[in]	rr	vector or scales
[in]	kk	vector of the wave vector modules
[in]	Pk_matter	the dark matter power spectrum

Definition at line 161 of file 3PCF.cpp.

◆ k_ell()

void cbl::cosmology::Cosmology::k_ell	(	std::vector< std::vector< double >> &	KK,
		const std::vector< double >	rr,
		const int	ll,
		const std::vector< double >	kk,
		const std::vector< double >	Pk
	)

compute the quantity \( k_l (r_1, r_2) \)

This function computes the quantity \( k_l (r_1, r_2) \):

\[ k_l (r_1, r_2) = \frac{64}{77175} \left[9I_{1,l}(r_1, r_2)- 14I_{3,l}(r_1, r_2) +5I_{5,l}(r_1, r_2) \right] \]

where \( I_{\mathcal{L}l} \) is computed by cbl::cosmology::Cosmology::I_ELL_ell This quantity is used the compute the tree-level theoretical prediction for the biased and redshift space three-point correlation function, following Slepian&Eisenstein, 2017

Parameters

KK	the quantity \( k_l (r_1, r_2) \)
rr	vector of scales
ll	the order \(l\)
kk	vector of wavevector modules
Pk	dark matter power spectrum

Definition at line 881 of file 3PCF.cpp.

◆ k_star()

double cbl::cosmology::Cosmology::k_star	(	const std::string	method_Pk,
		const double	redshift,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const double	k_max = `100.`,
		const std::string	file_par = `par::defaultString`
	)		const

the k_* parameter

this function provides the k_* parameter used to model the BAO (see e.g. Chuang & Wang 2012, Crocce et al. 2006, Matsubara 2008)

Parameters

method_Pk	method used to compute the power spectrum (i.e. the Boltzmann solver); valid choices for method_Pk are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
redshift	the redshift
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
k_max	maximum wave vector module up to which the power spectrum is computed
file_par	name of the parameter file; if a parameter file is provided (i.e. file_par!=NULL), it will be used, ignoring the cosmological parameters of the object

Returns: k_*

Definition at line 1886 of file PkXi.cpp.

◆ linear_growth_rate()

double cbl::cosmology::Cosmology::linear_growth_rate	(	const double	redshift,
		const double	prec = `1.e-4`
	)		const

the linear growth rate at a given redshift, \(f(z)\)

this function computes the following function:

\[ f(z) = \frac{{\rm d}\,\ln D}{{\rm d}\,\ln a} \]

Parameters

redshift	the redshift
prec	precision used for the resolution of the differential equation in the case w_a different than 0

Returns: the linear growth rate

Warning: for w_a different than 0 the current implementation does not take into account the precence of massive neutrinos

Definition at line 662 of file Cosmology.cpp.

◆ linear_point()

vector< double > cbl::cosmology::Cosmology::linear_point	(	const double	redshift,
		const double	rmin = `60.`,
		const double	rmax = `150.`,
		const int	nbinr = `100`,
		const std::string	interpType = `"Spline"`
	)

the linear point

see Anselmi et al. 2016

Author: Alfonso Veropalumbo; alfon.nosp@m.so.v.nosp@m.eropa.nosp@m.lumb.nosp@m.o@uni.nosp@m.bo.i.nosp@m.t

Parameters

redshift	the redshift
rmin	the minimum scale
rmax	the maximum scale
nbinr	the number of scale bins
interpType	the interpolation type

Returns: vector containing the linear point, the dip and the BAO peak for the correlation function at the redshift provided

Definition at line 263 of file BAO.cpp.

◆ lookback_time()

double cbl::cosmology::Cosmology::lookback_time ( const double redshift = 0. ) const

lookback time at a given redshift

Parameters

redshift the redshift

Returns: t_lookback [Gyr]

Definition at line 932 of file Cosmology.cpp.

◆ Lum_bol()

double cbl::cosmology::Cosmology::Lum_bol	(	const double	redshift = `0.`,
		const double	flux = `1.`
	)		const

bolometric luminosity

Parameters

redshift	the redshift
flux	flux

Returns: L_bol

Definition at line 1036 of file Cosmology.cpp.

◆ m_acn_dz()

double cbl::cosmology::Cosmology::m_acn_dz ( const double cc ) const

private

the inverse cosine amplitude of the Jacobian elliptic function

this method computes the inverse cosine amplitude of the Jacobian elliptic function cn^-1(c|m), with shape parameter fixed to m=(2+3^0.5)/4; namely cn^-1(s|m) = F(arccos(c)|m); it is used to compute the relation between comoving distance and redshift (see Numer. Math. (2010) 116:687–719, T. Fukushima "Fast computation of incomplete elliptic integral of first kind by half argument transformation")

Author: Mauro Roncarelli; mauro.nosp@m..ron.nosp@m.carel.nosp@m.li@u.nosp@m.nibo..nosp@m.it

Parameters

cc	scalar, argument

Returns: cn^-1(c|m)

Warning: this method works only for a fixed value of the shape parameter m=(2+3^0.5)/4; the argument c must be in the range 0<c<1

Definition at line 1409 of file Cosmology.cpp.

◆ m_asn_dz()

double cbl::cosmology::Cosmology::m_asn_dz ( const double ss ) const

private

the inverse sine amplitude of the Jacobian elliptic function

this method computes the inverse sine amplitude of the Jacobian elliptic function sn^-1(s|m), with shape parameter fixed to m=(2+3^0.5)/4, namely sn^-1(s|m) = F(arcsin(s)|m); it is used to compute the relation between comoving distance and redshift (see Numer. Math. (2010) 116:687–719, T. Fukushima "Fast computation of incomplete elliptic integral of first kind by half argument transformation")

Author: Mauro Roncarelli; mauro.nosp@m..ron.nosp@m.carel.nosp@m.li@u.nosp@m.nibo..nosp@m.it

Parameters

ss	scalar, argument

Returns: sn^-1(s|m)

Warning: this method works only for a fixed value of the shape parameter m=(2+3^0.5)/4; the argument s must be in the range 0<s<1

Definition at line 1428 of file Cosmology.cpp.

◆ m_bias_halo_generator() [1/2]

double cbl::cosmology::Cosmology::m_bias_halo_generator	(	const double	Sigma,
		const double	redshift,
		const double	D_N,
		const std::string	author,
		const double	Delta = `200.`
	)		const

private

auxiliary function to compute the halo bias

Parameters

Sigma	σ(mass, z=0): the mass variance at z=0
redshift	the redshift
D_N	the amplitude of the growing mode
author	author(s) who proposed the bias; valid authors are: ST99 (Sheth & Tormen 1999), SMT01 (Sheth, Mo & Tormen 2001), SMT01_WL04 (Sheth, Mo & Tormen 2001 with the correction of Warren 2004), Tinker (Tinker et al. 2010)
Delta	\(\Delta\), the overdensity

Returns: the halo bias

Warning: the input parameter \(\Delta\) is the background overdensity, not the critical overdensity \(\Delta_{crit}\); divide \(\Delta_{crit}\) by \(\Omega_M(z)\) (see cbl::cosmology::Cosmology::OmegaM) to obtain the background overdensity

Definition at line 100 of file Bias.cpp.

◆ m_bias_halo_generator() [2/2]

double cbl::cosmology::Cosmology::m_bias_halo_generator	(	const double	Sigma,
		const double	redshift,
		const std::string	author,
		const double	Delta = `200.`
	)		const

private

auxiliary function to compute the halo bias

Parameters

Sigma	σ(mass, z=0): the mass variance at z=0
redshift	the redshift
author	author(s) who proposed the bias; valid authors are: ST99 (Sheth & Tormen 1999), SMT01 (Sheth, Mo & Tormen 2001), SMT01_WL04 (Sheth, Mo & Tormen 2001 with the correction of Warren 2004), Tinker (Tinker et al. 2010)
Delta	\(\Delta\), the overdensity

Returns: the halo bias

Warning: the input parameter \(\Delta\) is the background overdensity, not the critical overdensity \(\Delta_{crit}\); divide \(\Delta_{crit}\) by \(\Omega_M(z)\) (see cbl::cosmology::Cosmology::OmegaM) to obtain the background overdensity

Definition at line 89 of file Bias.cpp.

◆ m_elf_dz()

double cbl::cosmology::Cosmology::m_elf_dz ( const double phi ) const

private

the incomplete elliptic integral

this method computes the incomplete elliptic integral of the first kind F(φ|m), with shape parameter fixed to m=(2+3^0.5)/4; it is used to compute the relation between comoving distance and redshift (see Numer. Math. (2010) 116:687–719, T. Fukushima "Fast computation of incomplete elliptic integral of first kind by half argument transformation")

Author: Mauro Roncarelli; mauro.nosp@m..ron.nosp@m.carel.nosp@m.li@u.nosp@m.nibo..nosp@m.it

Parameters

phi	φ scalar, argument

Returns: F(φ|m)

Warning: this method works only for a fixed value of the shape parameter m=(2+3^0.5)/4

Definition at line 1375 of file Cosmology.cpp.

◆ m_func_sigma()

double cbl::cosmology::Cosmology::m_func_sigma	(	const std::string	method_Pk,
		const double	redshift,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const std::string	interpType = `"Linear"`,
		const double	k_max = `100.`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`,
		std::function< double(double)>	filter = `{}`,
		const bool	unit1 = `false`
	)		const

private

function to compute the not-yet-normalised mass variances and their derivatives

this function computes the not-yet-normalised mass variances and their derivatives:

\[ \sigma^2(R) = \frac{1}{2\pi^2}\int_0^\infty {\rm d}k\, k^2 P_{lin}(k, z) F^2(k, R)\]

where \(F(x)\) is a generic filter

Parameters

method_Pk	method used to compute the power spectrum (i.e. the Boltzmann solver); valid choices for method_Pk are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
redshift	the redshift
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum; it can be any name. If this parameter is different from the default value it will be used also in the output directory name
interpType	method to interpolate the power spectrum
k_max	maximum wave vector module up to which the power spectrum is computed
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum
filter	the filter
unit1	true \(\rightarrow\) force cosmological units

Returns: the funciton to compute the not-yet-normalised mass variances

Definition at line 46 of file Sigma.cpp.

◆ m_mass_function()

double cbl::cosmology::Cosmology::m_mass_function	(	const double	Mass,
		std::shared_ptr< void >	mass_function_params
	)

private

auxiliary function to compute the mass function of dark matter haloes (filaments and sheets)

Author: Alfonso Veropalumbo, Jacopo Neri (and Federico Marulli); alfon.nosp@m.so.v.nosp@m.eropa.nosp@m.lumb.nosp@m.o@uni.nosp@m.bo.i.nosp@m.t, jacop.nosp@m.o.ne.nosp@m.ri6@g.nosp@m.mail.nosp@m..com (and feder.nosp@m.ico..nosp@m.marul.nosp@m.li3@.nosp@m.unibo.nosp@m..it)

Parameters

Mass	mass
mass_function_params	function to a container of the mass function parameters

Returns: the mass function, dΦ/dM=dn(M)/dM

Definition at line 105 of file MassFunction.cpp.

◆ m_MF_generator() [1/2]

double cbl::cosmology::Cosmology::m_MF_generator	(	const double	Mass,
		const double	Sigma,
		const double	Dln_Sigma,
		const double	redshift,
		const double	D_N,
		const std::string	model_MF,
		const double	Delta = `200.`,
		const bool	default_delta = `true`,
		const double	delta_t = `1.686`
	)

private

auxiliary function to compute the mass function

Author: Alfonso Veropalumbo, Jacopo Neri (and Federico Marulli); alfon.nosp@m.so.v.nosp@m.eropa.nosp@m.lumb.nosp@m.o@uni.nosp@m.bo.i.nosp@m.t, jacop.nosp@m.o.ne.nosp@m.ri6@g.nosp@m.mail.nosp@m..com (and feder.nosp@m.ico..nosp@m.marul.nosp@m.li3@.nosp@m.unibo.nosp@m..it)

Parameters

Mass	mass
Sigma	σ(mass): the mass variance
Dln_Sigma	dlnσ/dM: the derivative of the mass variance
redshift	the redshift
model_MF	author(s) who proposed the mass function; valid authors are: PS (Press & Schechter), ST (Sheth & Tormen), Jenkins (Jenkins et al. 2001), Warren (Warren et al. 2006), ShenH (halo MF, Shen et al. 2006), ShenF (filament MF, Shen et al. 2006), ShenS (sheet MF, Shen et al. 2006), Pan (Pan 2007), Peacock (Peacock at al. 2007), Reed (Reed et al. 2007), Tinker (Tinker et al. 2008), Crocce (Crocce et al. 2010), Manera (Manera et al. 2010), Courtin (Courtin et al. 2010), Bhattacharya (Bhattacharya et al. 2011), Angulo_FOF (FoF MF, Angulo et al. 2012), Angulo_Sub (SUBFIND MF, Angulo et al. 2012), Watson_FOF (FoF MF, Watson et al. 2012), Watson_SOH (Spherical Overdensity halo MF, Watson et al. 2012), Despali_Z0, Despali_AllZ, Despali_AllZAllCosmo, Despali_HighM (Despali et al. 2016)
D_N	the growth factor, precomputed.
Delta	\(\Delta\), the overdensity
default_delta	true = using function cbl::cosmology::deltac; false = using delta_t*growth factor
delta_t	user defined density contrast at \(z = 0\)

Returns: the mass function, dΦ/dM=dn(M)/dM

Warning: the input parameter \(\Delta\) is the background overdensity, not the critical overdensity \(\Delta_{crit}\); divide \(\Delta_{crit}\) by \(\Omega_M(z)\) (see cbl::cosmology::Cosmology::OmegaM) to obtain the background overdensity; the mass function by Manera et al. (2010) has been tested only for z=0 and z=0.5; the mass function by Despali et al. (2016) is currently implemented only for virial masses and at \(z<1.25\)

Definition at line 211 of file MassFunction.cpp.

◆ m_MF_generator() [2/2]

double cbl::cosmology::Cosmology::m_MF_generator	(	const double	Mass,
		const double	Sigma,
		const double	Dln_Sigma,
		const double	redshift,
		const std::string	model_MF,
		const double	Delta = `200.`,
		const bool	default_delta = `true`,
		const double	delta_t = `1.686`
	)

private

auxiliary function to compute the mass function

Author: Alfonso Veropalumbo, Jacopo Neri (and Federico Marulli); alfon.nosp@m.so.v.nosp@m.eropa.nosp@m.lumb.nosp@m.o@uni.nosp@m.bo.i.nosp@m.t, jacop.nosp@m.o.ne.nosp@m.ri6@g.nosp@m.mail.nosp@m..com (and feder.nosp@m.ico..nosp@m.marul.nosp@m.li3@.nosp@m.unibo.nosp@m..it)

Parameters

Mass	mass
Sigma	σ(mass): the mass variance
Dln_Sigma	dlnσ/dM: the derivative of the mass variance
redshift	the redshift
model_MF	author(s) who proposed the mass function; valid authors are: PS (Press & Schechter), ST (Sheth & Tormen), Jenkins (Jenkins et al. 2001), Warren (Warren et al. 2006), ShenH (halo MF, Shen et al. 2006), ShenF (filament MF, Shen et al. 2006), ShenS (sheet MF, Shen et al. 2006), Pan (Pan 2007), Peacock (Peacock at al. 2007), Reed (Reed et al. 2007), Tinker (Tinker et al. 2008), Crocce (Crocce et al. 2010), Manera (Manera et al. 2010), Courtin (Courtin et al. 2010), Bhattacharya (Bhattacharya et al. 2011), Angulo_FOF (FoF MF, Angulo et al. 2012), Angulo_Sub (SUBFIND MF, Angulo et al. 2012), Watson_FOF (FoF MF, Watson et al. 2012), Watson_SOH (Spherical Overdensity halo MF, Watson et al. 2012), Despali_Z0, Despali_AllZ, Despali_AllZAllCosmo, Despali_HighM (Despali et al. 2016)
Delta	\(\Delta\), the overdensity
default_delta	true = using function cbl::cosmology::deltac; false = using delta_t*growth factor
delta_t	user defined density contrast at \(z = 0\)

Returns: the mass function, dΦ/dM=dn(M)/dM

Warning: the input parameter \(\Delta\) is the background overdensity, not the critical overdensity \(\Delta_{crit}\); divide \(\Delta_{crit}\) by \(\Omega_M(z)\) (see cbl::cosmology::Cosmology::OmegaM) to obtain the background overdensity; the mass function by Manera et al. (2010) has been tested only for z=0 and z=0.5; the mass function by Despali et al. (2016) is currently implemented only for virial masses and at \(z<1.25\)

Definition at line 200 of file MassFunction.cpp.

◆ m_serf_dz()

double cbl::cosmology::Cosmology::m_serf_dz ( const double yy ) const

private

the inverse truncated series necessary to compute sn^-1(s|m) in ASN_DZ

this method computes the inverse truncated series necessary to compute sn^-1(s|m) in ASN_DZ; the shape parameter is fixed to m=(2+3^0.5)/4; it is used to compute the relation between comoving distance and redshift (see Numer. Math. (2010) 116:687–719, T. Fukushima "Fast computation of incomplete elliptic integral of first kind by half argument transformation"; the output of the function corresponds to the second factor of eq. (23))

Author: Mauro Roncarelli; mauro.nosp@m..ron.nosp@m.carel.nosp@m.li@u.nosp@m.nibo..nosp@m.it

Parameters

yy	scalar, argument

Returns: \(\sum_{l=0}^L u_l(m)y^l\), with L fixed to 9

Warning: this method works only for a fixed value of the shape parameter m=(2+3^0.5)/4

Definition at line 1452 of file Cosmology.cpp.

◆ m_sigma2M_notNormalised()

double cbl::cosmology::Cosmology::m_sigma2M_notNormalised	(	const double	mass,
		const std::string	method_Pk,
		const double	redshift,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const std::string	interpType = `"Linear"`,
		const double	k_max = `100.`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`,
		const bool	unit1 = `false`
	)		const

private

the not-yet-normalised mass variance, \(\sigma^2(M)\)

this function computes the not-yet-normalised variance of the linear density field:

\[ \sigma^2(M) = \frac{1}{2\pi^2}\int_0^\infty {\rm d}k\, k^2 P_{lin}(k, z) W^2(k, R)\]

where \(W(x)=(3/x)^3(\sin x-x\cos x)\) and \(R=(3M/4\pi\rho_m)^{1/3}\)

Parameters

mass	the mass
method_Pk	method used to compute the power spectrum (i.e. the Boltzmann solver); valid choices for method_Pk are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
redshift	the redshift
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum; it can be any name. If this parameter is different from the default value it will be used also in the output directory name
interpType	method to interpolate the power spectrum
k_max	maximum wave vector module up to which the power spectrum is computed
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum
unit1	true \(\rightarrow\) force cosmological units

Returns: the not-yet-normalised \(\sigma^2(M)\)

Definition at line 212 of file Sigma.cpp.

◆ m_sigma2R_notNormalised()

double cbl::cosmology::Cosmology::m_sigma2R_notNormalised	(	const double	radius,
		const std::string	method_Pk,
		const double	redshift,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const std::string	interpType = `"Linear"`,
		const double	k_max = `100.`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`,
		const bool	unit1 = `false`
	)		const

private

the not-yet-normalised mass variance, \(\sigma^2(R)\)

this function computes the not-yet-normalised variance of the linear density field:

\[ \sigma^2(R) = \frac{1}{2\pi^2}\int_0^\infty {\rm d}k\, k^2 P_{lin}(k, z) W^2(k, R)\]

where \(W(x)=(3/x)^3(\sin x-x\cos x)\) and \(R=(3M/4\pi\rho_m)^{1/3}\)

Parameters

radius	the radius, \(R\)
method_Pk	method used to compute the power spectrum (i.e. the Boltzmann solver); valid choices for method_Pk are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
redshift	the redshift
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum; it can be any name. If this parameter is different from the default value it will be used also in the output directory name
interpType	method to interpolate the power spectrum
k_max	maximum wave vector module up to which the power spectrum is computed
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum
unit1	true \(\rightarrow\) force cosmological units

Returns: the not-yet-normalised \(\sigma^2(R)\)

Definition at line 137 of file Sigma.cpp.

◆ m_Table_Pk_CAMB_MPTbreeze() [1/2]

void cbl::cosmology::Cosmology::m_Table_Pk_CAMB_MPTbreeze	(	const std::string	code,
		const bool	NL,
		std::vector< double > &	lgkk,
		std::vector< double > &	lgPk,
		const double	redshift,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const double	k_max = `100.`
	)		const

private

write and read the table where the dark matter power spectrum, computed with either CAMB or MPTbreeze, is stored

Parameters

[in]	code	method used to compute the power spectrum; valid codes are: CAMB [http://camb.info/] or MPTbreeze-v1 [http://arxiv.org/abs/1207.1465]
[in]	NL	false \(\rightarrow\) linear power spectrum; true \(\rightarrow\) non-linear power spectrum
[out]	lgkk	vector of log(k)
[out]	lgPk	vector of log(P(k))
[in]	redshift	redshift
[in]	store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
[in]	output_root	output_root of the parameter file used to compute the power spectrum; it can be any name. If this parameter is different from the default value it will be used also in the output directory name
[in]	k_max	maximum wave vector module up to which the power spectrum is computed

Definition at line 327 of file PkXi.cpp.

◆ m_Table_Pk_CAMB_MPTbreeze() [2/2]

void cbl::cosmology::Cosmology::m_Table_Pk_CAMB_MPTbreeze	(	const std::string	code,
		const bool	NL,
		std::vector< std::vector< double >> &	lgkk,
		std::vector< std::vector< double >> &	lgPk,
		const std::vector< double >	redshift,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const double	k_max = `100.`
	)		const

private

write and read the table where the dark matter power spectrum, computed with either CAMB or MPTbreeze, is stored

Parameters

[in]	code	method used to compute the power spectrum; valid codes are: CAMB [http://camb.info/] or MPTbreeze-v1 [http://arxiv.org/abs/1207.1465]
[in]	NL	false \(\rightarrow\) linear power spectrum; true \(\rightarrow\) non-linear power spectrum
[out]	lgkk	vector of vectors containing the log(k) at each redshift
[out]	lgPk	vector of vectors containing the log(P(k)) at each redshift
[in]	redshift	vector of redshifts
[in]	store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
[in]	output_root	output_root of the parameter file used to compute the power spectrum; it can be any name. If this parameter is different from the default value it will be used also in the output directory name
[in]	k_max	maximum wave vector module up to which the power spectrum is computed

Definition at line 504 of file PkXi.cpp.

◆ m_Table_Pk_CLASS() [1/2]

void cbl::cosmology::Cosmology::m_Table_Pk_CLASS	(	const bool	NL,
		std::vector< double > &	lgkk,
		std::vector< double > &	lgPk,
		const double	redshift,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const double	k_max = `100.`
	)		const

private

write and read the table where the dark matter power spectrum computed with CLASS is stored

Parameters

[in]	NL	false \(\rightarrow\) linear power spectrum; true \(\rightarrow\) non-linear power spectrum
[out]	lgkk	vector of log(k)
[out]	lgPk	vector of log(P(k))
[in]	redshift	redshift
[in]	store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
[in]	output_root	output_root of the parameter file used to compute the power spectrum; it can be any name. If this parameter is different from the default value it will be used also in the output directory name
[in]	k_max	maximum wave vector module up to which the power spectrum is computed

Definition at line 740 of file PkXi.cpp.

◆ m_Table_Pk_CLASS() [2/2]

void cbl::cosmology::Cosmology::m_Table_Pk_CLASS	(	const bool	NL,
		std::vector< std::vector< double >> &	lgkk,
		std::vector< std::vector< double >> &	lgPk,
		const std::vector< double >	redshift,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const double	k_max = `100.`
	)		const

private

write and read the table where the dark matter power spectrum computed with CLASS is stored

Parameters

[in]	NL	false \(\rightarrow\) linear power spectrum; true \(\rightarrow\) non-linear power spectrum
[out]	lgkk	vector of vectors containing the log(k) at each redshift
[out]	lgPk	vector of vectors containing the log(P(k)) at each redshift
[in]	redshift	vector of redshifts
[in]	store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
[in]	output_root	output_root of the parameter file used to compute the power spectrum; it can be any name. If this parameter is different from the default value it will be used also in the output directory name
[in]	k_max	maximum wave vector module up to which the power spectrum is computed

Definition at line 866 of file PkXi.cpp.

◆ m_Table_Pk_parameterFile()

void cbl::cosmology::Cosmology::m_Table_Pk_parameterFile	(	const std::string	code,
		const std::string	file_par,
		const bool	NL,
		std::vector< double > &	lgkk,
		std::vector< double > &	lgPk,
		const double	redshift,
		const std::string	output_root = `"test"`
	)		const

private

write and read the table where the dark matter power spectrum is stored; it is used when a parameter file is provided in input

Parameters

[in]	code	method used to compute the power spectrum; valid codes are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465]
[in]	file_par	name of the parameter file; if a parameter file is provided (i.e. file_par!=NULL), it will be used, ignoring the cosmological parameters of the object
[in]	NL	false \(\rightarrow\) linear power spectrum; true \(\rightarrow\) non-linear power spectrum
[out]	lgkk	vector of log(k)
[out]	lgPk	vector of log(P(k))
[in]	redshift	redshift
[in]	output_root	output_root of the parameter file used to compute the power spectrum; it can be any name. If this parameter is different from the default value it will be used also in the output directory name

Warning: the input output_root parameter must be the same as the one in the parameter file

Definition at line 1058 of file PkXi.cpp.

◆ M_vir()

double cbl::cosmology::Cosmology::M_vir	(	const double	r_vir,
		const double	redshift,
		const std::string	author = `"BryanNorman"`,
		const bool	unit1 = `false`
	)		const

the virial mass, given the virial radius and the redshift

this function computes the virial halo mass as follows:

\[M_{vir}(z) = \frac{4}{3}\pi r_{vir}^3\Delta_c(z)\rho_{crit}(z) = \frac{r_{vir}^3\Delta_c(z)H^2(z)}{2G}\]

where \(\Delta_c(z)\) is computed by cbl::cosmology::Cosmology::Delta_c and \(\rho_{crit}(z)\) is computed by cbl::cosmology::Cosmology::rho_crit

Parameters

r_vir	the virial radius
redshift	the redshift
author	the author of the \(\Delta_c(z)\) equation (see cbl::cosmology::Cosmology::Delta_c)
unit1	true \(\rightarrow\) force cosmological units

Returns: \(M_{vir}\)

Definition at line 1322 of file Cosmology.cpp.

◆ Mag_Volume_limited()

double cbl::cosmology::Cosmology::Mag_Volume_limited	(	const double	z_max = `1.`,
		const double	mag_lim = `-20.`
	)		const

maximum absolute magnitude to have a volume-limited catalogue

Parameters

z_max	maximum redshift
mag_lim	magnitude limit

Returns: r_s

Definition at line 1027 of file Cosmology.cpp.

◆ mass_function() [1/5]

double cbl::cosmology::Cosmology::mass_function	(	const double	Mass,
		const double	redshift,
		const std::string	model_MF,
		const std::string	method_SS,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const double	Delta = `200.`,
		const std::string	interpType = `"Linear"`,
		const int	norm = `-1`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`,
		const bool	default_delta = `true`,
		const double	delta_t = `1.686`
	)

the mass function of dark matter haloes (filaments and sheets)

Author: Alfonso Veropalumbo, Jacopo Neri (and Federico Marulli); alfon.nosp@m.so.v.nosp@m.eropa.nosp@m.lumb.nosp@m.o@uni.nosp@m.bo.i.nosp@m.t, jacop.nosp@m.o.ne.nosp@m.ri6@g.nosp@m.mail.nosp@m..com (and feder.nosp@m.ico..nosp@m.marul.nosp@m.li3@.nosp@m.unibo.nosp@m..it)

Parameters

Mass	mass
redshift	the redshift
model_MF	author(s) who proposed the mass function; valid authors are: PS (Press & Schechter), ST (Sheth & Tormen), Jenkins (Jenkins et al. 2001), Warren (Warren et al. 2006), ShenH (halo MF, Shen et al. 2006), ShenF (filament MF, Shen et al. 2006), ShenS (sheet MF, Shen et al. 2006), Pan (Pan 2007), Peacock (Peacock at al. 2007), Reed (Reed et al. 2007), Tinker (Tinker et al. 2008), Crocce (Crocce et al. 2010), Manera (Manera et al. 2010), Courtin (Courtin et al. 2010), Bhattacharya (Bhattacharya et al. 2011), Angulo_FOF (FoF MF, Angulo et al. 2012), Angulo_Sub (SUBFIND MF, Angulo et al. 2012), Watson_FOF (FoF MF, Watson et al. 2012), Watson_SOH (Spherical Overdensity halo MF, Watson et al. 2012), Despali_Z0, Despali_AllZ, Despali_AllZAllCosmo, Despali_HighM (Despali et al. 2016)
method_SS	method used to compute the power spectrum and σ(mass); valid method_SS are: CAMB [http://camb.info/], CLASS [http://class-code.net/], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
Delta	\(\Delta\), the overdensity
interpType	method to interpolate the power spectrum
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
prec	accuracy of the integration
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum
default_delta	true = using function cbl::cosmology::deltac; false = using delta_t*growth factor
delta_t	user defined density contrast at \(z = 0\)

Returns: the mass function, dΦ/dM=dn(M)/dM

Warning: the input parameter \(\Delta\) is the background overdensity, not the critical overdensity \(\Delta_{crit}\); divide \(\Delta_{crit}\) by \(\Omega_M(z)\) (see cbl::cosmology::Cosmology::OmegaM) to obtain the background overdensity; the mass function by Manera et al. (2010) has been tested only for z=0 and z=0.5; the mass function by Despali et al. (2016) is currently implemented only for virial masses and at \(z<1.25\)

Definition at line 45 of file MassFunction.cpp.

◆ mass_function() [2/5]

double cbl::cosmology::Cosmology::mass_function	(	const double	Mass,
		const double	Sigma,
		const double	Dln_Sigma,
		const double	redshift,
		const double	D_N,
		const std::string	model_MF,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const double	Delta = `200.`,
		const std::string	interpType = `"Linear"`,
		const int	norm = `-1`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`,
		const std::string	method_SS = `"CAMB"`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`
	)

the mass function of dark matter haloes (filaments and sheets) computed quickly passing directly the mass variance and its derivative as inputs

Author: Alfonso Veropalumbo, Jacopo Neri (and Federico Marulli); alfon.nosp@m.so.v.nosp@m.eropa.nosp@m.lumb.nosp@m.o@uni.nosp@m.bo.i.nosp@m.t, jacop.nosp@m.o.ne.nosp@m.ri6@g.nosp@m.mail.nosp@m..com (and feder.nosp@m.ico..nosp@m.marul.nosp@m.li3@.nosp@m.unibo.nosp@m..it)

Parameters

Mass	mass
Sigma	σ(mass): the mass variance
Dln_Sigma	dlnσ/dM: the derivative of the mass variance
redshift	the redshift
D_N	the amplitude of the growing mode
model_MF	author(s) who proposed the mass function; valid authors are: PS (Press & Schechter), ST (Sheth & Tormen), Jenkins (Jenkins et al. 2001), Warren (Warren et al. 2006), ShenH (halo MF, Shen et al. 2006), ShenF (filament MF, Shen et al. 2006), ShenS (sheet MF, Shen et al. 2006), Pan (Pan 2007), Peacock (Peacock at al. 2007), Reed (Reed et al. 2007), Tinker (Tinker et al. 2008), Crocce (Crocce et al. 2010), Manera (Manera et al. 2010), Courtin (Courtin et al. 2010), Bhattacharya (Bhattacharya et al. 2011), Angulo_FOF (FoF MF, Angulo et al. 2012), Angulo_Sub (SUBFIND MF, Angulo et al. 2012), Watson_FOF (FoF MF, Watson et al. 2012), Watson_SOH (Spherical Overdensity halo MF, Watson et al. 2012), Despali_Z0, Despali_AllZ, Despali_AllZAllCosmo, Despali_HighM (Despali et al. 2016)
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
Delta	\(\Delta\), the overdensity
interpType	method to interpolate the power spectrum
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed to estimate the power spectrum normalisation; this parameter is used only if norm=1
k_max	maximum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
prec	accuracy of the integration
method_SS	method used to compute the power spectrum and σ(mass); valid method_SS are: CAMB [http://camb.info/], CLASS [http://class-code.net/], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum

Returns: the mass function, dΦ/dM=dn(M)/dM

Warning: the input parameter \(\Delta\) is the background overdensity, not the critical overdensity \(\Delta_{crit}\); divide \(\Delta_{crit}\) by \(\Omega_M(z)\) (see cbl::cosmology::Cosmology::OmegaM) to obtain the background overdensity; the mass function by Manera et al. (2010) has been tested only for z=0 and z=0.5; the mass function by Despali et al. (2016) is currently implemented only for virial masses and at \(z<1.25\)

Definition at line 184 of file MassFunction.cpp.

◆ mass_function() [3/5]

double cbl::cosmology::Cosmology::mass_function	(	const double	Mass,
		const double	Sigma,
		const double	Dln_Sigma,
		const double	redshift,
		const std::string	model_MF,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const double	Delta = `200.`,
		const std::string	interpType = `"Linear"`,
		const int	norm = `-1`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`,
		const std::string	method_SS = `"CAMB"`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`
	)

the mass function of dark matter haloes (filaments and sheets) computed quickly passing directly the mass variance and its derivative as inputs

Author: Alfonso Veropalumbo, Jacopo Neri (and Federico Marulli); alfon.nosp@m.so.v.nosp@m.eropa.nosp@m.lumb.nosp@m.o@uni.nosp@m.bo.i.nosp@m.t, jacop.nosp@m.o.ne.nosp@m.ri6@g.nosp@m.mail.nosp@m..com (and feder.nosp@m.ico..nosp@m.marul.nosp@m.li3@.nosp@m.unibo.nosp@m..it)

Parameters

Mass	mass
Sigma	σ(mass): the mass variance
Dln_Sigma	dlnσ/dM: the derivative of the mass variance
redshift	the redshift
model_MF	author(s) who proposed the mass function; valid authors are: PS (Press & Schechter), ST (Sheth & Tormen), Jenkins (Jenkins et al. 2001), Warren (Warren et al. 2006), ShenH (halo MF, Shen et al. 2006), ShenF (filament MF, Shen et al. 2006), ShenS (sheet MF, Shen et al. 2006), Pan (Pan 2007), Peacock (Peacock at al. 2007), Reed (Reed et al. 2007), Tinker (Tinker et al. 2008), Crocce (Crocce et al. 2010), Manera (Manera et al. 2010), Courtin (Courtin et al. 2010), Bhattacharya (Bhattacharya et al. 2011), Angulo_FOF (FoF MF, Angulo et al. 2012), Angulo_Sub (SUBFIND MF, Angulo et al. 2012), Watson_FOF (FoF MF, Watson et al. 2012), Watson_SOH (Spherical Overdensity halo MF, Watson et al. 2012), Despali_Z0, Despali_AllZ, Despali_AllZAllCosmo, Despali_HighM (Despali et al. 2016)
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
Delta	\(\Delta\), the overdensity
interpType	method to interpolate the power spectrum
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed to estimate the power spectrum normalisation; this parameter is used only if norm=1
k_max	maximum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
prec	accuracy of the integration
method_SS	method used to compute the power spectrum and σ(mass); valid method_SS are: CAMB [http://camb.info/], CLASS [http://class-code.net/], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum

Returns: the mass function, dΦ/dM=dn(M)/dM

Warning: the input parameter \(\Delta\) is the background overdensity, not the critical overdensity \(\Delta_{crit}\); divide \(\Delta_{crit}\) by \(\Omega_M(z)\) (see cbl::cosmology::Cosmology::OmegaM) to obtain the background overdensity; the mass function by Manera et al. (2010) has been tested only for z=0 and z=0.5; the mass function by Despali et al. (2016) is currently implemented only for virial masses and at \(z<1.25\)

Definition at line 168 of file MassFunction.cpp.

◆ mass_function() [4/5]

std::vector< double > cbl::cosmology::Cosmology::mass_function	(	const std::vector< double >	mass,
		const double	z_min,
		const double	z_max,
		const std::string	model_MF,
		const std::string	method_SS,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const double	Delta = `200`,
		const bool	isDelta_critical = `false`,
		const std::string	interpType = `"Linear"`,
		const double	k_max = `100.`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`
	)

mass function for a range of masses

Author: Alfonso Veropalumbo; alfon.nosp@m.so.v.nosp@m.eropa.nosp@m.lumb.nosp@m.o@uni.nosp@m.bo.i.nosp@m.t

Parameters

mass	vector of mass
z_min	minimum redshift
z_max	maximum redshift
model_MF	author(s) who proposed the mass function; valid authors are: PS (Press & Schechter), ST (Sheth & Tormen), Jenkins (Jenkins et al. 2001), Warren (Warren et al. 2006), ShenH (halo MF, Shen et al. 2006), ShenF (filament MF, Shen et al. 2006), ShenS (sheet MF, Shen et al. 2006), Pan (Pan 2007), Peacock (Peacock at al. 2007), Reed (Reed et al. 2007), Tinker (Tinker et al. 2008), Crocce (Crocce et al. 2010), Manera (Manera et al. 2010), Courtin (Courtin et al. 2010), Bhattacharya (Bhattacharya et al. 2011), Angulo_FOF (FoF MF, Angulo et al. 2012), Angulo_Sub (SUBFIND MF, Angulo et al. 2012), Watson_FOF (FoF MF, Watson et al. 2012), Watson_SOH (Spherical Overdensity halo MF, Watson et al. 2012), Despali_Z0, Despali_AllZ, Despali_AllZAllCosmo, Despali_HighM (Despali et al. 2016)
method_SS	method used to compute the power spectrum and σ(mass); valid method_SS are: CAMB [http://camb.info/], CLASS [http://class-code.net/], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
Delta	\(\Delta\), the overdensity
isDelta_critical	\(\rightarrow\) \(\Delta\) is the overdensity defined with respect to the critical density
interpType	method to interpolate the power spectrum
k_max	maximum wave vector module up to which the power spectrum is computed
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum

Returns: n_haloes: the number density of dark matter haloes (per steradian or square degree)

Warning: the input parameter \(\Delta\) is the background overdensity, not the critical overdensity \(\Delta_{crit}\); divide \(\Delta_{crit}\) by \(\Omega_M(z)\) (see cbl::cosmology::Cosmology::OmegaM) to obtain the background overdensity; the mass function by Manera et al. (2010) has been tested only for z=0 and z=0.5; the mass function by Despali et al. (2016) is currently implemented only for virial masses and at \(z<1.25\)

Definition at line 655 of file MassFunction.cpp.

◆ mass_function() [5/5]

vector< double > cbl::cosmology::Cosmology::mass_function	(	const std::vector< double >	Mass,
		const std::vector< double >	Sigma,
		const std::vector< double >	Dln_Sigma,
		const double	redshift,
		const std::string	model_MF,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const double	Delta = `200.`,
		const std::string	interpType = `"Linear"`,
		const int	norm = `-1`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`,
		const std::string	method_SS = `"CAMB"`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`
	)

the mass function of dark matter haloes (filaments and sheets) computed quickly passing directly the mass variance and its derivative as inputs. This function takes vector in input and compute the mass function for the input masses

Author: Alfonso Veropalumbo, Jacopo Neri (and Federico Marulli); alfon.nosp@m.so.v.nosp@m.eropa.nosp@m.lumb.nosp@m.o@uni.nosp@m.bo.i.nosp@m.t, jacop.nosp@m.o.ne.nosp@m.ri6@g.nosp@m.mail.nosp@m..com (and feder.nosp@m.ico..nosp@m.marul.nosp@m.li3@.nosp@m.unibo.nosp@m..it)

Parameters

Mass	mass
Sigma	σ(mass): the mass variance
Dln_Sigma	dlnσ/dM: the derivative of the mass variance
redshift	the redshift
model_MF	author(s) who proposed the mass function; valid authors are: PS (Press & Schechter), ST (Sheth & Tormen), Jenkins (Jenkins et al. 2001), Warren (Warren et al. 2006), ShenH (halo MF, Shen et al. 2006), ShenF (filament MF, Shen et al. 2006), ShenS (sheet MF, Shen et al. 2006), Pan (Pan 2007), Peacock (Peacock at al. 2007), Reed (Reed et al. 2007), Tinker (Tinker et al. 2008), Crocce (Crocce et al. 2010), Manera (Manera et al. 2010), Courtin (Courtin et al. 2010), Bhattacharya (Bhattacharya et al. 2011), Angulo_FOF (FoF MF, Angulo et al. 2012), Angulo_Sub (SUBFIND MF, Angulo et al. 2012), Watson_FOF (FoF MF, Watson et al. 2012), Watson_SOH (Spherical Overdensity halo MF, Watson et al. 2012), Despali_Z0, Despali_AllZ, Despali_AllZAllCosmo, Despali_HighM (Despali et al. 2016)
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
Delta	\(\Delta\), the overdensity
interpType	method to interpolate the power spectrum
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed to estimate the power spectrum normalisation; this parameter is used only if norm=1
k_max	maximum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
prec	accuracy of the integration
method_SS	method used to compute the power spectrum and σ(mass); valid method_SS are: CAMB [http://camb.info/], CLASS [http://class-code.net/], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum

Returns: the mass function, dΦ/dM=dn(M)/dM

Warning: the input parameter \(\Delta\) is the background overdensity, not the critical overdensity \(\Delta_{crit}\); divide \(\Delta_{crit}\) by \(\Omega_M(z)\) (see cbl::cosmology::Cosmology::OmegaM) to obtain the background overdensity; the mass function by Manera et al. (2010) has been tested only for z=0 and z=0.5; the mass function by Despali et al. (2016) is currently implemented only for virial masses and at \(z<1.25\)

Definition at line 45 of file MassFunction_vector.cpp.

◆ mass_function_fast()

double cbl::cosmology::Cosmology::mass_function_fast	(	const double	Mass,
		const double	redshift,
		const std::string	model_MF,
		const std::string	method_SS,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const double	Delta = `200.`,
		const std::string	interpType = `"Linear"`,
		const int	norm = `-1`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`
	)

the mass function of dark matter haloes (filaments and sheets) computed quickly using a grid

Author: Alfonso Veropalumbo, Jacopo Neri (and Federico Marulli); alfon.nosp@m.so.v.nosp@m.eropa.nosp@m.lumb.nosp@m.o@uni.nosp@m.bo.i.nosp@m.t, jacop.nosp@m.o.ne.nosp@m.ri6@g.nosp@m.mail.nosp@m..com (and feder.nosp@m.ico..nosp@m.marul.nosp@m.li3@.nosp@m.unibo.nosp@m..it)

Parameters

Mass	mass
redshift	the redshift
model_MF	author(s) who proposed the mass function; valid authors are: PS (Press & Schechter), ST (Sheth & Tormen), Jenkins (Jenkins et al. 2001), Warren (Warren et al. 2006), ShenH (halo MF, Shen et al. 2006), ShenF (filament MF, Shen et al. 2006), ShenS (sheet MF, Shen et al. 2006), Pan (Pan 2007), Peacock (Peacock at al. 2007), Reed (Reed et al. 2007), Tinker (Tinker et al. 2008), Crocce (Crocce et al. 2010), Manera (Manera et al. 2010), Courtin (Courtin et al. 2010), Bhattacharya (Bhattacharya et al. 2011), Angulo_FOF (FoF MF, Angulo et al. 2012), Angulo_Sub (SUBFIND MF, Angulo et al. 2012), Watson_FOF (FoF MF, Watson et al. 2012), Watson_SOH (Spherical Overdensity halo MF, Watson et al. 2012), Despali_Z0, Despali_AllZ, Despali_AllZAllCosmo, Despali_HighM (Despali et al. 2016)
method_SS	method used to compute the power spectrum and σ(mass); valid method_SS are: CAMB [http://camb.info/], CLASS [http://class-code.net/], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. . If this parameter is different from the default value it will be used also in the output directory name
Delta	\(\Delta\), the overdensity
interpType	method to interpolate the power spectrum
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
prec	accuracy of the integration
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum

Returns: the mass function, dΦ/dM=dn(M)/dM

Warning: the input parameter \(\Delta\) is the background overdensity, not the critical overdensity \(\Delta_{crit}\); divide \(\Delta_{crit}\) by \(\Omega_M(z)\) (see cbl::cosmology::Cosmology::OmegaM) to obtain the background overdensity; the mass function by Manera et al. (2010) has been tested only for z=0 and z=0.5; the mass function by Despali et al. (2016) is currently implemented only for virial masses and at \(z<1.25\)

Definition at line 130 of file MassFunction.cpp.

◆ mass_function_fR()

double cbl::cosmology::Cosmology::mass_function_fR	(	const double	Mass,
		const double	redshift,
		const std::string	model_MF,
		const double	f_R0 = `0.`,
		const bool	store_output = `true`,
		const double	Delta = `200.`,
		const std::string	interpType = `"Linear"`,
		const int	norm = `-1`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`,
		const bool	default_delta = `true`,
		const double	delta_t = `1.686`
	)

the mass function of dark matter haloes in f(R) cosmologies (see Hu & Sawicki 2007) computed with the Boltzmann solver MGCAMB

Author: Leonardo Gabriele Coppola and Sofia Contarini; leona.nosp@m.rdo..nosp@m.coppo.nosp@m.la@s.nosp@m.tudio.nosp@m..uni.nosp@m.bo.it, sofia.nosp@m..con.nosp@m.tarin.nosp@m.i3@u.nosp@m.nibo..nosp@m.it

Parameters

Mass	the mass
redshift	the redshift
model_MF	author(s) who proposed the mass function; valid authors are: PS (Press & Schechter), ST (Sheth & Tormen), Jenkins (Jenkins et al. 2001), Warren (Warren et al. 2006), ShenH (halo MF, Shen et al. 2006), ShenF (filament MF, Shen et al. 2006), ShenS (sheet MF, Shen et al. 2006), Pan (Pan 2007), Peacock (Peacock at al. 2007), Reed (Reed et al. 2007), Tinker (Tinker et al. 2008), Crocce (Crocce et al. 2010), Manera (Manera et al. 2010), Courtin (Courtin et al. 2010), Bhattacharya (Bhattacharya et al. 2011), Angulo_FOF (FoF MF, Angulo et al. 2012), Angulo_Sub (SUBFIND MF, Angulo et al. 2012), Watson_FOF (FoF MF, Watson et al. 2012), Watson_SOH (Spherical Overdensity halo MF, Watson et al. 2012), Despali_Z0, Despali_AllZ, Despali_AllZAllCosmo, Despali_HighM (Despali et al. 2016)
f_R0	value of the parameter \(f_\mathrm{R0}\)
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
Delta	\(\Delta\), the overdensity
interpType	method to interpolate the power spectrum
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
prec	accuracy of the integration
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum
default_delta	true = using function cbl::cosmology::deltac; false = using delta_t*growth factor
delta_t	user defined density contrast at \(z = 0\)

Returns: the mass function, dΦ/dM=dn(M)/dM

Warning: the input parameter \(\Delta\) is the background overdensity, not the critical overdensity \(\Delta_{crit}\); divide \(\Delta_{crit}\) by \(\Omega_M(z)\) (see cbl::cosmology::Cosmology::OmegaM) to obtain the background overdensity; the mass function by Manera et al. (2010) has been tested only for z=0 and z=0.5; the mass function by Despali et al. (2016) is currently implemented only for virial masses and at \(z<1.25\)

Definition at line 67 of file MassFunction.cpp.

◆ mass_function_selection_function_vector()

std::vector< double > cbl::cosmology::Cosmology::mass_function_selection_function_vector	(	const std::vector< double >	mass,
		const double	z_min,
		const double	z_max,
		const std::string	model_MF,
		const std::string	method_SS,
		const std::string	selection_function_file,
		const std::vector< int >	column = `{}`,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const double	Delta = `200`,
		const bool	isDelta_critical = `false`,
		const std::string	interpType = `"Linear"`,
		const double	k_max = `100.`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`
	)

mass function given a selection function

Author: Alfonso Veropalumbo; alfon.nosp@m.so.v.nosp@m.eropa.nosp@m.lumb.nosp@m.o@uni.nosp@m.bo.i.nosp@m.t

Parameters

mass	vector of mass
z_min	minimum redshift
z_max	maximum redshift
model_MF	author(s) who proposed the mass function; valid authors are: PS (Press & Schechter), ST (Sheth & Tormen), Jenkins (Jenkins et al. 2001), Warren (Warren et al. 2006), ShenH (halo MF, Shen et al. 2006), ShenF (filament MF, Shen et al. 2006), ShenS (sheet MF, Shen et al. 2006), Pan (Pan 2007), Peacock (Peacock at al. 2007), Reed (Reed et al. 2007), Tinker (Tinker et al. 2008), Crocce (Crocce et al. 2010), Manera (Manera et al. 2010), Courtin (Courtin et al. 2010), Bhattacharya (Bhattacharya et al. 2011), Angulo_FOF (FoF MF, Angulo et al. 2012), Angulo_Sub (SUBFIND MF, Angulo et al. 2012), Watson_FOF (FoF MF, Watson et al. 2012), Watson_SOH (Spherical Overdensity halo MF, Watson et al. 2012), Despali_Z0, Despali_AllZ, Despali_AllZAllCosmo, Despali_HighM (Despali et al. 2016)
method_SS	method used to compute the power spectrum and σ(mass); valid method_SS are: CAMB [http://camb.info/], CLASS [http://class-code.net/], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
selection_function_file	input file where the selection function is stored
column	the columns to be read
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
Delta	\(\Delta\), the overdensity
isDelta_critical	\(\rightarrow\) \(\Delta\) is the overdensity defined with respect to the critical density
interpType	method to interpolate the power spectrum
k_max	maximum wave vector module up to which the power spectrum is computed
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum

Returns: n_haloes: the number density of dark matter haloes (per steradian or square degree)

Warning: the input parameter \(\Delta\) is the background overdensity, not the critical overdensity \(\Delta_{crit}\); divide \(\Delta_{crit}\) by \(\Omega_M(z)\) (see cbl::cosmology::Cosmology::OmegaM) to obtain the background overdensity; the mass function by Manera et al. (2010) has been tested only for z=0 and z=0.5; the mass function by Despali et al. (2016) is currently implemented only for virial masses and at \(z<1.25\)

wrapper::gsl::GSL_integrate_qag(funcD, z_min, z_max);

Definition at line 703 of file MassFunction.cpp.

◆ massive_neutrinos()

int cbl::cosmology::Cosmology::massive_neutrinos ( ) const

inline

get the private member Cosmology::m_massive_neutrinos

Returns: the number of degenerate massive neutrino species

Definition at line 1149 of file Cosmology.h.

◆ massless_neutrinos()

double cbl::cosmology::Cosmology::massless_neutrinos ( ) const

inline

get the private member Cosmology::m_massless_neutrinos

Returns: N_eff: the effective number (for QED + non-instantaneous decoupling)

Definition at line 1142 of file Cosmology.h.

◆ max_redshift()

double cbl::cosmology::Cosmology::max_redshift	(	const double	Volume,
		const double	Area,
		const double	z_min
	)		const

maximum redshift for a given volume, sky area and minimum redshift

Parameters

Volume	volume
Area	sky area
z_min	minimum redshift

Returns: redshift

Definition at line 1223 of file Cosmology.cpp.

◆ mean_redshift_haloes_selection_function()

double cbl::cosmology::Cosmology::mean_redshift_haloes_selection_function	(	const double	z_min,
		const double	z_max,
		const double	Mass_min,
		const double	Mass_max,
		const std::string	model_MF,
		const std::string	method_SS,
		const std::string	selection_function_file,
		const std::vector< int >	column = `{}`,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const double	Delta = `200`,
		const bool	isDelta_critical = `false`,
		const std::string	interpType = `"Linear"`,
		const double	k_max = `100.`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`
	)

the mean redshift of a dark matter haloe sample, given a selection function

Author: Alfonso Veropalumbo; alfon.nosp@m.so.v.nosp@m.eropa.nosp@m.lumb.nosp@m.o@uni.nosp@m.bo.i.nosp@m.t

Parameters

z_min	minimum redshift
z_max	maximum redshift
Mass_min	minimum halo mass
Mass_max	maximum halo mass
model_MF	author(s) who proposed the mass function; valid authors are: PS (Press & Schechter), ST (Sheth & Tormen), Jenkins (Jenkins et al. 2001), Warren (Warren et al. 2006), ShenH (halo MF, Shen et al. 2006), ShenF (filament MF, Shen et al. 2006), ShenS (sheet MF, Shen et al. 2006), Pan (Pan 2007), Peacock (Peacock at al. 2007), Reed (Reed et al. 2007), Tinker (Tinker et al. 2008), Crocce (Crocce et al. 2010), Manera (Manera et al. 2010), Courtin (Courtin et al. 2010), Bhattacharya (Bhattacharya et al. 2011), Angulo_FOF (FoF MF, Angulo et al. 2012), Angulo_Sub (SUBFIND MF, Angulo et al. 2012), Watson_FOF (FoF MF, Watson et al. 2012), Watson_SOH (Spherical Overdensity halo MF, Watson et al. 2012), Despali_Z0, Despali_AllZ, Despali_AllZAllCosmo, Despali_HighM (Despali et al. 2016)
method_SS	method used to compute the power spectrum and σ(mass); valid method_SS are: CAMB [http://camb.info/], CLASS [http://class-code.net/], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
selection_function_file	input file where the selection function is stored
column	the columns to be read
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
Delta	\(\Delta\), the overdensity
isDelta_critical	\(\rightarrow\) \(\Delta\) is the overdensity defined with respect to the critical density
interpType	method to interpolate the power spectrum
k_max	maximum wave vector module up to which the power spectrum is computed
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum

Returns: the mean redshift of dark matter haloes

Warning: the input parameter \(\Delta\) is the background overdensity, not the critical overdensity \(\Delta_{crit}\); divide \(\Delta_{crit}\) by \(\Omega_M(z)\) (see cbl::cosmology::Cosmology::OmegaM) to obtain the background overdensity; the mass function by Manera et al. (2010) has been tested only for z=0 and z=0.5; the mass function by Despali et al. (2016) is currently implemented only for virial masses and at \(z<1.25\)

Definition at line 890 of file MassFunction.cpp.

◆ medianwf()

void cbl::cosmology::Cosmology::medianwf	(	const double	ff,
		const std::string	model_model,
		std::vector< double > &	wf
	)		const

median formation w

Author: Carlo Giocoli; cgioc.nosp@m.oli@.nosp@m.gmail.nosp@m..com

Parameters

[in]	ff	assembled fraction
[in]	model_model	valid authors are: NS (Nusser and Sheth), GTS (Giocoli et al. 2012)
[out]	wf	vector of w(f)

Definition at line 118 of file MassGrowth.cpp.

◆ medianzf()

void cbl::cosmology::Cosmology::medianzf	(	const double	ff,
		const double	mass,
		const double	z0,
		const std::string	model_model,
		const std::string	method_SS,
		std::vector< double > &	zf,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`
	)		const

median formation z

Author: Carlo Giocoli; cgioc.nosp@m.oli@.nosp@m.gmail.nosp@m..com

Parameters

[in]	ff	assembled fraction
[in]	mass	halo mass
[in]	z0	redshift when the halo has a mass mass
[in]	model_model	valid authors are: NS (Nusser and Sheth), GTS (Giocoli et al. 2012)
	method_SS	method used to compute the power spectrum and σ(mass); valid method_SS are: CAMB [http://camb.info/], CLASS [http://class-code.net/], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
[out]	zf	vector of z(f)
	store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
	output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name

Definition at line 192 of file MassGrowth.cpp.

◆ MF_correction()

double cbl::cosmology::Cosmology::MF_correction	(	const double	mass,
		const double	redshift,
		const std::string	method_Pk,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const std::string	interpType = `"Linear"`,
		const int	norm = `-1`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`
	)

correction to the halo mass in non-Gaussian cosmologies

Author: Cosimo Fedeli; cosim.nosp@m.o.fe.nosp@m.deli@.nosp@m.oabo.nosp@m..inaf.nosp@m..it

Parameters

mass	the halo mass
redshift	the redshift
method_Pk	method used to compute the power spectrum (i.e. the Boltzmann solver); valid choices for method_Pk are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	the output_root parameter of the parameter file used to compute the power spectrum; it can be any name. If this parameter is different from the default value it will be used also in the output directory name
interpType	method to interpolate the power spectrum
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
prec	accuracy of the integration
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum

Returns: bias correction

Definition at line 552 of file NG.cpp.

◆ MhaloMin()

double cbl::cosmology::Cosmology::MhaloMin	(	const int	n_halo,
		const double	Area,
		const bool	angle_rad,
		const double	z_min,
		const double	z_max,
		const double	Mmax,
		const double	lgM1_guess,
		const double	lgM2_guess,
		const std::string	model_MF,
		const std::string	method_SS,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const double	Delta = `200`,
		const std::string	interpType = `"Linear"`,
		const double	k_max = `100.`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`
	)		const

minimum halo mass, given the number of haloes in a given region of sky

Author: Alfonso Veropalumbo, Jacopo Neri (and Federico Marulli); alfon.nosp@m.so.v.nosp@m.eropa.nosp@m.lumb.nosp@m.o@uni.nosp@m.bo.i.nosp@m.t, jacop.nosp@m.o.ne.nosp@m.ri6@g.nosp@m.mail.nosp@m..com (and feder.nosp@m.ico..nosp@m.marul.nosp@m.li3@.nosp@m.unibo.nosp@m..it)

Parameters

n_halo	number density of dark matter haloes
Area	sky area
angle_rad	0 \(\rightarrow\) Ω in square degrees; 1 \(\rightarrow\) Ω in steradians
z_min	minimum redshift
z_max	maximum redshift
Mmax	maximum mass
lgM1_guess	logarithm of the minimum mass used by the root finder
lgM2_guess	logarithm of the maximum mass used by the root finder
model_MF	author(s) who proposed the mass function; valid authors are: PS (Press & Schechter), ST (Sheth & Tormen), Jenkins (Jenkins et al. 2001), Warren (Warren et al. 2006), ShenH (halo MF, Shen et al. 2006), ShenF (filament MF, Shen et al. 2006), ShenS (sheet MF, Shen et al. 2006), Pan (Pan 2007), Peacock (Peacock at al. 2007), Reed (Reed et al. 2007), Tinker (Tinker et al. 2008), Crocce (Crocce et al. 2010), Manera (Manera et al. 2010), Courtin (Courtin et al. 2010), Bhattacharya (Bhattacharya et al. 2011), Angulo_FOF (FoF MF, Angulo et al. 2012), Angulo_Sub (SUBFIND MF, Angulo et al. 2012), Watson_FOF (FoF MF, Watson et al. 2012), Watson_SOH (Spherical Overdensity halo MF, Watson et al. 2012), Despali_Z0, Despali_AllZ, Despali_AllZAllCosmo, Despali_HighM (Despali et al. 2016)
method_SS	method used to compute the power spectrum and σ(mass); valid method_SS are: CAMB [http://camb.info/], CLASS [http://class-code.net/], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
Delta	\(\Delta\), the overdensity
interpType	method to interpolate the power spectrum
k_max	maximum wave vector module up to which the power spectrum is computed
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum

Returns: minimum halo mass

Warning: the input parameter \(\Delta\) is the background overdensity, not the critical overdensity \(\Delta_{crit}\); divide \(\Delta_{crit}\) by \(\Omega_M(z)\) (see cbl::cosmology::Cosmology::OmegaM) to obtain the background overdensity; the mass function by Manera et al. (2010) has been tested only for z=0 and z=0.5; the mass function by Despali et al. (2016) is currently implemented only for virial masses and at \(z<1.25\)

Definition at line 564 of file MassFunction.cpp.

◆ model()

std::string cbl::cosmology::Cosmology::model ( ) const

inline

get the private member Cosmology::m_model

Returns: the cosmologial model used to compute distances

Definition at line 1328 of file Cosmology.h.

◆ mrk()

double cbl::cosmology::Cosmology::mrk	(	const double	kk,
		const double	mass,
		const std::string	method_Pk,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const int	norm = `-1`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`,
		const std::string	file_par = `par::defaultString`
	)

auxiliary function to estimate cosmological quantities in non-Gaussian cosmologies

Author: Cosimo Fedeli; cosim.nosp@m.o.fe.nosp@m.deli@.nosp@m.oabo.nosp@m..inaf.nosp@m..it

Parameters

kk	wave vector module
mass	halo mass
method_Pk	method used to compute the power spectrum (i.e. the Boltzmann solver); valid choices for method_Pk are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	the output_root parameter of the parameter file used to compute the power spectrum; it can be any name. If this parameter is different from the default value it will be used also in the output directory name
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
prec	accuracy of the integration
file_par	name of the parameter file; if a parameter file is provided (i.e. file_par!=NULL), it will use be used, ignoring the cosmological parameters of the object

Returns: mrk

Definition at line 116 of file NG.cpp.

◆ n_haloes() [1/2]

double cbl::cosmology::Cosmology::n_haloes	(	const double	Mass_min,
		const double	Mass_max,
		const double	Volume,
		const double	redshift,
		const std::string	model_MF,
		const std::string	method_SS,
		const int	nbin_mass = `0`,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const double	Delta = `200.`,
		const std::string	interpType = `"Linear"`,
		const int	norm = `-1`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`,
		const bool	default_delta = `true`,
		const double	delta_t = `1.686`
	)

number of dark matter haloes per volume at fixed redshift

this function computes the number of dark matter haloes per volume at fixed redshift as follows:

\[ N_h = \int_{M_{min}}^{M_{max}} d M \Phi(M)\]

Author: Alfonso Veropalumbo, Jacopo Neri (and Federico Marulli); alfon.nosp@m.so.v.nosp@m.eropa.nosp@m.lumb.nosp@m.o@uni.nosp@m.bo.i.nosp@m.t, jacop.nosp@m.o.ne.nosp@m.ri6@g.nosp@m.mail.nosp@m..com (and feder.nosp@m.ico..nosp@m.marul.nosp@m.li3@.nosp@m.unibo.nosp@m..it)

Parameters

Mass_min	minimum mass
Mass_max	maximum mass
Volume	the volume
redshift	the redshift
model_MF	author(s) who proposed the mass function; valid authors are: PS (Press & Schechter), ST (Sheth & Tormen), Jenkins (Jenkins et al. 2001), Warren (Warren et al. 2006), ShenH (halo MF, Shen et al. 2006), ShenF (filament MF, Shen et al. 2006), ShenS (sheet MF, Shen et al. 2006), Pan (Pan 2007), Peacock (Peacock at al. 2007), Reed (Reed et al. 2007), Tinker (Tinker et al. 2008), Crocce (Crocce et al. 2010), Manera (Manera et al. 2010), Courtin (Courtin et al. 2010), Bhattacharya (Bhattacharya et al. 2011), Angulo_FOF (FoF MF, Angulo et al. 2012), Angulo_Sub (SUBFIND MF, Angulo et al. 2012), Watson_FOF (FoF MF, Watson et al. 2012), Watson_SOH (Spherical Overdensity halo MF, Watson et al. 2012), Despali_Z0, Despali_AllZ, Despali_AllZAllCosmo, Despali_HighM (Despali et al. 2016)
method_SS	method used to compute the power spectrum and σ(mass); valid method_SS are: CAMB [http://camb.info/], CLASS [http://class-code.net/], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
nbin_mass	number of bin for the mass function computation
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
Delta	\(\Delta\), the overdensity
interpType	method to interpolate the power spectrum
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed to estimate the power spectrum normalisation; this parameter is used only if norm=1
k_max	maximum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
prec	accuracy of the integration
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum
default_delta	true = using function cbl::cosmology::deltac; false = using delta_t*growth factor
delta_t	user defined density contrast at \(z = 0\)

Returns: the mass function, dΦ/dM=dn(M)/dM

Warning: the input parameter \(\Delta\) is the background overdensity, not the critical overdensity \(\Delta_{crit}\); divide \(\Delta_{crit}\) by \(\Omega_M(z)\) (see cbl::cosmology::Cosmology::OmegaM) to obtain the background overdensity; the mass function by Manera et al. (2010) has been tested only for z=0 and z=0.5; the mass function by Despali et al. (2016) is currently implemented only for virial masses and at \(z<1.25\)

Definition at line 514 of file MassFunction.cpp.

◆ n_haloes() [2/2]

double cbl::cosmology::Cosmology::n_haloes	(	const double	Mass_min,
		const double	Mass_max,
		const double	z_min,
		const double	z_max,
		const bool	angle_rad,
		const std::string	model_MF,
		const std::string	method_SS,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const double	Delta = `200`,
		const std::string	interpType = `"Linear"`,
		const double	k_max = `100.`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`
	)

number of dark matter haloes per steradian or square degree, for a given redshift range

Author: Alfonso Veropalumbo, Jacopo Neri (and Federico Marulli); alfon.nosp@m.so.v.nosp@m.eropa.nosp@m.lumb.nosp@m.o@uni.nosp@m.bo.i.nosp@m.t, jacop.nosp@m.o.ne.nosp@m.ri6@g.nosp@m.mail.nosp@m..com (and feder.nosp@m.ico..nosp@m.marul.nosp@m.li3@.nosp@m.unibo.nosp@m..it)

Parameters

Mass_min	minimum mass
Mass_max	maximum mass
z_min	minimum redshift
z_max	maximum redshift
angle_rad	0 \(\rightarrow\) Ω in square degrees; 1 \(\rightarrow\) Ω in steradians
model_MF	author(s) who proposed the mass function; valid authors are: PS (Press & Schechter), ST (Sheth & Tormen), Jenkins (Jenkins et al. 2001), Warren (Warren et al. 2006), ShenH (halo MF, Shen et al. 2006), ShenF (filament MF, Shen et al. 2006), ShenS (sheet MF, Shen et al. 2006), Pan (Pan 2007), Peacock (Peacock at al. 2007), Reed (Reed et al. 2007), Tinker (Tinker et al. 2008), Crocce (Crocce et al. 2010), Manera (Manera et al. 2010), Courtin (Courtin et al. 2010), Bhattacharya (Bhattacharya et al. 2011), Angulo_FOF (FoF MF, Angulo et al. 2012), Angulo_Sub (SUBFIND MF, Angulo et al. 2012), Watson_FOF (FoF MF, Watson et al. 2012), Watson_SOH (Spherical Overdensity halo MF, Watson et al. 2012), Despali_Z0, Despali_AllZ, Despali_AllZAllCosmo, Despali_HighM (Despali et al. 2016)
method_SS	method used to compute the power spectrum and σ(mass); valid method_SS are: CAMB [http://camb.info/], CLASS [http://class-code.net/], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
Delta	\(\Delta\), the overdensity
interpType	method to interpolate the power spectrum
k_max	maximum wave vector module up to which the power spectrum is computed
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum

Returns: n_haloes: the number density of dark matter haloes (per steradian or square degree)

Warning: the input parameter \(\Delta\) is the background overdensity, not the critical overdensity \(\Delta_{crit}\); divide \(\Delta_{crit}\) by \(\Omega_M(z)\) (see cbl::cosmology::Cosmology::OmegaM) to obtain the background overdensity; the mass function by Manera et al. (2010) has been tested only for z=0 and z=0.5; the mass function by Despali et al. (2016) is currently implemented only for virial masses and at \(z<1.25\)

Definition at line 469 of file MassFunction.cpp.

◆ n_haloes_selection_function()

double cbl::cosmology::Cosmology::n_haloes_selection_function	(	const double	Mass_min,
		const double	Mass_max,
		const double	z_min,
		const double	z_max,
		const bool	angle_rad,
		const std::string	model_MF,
		const std::string	method_SS,
		const std::string	selection_function_file,
		const std::vector< int >	column = `{}`,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const double	Delta = `200`,
		const bool	isDelta_critical = `false`,
		const std::string	interpType = `"Linear"`,
		const double	k_max = `100.`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`
	)

number of dark matter haloes per steradian or square degree, for a given redshift range and with selection function defined on a grid

Author: Alfonso Veropalumbo, Jacopo Neri (and Federico Marulli); alfon.nosp@m.so.v.nosp@m.eropa.nosp@m.lumb.nosp@m.o@uni.nosp@m.bo.i.nosp@m.t, jacop.nosp@m.o.ne.nosp@m.ri6@g.nosp@m.mail.nosp@m..com (and feder.nosp@m.ico..nosp@m.marul.nosp@m.li3@.nosp@m.unibo.nosp@m..it)

Parameters

Mass_min	minimum mass
Mass_max	maximum mass
z_min	minimum redshift
z_max	maximum redshift
angle_rad	0 \(\rightarrow\) Ω in square degrees; 1 \(\rightarrow\) Ω in steradians
model_MF	author(s) who proposed the mass function; valid authors are: PS (Press & Schechter), ST (Sheth & Tormen), Jenkins (Jenkins et al. 2001), Warren (Warren et al. 2006), ShenH (halo MF, Shen et al. 2006), ShenF (filament MF, Shen et al. 2006), ShenS (sheet MF, Shen et al. 2006), Pan (Pan 2007), Peacock (Peacock at al. 2007), Reed (Reed et al. 2007), Tinker (Tinker et al. 2008), Crocce (Crocce et al. 2010), Manera (Manera et al. 2010), Courtin (Courtin et al. 2010), Bhattacharya (Bhattacharya et al. 2011), Angulo_FOF (FoF MF, Angulo et al. 2012), Angulo_Sub (SUBFIND MF, Angulo et al. 2012), Watson_FOF (FoF MF, Watson et al. 2012), Watson_SOH (Spherical Overdensity halo MF, Watson et al. 2012), Despali_Z0, Despali_AllZ, Despali_AllZAllCosmo, Despali_HighM (Despali et al. 2016)
method_SS	method used to compute the power spectrum and σ(mass); valid method_SS are: CAMB [http://camb.info/], CLASS [http://class-code.net/], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
selection_function_file	input file where the selection function is stored
column	the columns to be read
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
Delta	\(\Delta\), the overdensity
isDelta_critical	\(\rightarrow\) \(\Delta\) is the overdensity defined with respect to the critical density
interpType	method to interpolate the power spectrum
k_max	maximum wave vector module up to which the power spectrum is computed
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum

Returns: n_haloes: the number density of dark matter haloes (per steradian or square degree)

Warning: the input parameter \(\Delta\) is the background overdensity, not the critical overdensity \(\Delta_{crit}\); divide \(\Delta_{crit}\) by \(\Omega_M(z)\) (see cbl::cosmology::Cosmology::OmegaM) to obtain the background overdensity; the mass function by Manera et al. (2010) has been tested only for z=0 and z=0.5; the mass function by Despali et al. (2016) is currently implemented only for virial masses and at \(z<1.25\)

Definition at line 592 of file MassFunction.cpp.

◆ n_spec()

double cbl::cosmology::Cosmology::n_spec ( ) const

inline

get the private member Cosmology::m_n_spec

Returns: n_spec: the primordial spectral index

Definition at line 1234 of file Cosmology.h.

◆ neutrino_mass()

double cbl::cosmology::Cosmology::neutrino_mass ( ) const

the total neutrino mass

this function computes the neutrino mass as follows:

\[\sum m_\nu = \Omega_\nu\cdot94\, h^2 eV\]

Returns: \(\sum m_\nu\)

Definition at line 652 of file Cosmology.cpp.

◆ Nvoids() [1/2]

std::vector< std::vector< double > > cbl::cosmology::Cosmology::Nvoids	(	const double	min_r,
		const double	max_r,
		const int	num_bins,
		const double	mean_z,
		const double	Volume,
		const std::string	model,
		const double	b_eff,
		double	slope = `0.854`,
		double	offset = `0.420`,
		const double	deltav_NL = `-0.795`,
		const double	del_c = `1.69`,
		const std::string	method_Pk = `"EisensteinHu"`,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const std::string	interpType = `"Linear"`,
		const double	k_max = `100.`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`
	)		const

number of voids computed from the void size function model for bins of radii spaced in log scale and for a specified survey/simulation volume

Author: Sofia Contarini; sofia.nosp@m..con.nosp@m.tarin.nosp@m.i3@u.nosp@m.nibo..nosp@m.it

Parameters

min_r	the minimum void radius
max_r	the maximum void radius
num_bins	number of bins of void radius
mean_z	the mean redshift of the sample
Volume	the volume of the survey/simulation in units of \((Mpc/h)^3\)
model	size function model name; valid choices for model name are SvdW (Sheth and van de Weygaert, 2004), linear and Vdn (Jennings et al., 2013)
b_eff	the effective bias of the sample
slope	first coefficent to convert the effective bias (default value set to \(0.854\))
offset	second coefficent to convert the effective bias (default value set to \(0.420\))
deltav_NL	the non linear density contrast: \(\rho_v/\rho_m\) (default value set to \(-0.795\))
del_c	critical value of the linear density field (default value set to \(1.06\))
method_Pk	method used to compute the power spectrum (i.e. the Boltzmann solver); valid choices for method_Pk are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
interpType	method to interpolate the power spectrum
k_max	maximum wave vector module up to which the power spectrum is computed
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum

Returns: a vector of vectors with dimensions 2xnum_bins. The first component contains the void radii (centres of the bins computed in log scale), while the second the predicted void counts

Definition at line 194 of file SizeFunction.cpp.

◆ Nvoids() [2/2]

std::vector< std::vector< double > > cbl::cosmology::Cosmology::Nvoids	(	const double	min_r,
		const double	max_r,
		const int	num_bins,
		const double	min_z,
		const double	max_z,
		const double	mean_z,
		const double	Area,
		const std::string	model,
		const double	b_eff,
		double	slope = `0.854`,
		double	offset = `0.420`,
		const double	deltav_NL = `-0.795`,
		const double	del_c = `1.69`,
		const std::string	method_Pk = `"EisensteinHu"`,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const std::string	interpType = `"Linear"`,
		const double	k_max = `100.`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`
	)		const

number of voids computed from the void size function model for bins of radii spaced in log scale. The considered volume is computed from a (fraction of) a sphere shell, included in between two different redshifts

Author: Sofia Contarini; sofia.nosp@m..con.nosp@m.tarin.nosp@m.i3@u.nosp@m.nibo..nosp@m.it

Parameters

min_r	the minimum void radius
max_r	the maximum void radius
num_bins	number of bins of void radius
min_z	the minimum redshift of the shell
max_z	the maximum redshift of the shell
mean_z	the mean redshift of the sample
Area	sky area in units of squares degrees
model	size function model name; valid choices for model name are SvdW (Sheth and van de Weygaert, 2004), linear and Vdn (Jennings et al., 2013)
b_eff	the effective bias of the sample
slope	first coefficent to convert the effective bias (default value set to \(0.854\))
offset	second coefficent to convert the effective bias (default value set to \(0.420\))
deltav_NL	the non linear density contrast: \(\rho_v/\rho_m\) (default value set to \(-0.795\))
del_c	critical value of the linear density field (default value set to \(1.06\))
method_Pk	method used to compute the power spectrum (i.e. the Boltzmann solver); valid choices for method_Pk are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
interpType	method to interpolate the power spectrum
k_max	maximum wave vector module up to which the power spectrum is computed
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum

Returns: a vector of vectors with dimensions 2xnum_bins. The first component contains the void radii (centres of the bins computed in log scale), while the second the predicted void counts

Definition at line 249 of file SizeFunction.cpp.

◆ Omega()

double cbl::cosmology::Cosmology::Omega ( const double redshift = 0. ) const

the cosmic density at a given redshift

Parameters

redshift the redshift

Returns: \(Omega\)

Definition at line 633 of file Cosmology.cpp.

◆ Omega_baryon()

double cbl::cosmology::Cosmology::Omega_baryon ( ) const

inline

get the private member Cosmology::m_Omega_baryon

Returns: Ω_b: the baryons density

Definition at line 1126 of file Cosmology.h.

◆ Omega_CDM()

double cbl::cosmology::Cosmology::Omega_CDM ( ) const

inline

get the private member Cosmology::m_Omega_CDM

Returns: Ω_CDM: the cold dark matter density

Definition at line 1177 of file Cosmology.h.

◆ Omega_DE()

double cbl::cosmology::Cosmology::Omega_DE ( ) const

inline

get the private member Cosmology::m_Omega_DE

Returns: Ω_DE: the dark energy density

Definition at line 1156 of file Cosmology.h.

◆ Omega_k()

double cbl::cosmology::Cosmology::Omega_k ( ) const

inline

get the private member Cosmology::m_Omega_k

Returns: Ω_k: the density of curvature energy

Definition at line 1170 of file Cosmology.h.

◆ Omega_matter()

double cbl::cosmology::Cosmology::Omega_matter ( ) const

inline

get the private member Cosmology::m_Omega_matter

Returns: Ω_M: the matter density, i.e. the density of baryons, cold dark matter, and massive neutrinos (in units of the critical density)

Examples: fit.cpp.

Definition at line 1119 of file Cosmology.h.

◆ Omega_neutrinos() [1/2]

double cbl::cosmology::Cosmology::Omega_neutrinos ( ) const

inline

get the private member Cosmology::m_Omega_neutrinos

Returns: Ω_ν: the density of massive neutrinos

Definition at line 1134 of file Cosmology.h.

◆ Omega_neutrinos() [2/2]

double cbl::cosmology::Cosmology::Omega_neutrinos ( const double Mnu ) const

the density of massive neutrinos, given the neutrino mass

this function computes the density of massive neutrinos as follows:

\[\Omega_\nu = \frac{\sum m_\nu}{93.8h^2 eV}\]

Parameters

Mnu	\(\sum m_\nu\) in eV

Returns: \(\Omega_nu\)

Definition at line 642 of file Cosmology.cpp.

◆ Omega_radiation()

double cbl::cosmology::Cosmology::Omega_radiation ( ) const

inline

get the private member Cosmology::m_Omega_radiation

Returns: Ω_rad: the radiation density

Definition at line 1163 of file Cosmology.h.

◆ OmegaDE()

double cbl::cosmology::Cosmology::OmegaDE ( const double redshift = 0. ) const

the dark energy density at a given redshift

Parameters

redshift the redshift

Returns: Ω_DE

Definition at line 588 of file Cosmology.cpp.

◆ OmegaK()

double cbl::cosmology::Cosmology::OmegaK ( const double redshift = 0. ) const

the density of curvature energy at a given redshift

Parameters

redshift the redshift

Returns: Ω_k

Definition at line 615 of file Cosmology.cpp.

◆ OmegaM()

double cbl::cosmology::Cosmology::OmegaM ( const double redshift = 0. ) const

the matter density at a given redshift

Parameters

redshift the redshift

Returns: Ω_M

Definition at line 579 of file Cosmology.cpp.

◆ OmegaNu()

double cbl::cosmology::Cosmology::OmegaNu ( const double redshift = 0. ) const

the neutrino density at a given redshift

Parameters

redshift the redshift

Returns: Ω_ν

Definition at line 624 of file Cosmology.cpp.

◆ OmegaR()

double cbl::cosmology::Cosmology::OmegaR ( const double redshift = 0. ) const

the radiation density at a given redshift

Parameters

redshift the redshift

Returns: Ω_rad

Definition at line 597 of file Cosmology.cpp.

◆ OmegaR_zeq()

double cbl::cosmology::Cosmology::OmegaR_zeq ( const double z_eq = 3395. ) const

the radiation density, as a function of the redshift of radiation-matter equality

Parameters

z_eq	the redshift of radiation-matter equality

Returns: Ω_rad

Definition at line 606 of file Cosmology.cpp.

◆ Pk0_CAMB()

double cbl::cosmology::Cosmology::Pk0_CAMB ( ) const

inline

get the private member Cosmology::m_Pk0_CAMB

Returns: the normalisation of the power spectrum for CAMB [http://camb.info/]

Definition at line 1306 of file Cosmology.h.

◆ Pk0_CLASS()

double cbl::cosmology::Cosmology::Pk0_CLASS ( ) const

inline

get the private member Cosmology::m_Pk0_CLASS

Returns: the normalisation of the power spectrum for CLASS [http://class-code.net/]

Definition at line 1321 of file Cosmology.h.

◆ Pk0_EH()

double cbl::cosmology::Cosmology::Pk0_EH ( ) const

inline

get the private member Cosmology::m_Pk0_EH

Returns: the normalisation of the power spectrum for Eisenstein & Hu [http://background.uchicago.edu/~whu/transfer/transferpage.html]

Definition at line 1298 of file Cosmology.h.

◆ Pk0_MPTbreeze()

double cbl::cosmology::Cosmology::Pk0_MPTbreeze ( ) const

inline

get the private member Cosmology::m_Pk0_MPTbreeze

Returns: the normalisation of the power spectrum for MPTbreeze [http://arxiv.org/abs/1207.1465]

Definition at line 1314 of file Cosmology.h.

◆ Pk_0()

void cbl::cosmology::Cosmology::Pk_0	(	const std::string	method_Pk,
		const double	redshift,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`,
		const std::string	file_par = `par::defaultString`
	)

normalisation of the power spectrum

this function sets the value of the private member m_Pk0_*, i.e. the normalisation of the power spectrum

Parameters

method_Pk	method used to compute the power spectrum (i.e. the Boltzmann solver); valid choices for method_Pk are: CAMB [http://camb.info/], CAMB_wrapper (running CAMB wrapper), CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
redshift	the redshift
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	the output_root parameter of the parameter file used to compute the power spectrum; it can be any name. If this parameter is different from the default value it will be used also in the output directory name
k_min	minimum wave vector module up to which the power spectrum is computed to estimate the power spectrum normalisation;
k_max	maximum wave vector module up to which the power spectrum is computed to estimate the power spectrum normalisation;
prec	accuracy of the integration
file_par	name of the parameter file; if a parameter file is provided (i.e. file_par!=NULL), it will be used, ignoring the cosmological parameters of the object

Definition at line 1251 of file PkXi.cpp.

◆ Pk_1loop()

double cbl::cosmology::Cosmology::Pk_1loop	(	const double	kk,
		const std::shared_ptr< cbl::glob::FuncGrid >	PkLin,
		const int	corrtype,
		const double	qmin,
		const double	qmax,
		const double	prec = `1.e-3`
	)

the one-loop power spectrum

this function computes the one-loop power spectrum corrections (Crocce et al. 2012, https://arxiv.org/pdf/1207.1465.pdf):

\[ P^{1loop}(k; f_1, f_2) = 4\pi\int_{q_{min}}^{q_{max}} \mathrm{d} q\, q^2P(q) \int_{-1}^{1} \mathrm{d} x\, f_1(kq, q, akq) \, f_2(kq, q, akq) \, P(kq) \]

where

\[ kq = \sqrt{k^2+q^2-2kqx} \]

\[ akq = \frac{kx-q}{kq} \]

and \(f_1\), \(f_2\) can be compute by either cbl::cosmology::Cosmology::F2 or cbl::cosmology::Cosmology::G2

Parameters

kk	the wavevector module
PkLin	linear power spectrum
corrtype	0 \(\rightarrow\) \(f_1=f_2=F_2\); 1 \(\rightarrow\) \(f_1=F_2\), \(f_2=G_2\); 2 \(\rightarrow\) \(f_1=f_2=G_2\)
qmin	minimum q value in the integration
qmax	maximum q value in the integration
prec	the integral precision

Returns: one-loop power spectrum

Definition at line 95 of file PkXiNonLinear.cpp.

◆ Pk_DeltaDelta() [1/2]

double cbl::cosmology::Cosmology::Pk_DeltaDelta	(	const double	kk,
		const std::shared_ptr< cbl::glob::FuncGrid >	Pk,
		const double	qmin,
		const double	qmax,
		const double	prec = `1.e-3`
	)

the real-space matter non-linear power spectrum \(P_{\delta\delta}(k)\), computed at 1-loop

this function computes the real-space non-linear matter power spectrum \(P_{\delta\delta}(k)\) at 1-loop, following the MPTbreeze scheme (Crocce et al. 2012, https://arxiv.org/pdf/1207.1465.pdf):

\[ P_{\delta\delta}(k) = \left(2\pi\right)^3\left(\exp(f(k)\right)^2 (P^{lin}(k)+P^{1loop}(k; F_2, F_2)) \]

where \(P^{lin}(k)\) is the linear power spectrum, \(f(k)\) is the second-order correction of the non-linear propagator computed by cbl::cosmology::Cosmology::f_k, and \(P^{1loop}\) is the one-loop power spectrum correction, computed by cbl::cosmology::Cosmology::Pk_1loop

Parameters

kk	the wavevector module
Pk	pointer to a FuncGrid object to interpolate the linear power spectrum
qmin	the lower integration limit
qmax	the upper integration limit
prec	the integral precision

Returns: \(P_{\delta\delta}(k)\)

Definition at line 133 of file PkXiNonLinear.cpp.

◆ Pk_DeltaDelta() [2/2]

std::vector< double > cbl::cosmology::Cosmology::Pk_DeltaDelta	(	const std::vector< double >	kk,
		const double	redshift,
		const std::string	method_Pk,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const int	norm = `-1`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`,
		const std::string	file_par = `par::defaultString`,
		const bool	unit1 = `false`
	)

the real-space matter non-linear power spectrum \(P_{\delta\delta}(k)\), computed at 1-loop

this function computes the real-space non-linear matter power spectrum \(P_{\delta\delta}(k)\) at 1-loop, following the MPTbreeze scheme (Crocce et al. 2012, https://arxiv.org/pdf/1207.1465.pdf):

\[ P_{\delta\delta}(k) = \left(2\pi\right)^3\left(\exp(f(k)\right)^2 (P^{lin}(k)+P^{1loop}(k; F_2, F_2)) \]

where \(P^{lin}(k)\) is the linear power spectrum, \(f(k)\) is the second-order correction of the non-linear propagator computed by cbl::cosmology::Cosmology::f_k, and \(P^{1loop}\) is the one-loop power spectrum correction, computed by cbl::cosmology::Cosmology::Pk_1loop

Parameters

kk	the wavevector module
redshift	the redshift
method_Pk	method used to compute the power spectrum (i.e. the Boltzmann solver); valid choices for method_Pk are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	the output_root parameter of the parameter file used to compute the power spectrum; it can be any name. If this parameter is different from the default value it will be used also in the output directory name
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
prec	accuracy of the integration
file_par	name of the parameter file; if a parameter file is provided (i.e. file_par!=NULL), it will use be used, ignoring the cosmological parameters of the object
unit1	true \(\rightarrow\) force cosmological units

Returns: \(P_{\delta\delta}(k)\)

Definition at line 162 of file PkXiNonLinear.cpp.

◆ Pk_DeltaDelta_fitting_function()

double cbl::cosmology::Cosmology::Pk_DeltaDelta_fitting_function	(	const double	kk,
		const std::string	method_Pk,
		const double	redshift,
		const std::string	author,
		const bool	store_output,
		const std::string	output_root,
		const int	norm,
		double	k_min,
		double	k_max,
		const double	prec,
		const std::string	file_par,
		const bool	unit1
	)

the non-linear dark matter power spectrum using fitting functions given by Bel et. al (2019)

the non-linear dark matter power spectrum, P_δδ, is computed using the fitting functions given by Bel et. al (2019) [https://arxiv.org/abs/1809.09338].

Author: J.E. Garcia-Farieta; joega.nosp@m.rcia.nosp@m.fa@un.nosp@m.al.e.nosp@m.du.co

Parameters

kk	the wave vector module
method_Pk	method used to compute the power spectrum (i.e. the Boltzmann solver); valid choices for method_Pk are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
redshift	the redshift
author	author(s) who proposed the fitting functions; valid authors are: Pezzotta (Pezzotta, et.al, 2017), Bel (Bel et.al., 2019)
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	the output_root parameter of the parameter file used to compute the power spectrum; it can be any name. If this parameter is different from the default value it will be used also in the output directory name
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
prec	accuracy of the integration
file_par	name of the parameter file; if a parameter file is provided (i.e. file_par!=NULL), it will be used, ignoring the cosmological parameters of the object
unit1	true \(\rightarrow\) force cosmological units

Returns: P_δδ: the non linear power spectrum using fitting functions

Definition at line 141 of file RSD.cpp.

◆ Pk_DeltaTheta() [1/2]

double cbl::cosmology::Cosmology::Pk_DeltaTheta	(	const double	kk,
		const std::shared_ptr< cbl::glob::FuncGrid >	Pk,
		const double	qmin,
		const double	qmax,
		const double	prec = `1.e-3`
	)

the real-space matter non-linear power spectrum \(P_{\delta\theta}(k)\), computed at 1-loop

this function computes the real-space non-linear matter power spectrum \(P_{\delta\delta}(k)\) at 1-loop, following the MPTbreeze scheme (Crocce et al. 2012, https://arxiv.org/pdf/1207.1465.pdf):

\[ P_{\delta\theta}(k) = \left(2\pi\right)^3\left(\exp(f(k)\right)^2 (P^{lin}(k)+P^{1loop}(k; F_2, G_2)) \]

where \(P^{lin}(k)\) is the linear power spectrum, \(f(k)\) is the second-order correction of the non-linear propagator computed by cbl::cosmology::Cosmology::f_k, and \(P^{1loop}\) is the one-loop power spectrum correction, computed by cbl::cosmology::Cosmology::Pk_1loop

Parameters

kk	the wavevector module
Pk	pointer to a FuncGrid object to interpolate the linear power spectrum
qmin	the lower integration limit
qmax	the upper integration limit
prec	the integral precision

Returns: \(P_{\delta\theta}(k)\)

Definition at line 143 of file PkXiNonLinear.cpp.

◆ Pk_DeltaTheta() [2/2]

std::vector< double > cbl::cosmology::Cosmology::Pk_DeltaTheta	(	const std::vector< double >	kk,
		const double	redshift,
		const std::string	method_Pk,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const int	norm = `-1`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`,
		const std::string	file_par = `par::defaultString`,
		const bool	unit1 = `false`
	)

the real-space matter non-linear power spectrum \(P_{\delta\theta}(k)\), computed at 1-loop

this function computes the real-space non-linear matter power spectrum \(P_{\delta\delta}(k)\) at 1-loop, following the MPTbreeze scheme (Crocce et al. 2012, https://arxiv.org/pdf/1207.1465.pdf):

\[ P_{\delta\theta}(k) = \left(2\pi\right)^3\left(\exp(f(k)\right)^2 (P^{lin}(k)+P^{1loop}(k; F_2, G_2)) \]

where \(P^{lin}(k)\) is the linear power spectrum, \(f(k)\) is the second-order correction of the non-linear propagator computed by cbl::cosmology::Cosmology::f_k, and \(P^{1loop}\) is the one-loop power spectrum correction, computed by cbl::cosmology::Cosmology::Pk_1loop

Parameters

kk	the wavevector module
redshift	the redshift
method_Pk	method used to compute the power spectrum (i.e. the Boltzmann solver); valid choices for method_Pk are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	the output_root parameter of the parameter file used to compute the power spectrum; it can be any name. If this parameter is different from the default value it will be used also in the output directory name
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
prec	accuracy of the integration
file_par	name of the parameter file; if a parameter file is provided (i.e. file_par!=NULL), it will use be used, ignoring the cosmological parameters of the object
unit1	true \(\rightarrow\) force cosmological units

Returns: \(P_{\delta\theta}(k)\)

Definition at line 183 of file PkXiNonLinear.cpp.

◆ Pk_DeltaTheta_fitting_function()

double cbl::cosmology::Cosmology::Pk_DeltaTheta_fitting_function	(	const double	kk,
		const std::string	method_Pk,
		const double	redshift,
		const std::string	author,
		const bool	store_output,
		const std::string	output_root,
		const bool	NL,
		const int	norm,
		double	k_min,
		double	k_max,
		const double	prec,
		const std::string	file_par,
		const bool	unit1
	)

the dark matter cross power spectrum

the dark matter cross power spectrum, P_δθ, is computed using the fitting functions given by Bel et. al (2019) [https://arxiv.org/abs/1809.09338].

\[ P_{\delta\theta} (k) = \left(P_{\delta\delta}(k)P_{\theta\theta}^{Lin}(k)\right)^{1/2}e^{-k/k_\delta-bk^6} \]

with \(b = 0.091 + 0.702*\sigma8^2\)

Author: J.E. Garcia-Farieta; joega.nosp@m.rcia.nosp@m.fa@un.nosp@m.al.e.nosp@m.du.co

Parameters

kk	the wave vector module
method_Pk	method used to compute the power spectrum (i.e. the Boltzmann solver); valid choices for method_Pk are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
redshift	the redshift
author	author(s) who proposed the fitting functions; valid authors are: Pezzotta (Pezzotta, et.al, 2017), Bel (Bel et.al., 2019)
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	the output_root parameter of the parameter file used to compute the power spectrum; it can be any name. If this parameter is different from the default value it will be used also in the output directory name
NL	0 \(\rightarrow\) linear power spectrum; 1 \(\rightarrow\) non-linear power spectrum
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
prec	accuracy of the integration
file_par	name of the parameter file; if a parameter file is provided (i.e. file_par!=NULL), it will be used, ignoring the cosmological parameters of the object
unit1	true \(\rightarrow\) force cosmological units

Returns: P_δθ: the cross power spectrum using fitting functions

Definition at line 154 of file RSD.cpp.

◆ Pk_eTNS_terms_1loop()

std::vector< std::vector< double > > cbl::cosmology::Cosmology::Pk_eTNS_terms_1loop	(	std::vector< double >	kk,
		const std::string	method,
		const double	redshift,
		const bool	store_output,
		const std::string	output_root,
		const int	norm,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`
	)

The expanded correction terms for the extended TNS model (eTNS)

the expanded correction terms for the eTNS model are computed at 1-loop using the Standard Perturbation Theory implemented in the CAMB-integrated version by Shun Saito. [http://www2.yukawa.kyoto-u.ac.jp/~atsushi.taruya/cpt_pack.html]. Details can be found in Saito et al. (2014) and Beutler et al. (2014) [https://arxiv.org/abs/1405.1447 and https://arxiv.org/abs/1312.4611v2].

\[ P(k, \mu) = D_{FoG}(k', \mu', f, \sigma_v)\left[P_{\mathrm{g}, \delta \delta}(k) +2 f \mu^{2} P_{\mathrm{g}, \delta \theta}(k)+f^{2} \mu^{4} P_{\theta \theta}(k) + b_{1}^{3} A(k, \mu, \beta)+b_{1}^{4} B(k, \mu, \beta)\right] \]

where

\[ P_{\mathrm{g}, \delta \delta}(k) = b_{1}^{2} P_{\delta \delta}(k)+2 b_{2} b_{1} P_{b 2, \delta}(k)+2 b_{s 2} b_{1} P_{b s 2, \delta}(k) \\ +2 b_{3 \mathrm{nl}} b_{1} \sigma_{3}^{2}(k) P_{\mathrm{m}}^{\mathrm{lin}}(k)+b_{2}^{2} P_{b 22}(k) \\ +2 b_{2} b_{s 2} P_{b 2 s 2}(k)+b_{s 2}^{2} P_{b s 22}(k)+N \]

\[ P_{\mathrm{g}, \delta \theta}(k) = b_{1} P_{\delta \theta}(k)+b_{2} P_{b 2, \theta}(k)+b_{s 2} P_{b s 2, \theta}(k) \\ +b_{3 \mathrm{nl}} \sigma_{3}^{2}(k) P_{\mathrm{m}}^{\mathrm{lin}}(k) \]

Author: J.E. Garcia-Farieta; joega.nosp@m.rcia.nosp@m.fa@un.nosp@m.al.e.nosp@m.du.co

Parameters

kk	the wave vector module
method	method used to compute the linear power spectrum; valid choices for method_Pk are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
redshift	the redshift
store_output	if true the output files created by CAMB are stored; if false the output files created by CAMB are removed
output_root	the output_root parameter of the parameter file used to compute the power spectrum; it can be any name. If this parameter is different from the default value it will be used also in the output directory name
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed
prec	accuracy of the integration

Returns: expanded terms of the eTNS model: Pdd, Pdv, Pvv, Pb2d, Pb2v, Pb22, Pbs2d, Pbs2v, Pb2s2, Pbs22, sigma32Pklin, Bb1, Bb2, Bbs2

Definition at line 573 of file PkXiNonLinear.cpp.

◆ Pk_matter() [1/2]

std::vector< double > cbl::cosmology::Cosmology::Pk_matter	(	const std::vector< double >	kk,
		const std::string	method_Pk,
		const bool	NL,
		const double	redshift,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const int	norm = `-1`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`,
		const std::string	file_par = `par::defaultString`,
		const bool	unit1 = `false`
	)

the dark matter power spectrum

this function provides the dark matter power spectrum; it can use either CAMB, CLASS, MPTbreeze or the analytic approximation by Eisenstein & Hu

Parameters

kk	vector of wave vector modules
method_Pk	method used to compute the power spectrum (i.e. the Boltzmann solver); valid choices for method_Pk are: CAMB [http://camb.info/], CAMB_wrapper (running CAMB wrapper), CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
NL	0 \(\rightarrow\) linear power spectrum; 1 \(\rightarrow\) non-linear power spectrum
redshift	the redshift
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	the output_root parameter of the parameter file used to compute the power spectrum; it can be any name. If this parameter is different from the default value it will be used also in the output directory name
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed to estimate the power spectrum normalisation; this parameter is used only if norm=1
prec	accuracy of the integration
file_par	name of the parameter file; if a parameter file is provided (i.e. file_par!=NULL), it will be used, ignoring the cosmological parameters of the object
unit1	true \(\rightarrow\) force cosmological units

Returns: the dark matter power spectrum

Examples: Pk_dynamical_DE.cpp.

Definition at line 1331 of file PkXi.cpp.

◆ Pk_matter() [2/2]

std::vector< std::vector< double > > cbl::cosmology::Cosmology::Pk_matter	(	const std::vector< double >	kk,
		const std::string	method_Pk,
		const bool	NL,
		const std::vector< double >	redshift,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const int	norm = `-1`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`,
		const std::string	file_par = `par::defaultString`,
		const bool	unit1 = `false`
	)

the dark matter power spectrum

this function provides the dark matter power spectrum; it can use either CAMB, CLASS, MPTbreeze or the analytic approximation by Eisenstein & Hu

Parameters

kk	vector of wave vector modules
method_Pk	method used to compute the power spectrum (i.e. the Boltzmann solver); valid choices for method_Pk are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
NL	0 \(\rightarrow\) linear power spectrum; 1 \(\rightarrow\) non-linear power spectrum
redshift	vector of redshifts
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	the output_root parameter of the parameter file used to compute the power spectrum; it can be any name. If this parameter is different from the default value it will be used also in the output directory name
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed to estimate the power spectrum normalisation; this parameter is used only if norm=1
prec	accuracy of the integration
file_par	name of the parameter file; if a parameter file is provided (i.e. file_par!=NULL), it will be used, ignoring the cosmological parameters of the object
unit1	true \(\rightarrow\) force cosmological units

Returns: the dark matter power spectrum

Definition at line 1405 of file PkXi.cpp.

◆ Pk_matter_DeWiggled()

vector< double > cbl::cosmology::Cosmology::Pk_matter_DeWiggled	(	const std::string	linear_method,
		const std::string	nowiggles_method,
		const std::vector< double >	kk,
		const double	redshift,
		const double	sigma_NL,
		const int	order = `4`,
		const int	nknots = `10`,
		const double	lambda = `0.25`,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const bool	norm = `1`,
		const double	prec = `1.e-4`
	)

the dark matter power spectrum, de-wiggled (see e.g. Anderson et al 2014)

this function provides the De-Wiggled dark matter power spectrum

Author: Alfonso Veropalumbo; alfon.nosp@m.so.v.nosp@m.eropa.nosp@m.lumb.nosp@m.o@uni.nosp@m.bo.i.nosp@m.t

Parameters

linear_method	method to obtain linear power spectrum
nowiggles_method	method to obtain power spectrum with no wiggles
kk	array containing the wave vector module
redshift	the redshift
sigma_NL	the non linear BAO damping
order	basis spline order. This is used only when method=="bspline"
nknots	number of knots This is used only when method=="bspline"
lambda	width of the gaussian filter This is used only when method=="gaussian_3d" or "gaussian_1d"
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
prec	accuracy of the integration

Returns: P;_DW(k): the De-Wiggled power spectrum of dark matter

Definition at line 2193 of file PkXi.cpp.

◆ Pk_matter_Linear()

vector< double > cbl::cosmology::Cosmology::Pk_matter_Linear	(	const std::string	method,
		const std::vector< double >	kk,
		const double	redshift,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const bool	norm = `1`,
		const double	prec = `1.e-4`
	)

the dark matter linear power spectrum.

This function provides the linear dark matter power spectrum. Valid choices are: CAMB [http://camb.info/], CLASS [http://class-code.net/]

Author: Alfonso Veropalumbo; alfon.nosp@m.so.v.nosp@m.eropa.nosp@m.lumb.nosp@m.o@uni.nosp@m.bo.i.nosp@m.t

Parameters

method	method to obtain power spectrum with no wiggles. It can be "CAMB" or "CLASS"
kk	array containing the wave vector module
redshift	the redshift
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name␓
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
prec	accuracy of the integration

Returns: P;_DW(k): the De-Wiggled power spectrum of dark matter

Definition at line 2178 of file PkXi.cpp.

◆ Pk_matter_NoWiggles()

vector< double > cbl::cosmology::Cosmology::Pk_matter_NoWiggles	(	const std::string	method,
		const std::vector< double >	kk,
		const double	redshift,
		const std::string	linear_method = `"CAMB"`,
		const int	order = `4`,
		const int	nknots = `10`,
		const double	lambda = `0.25`,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const bool	norm = `1`,
		const double	prec = `1.e-4`
	)

the dark matter power spectrum without BAO wiggles

This function provides the No Wiggles dark matter power spectrum. It can be computed with:

EisensteinHu approximate formulas [http://arxiv.org/abs/1207.1465]:
bspline interpolation (see cbl::cosmology::Cosmology::Pk_matter_NoWiggles_bspline).
gaussian 3d smoothing (see cbl::cosmology::Cosmology::Pk_matter_NoWiggles_gaussian_3d).
gaussian 1d smoothing (see cbl::cosmology::Cosmology::Pk_matter_NoWiggles_gaussian_1d).

Author: Alfonso Veropalumbo; alfon.nosp@m.so.v.nosp@m.eropa.nosp@m.lumb.nosp@m.o@uni.nosp@m.bo.i.nosp@m.t

Parameters

method	method to obtain power spectrum with no wiggles. It can be "EisensteinHu", "bspline" "gaussian_3d" or "gaussian_1d"
kk	array containing the wave vector module
redshift	the redshift
linear_method	method to compute the linear power spectrum. It can be "CAMB" or "CLASS" This is used only when method=="bspline"
order	basis spline order. This is used only when method=="bspline"
nknots	number of knots This is used only when method=="bspline"
lambda	width of the gaussian filter This is used only when method=="gaussian_3d" or "gaussian_1d"
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
prec	accuracy of the integration

Returns: P;_DW(k): the De-Wiggled power spectrum of dark matter

Definition at line 2141 of file PkXi.cpp.

◆ Pk_matter_NoWiggles_bspline()

vector< double > cbl::cosmology::Cosmology::Pk_matter_NoWiggles_bspline	(	const std::vector< double >	kk,
		const std::vector< double >	PkLin,
		const std::vector< double >	PkApprox,
		const int	order,
		const int	nknots
	)

the dark matter power spectrum without BAO wiggles.

This function provides the No Wiggles dark matter power spectrum. It follows the method proposed in Vlah et al. 2015 (https://arxiv.org/abs/1509.02120, Appendix A). The no wiggles power spectrum is obtained by interpolating the oscillatory part of the linear power spectrum with a basis spline of a given order and number of knots.

Author: Alfonso Veropalumbo; alfon.nosp@m.so.v.nosp@m.eropa.nosp@m.lumb.nosp@m.o@uni.nosp@m.bo.i.nosp@m.t

Parameters

kk	array containing the wave vector module
PkLin	array that contains the linear power spectrum
PkApprox	array that contains the approximated no-wiggle power spectrum
order	basis spline order
nknots	number of knots

Returns: P;_NW(k): the No-Wiggle par of the power spectrum of dark matter

Definition at line 2117 of file PkXi.cpp.

◆ Pk_matter_NoWiggles_gaussian()

vector< double > cbl::cosmology::Cosmology::Pk_matter_NoWiggles_gaussian	(	const std::vector< double >	kk,
		const std::vector< double >	PkLin,
		const std::vector< double >	PkApprox,
		const double	lambda,
		const std::string	method
	)

the dark matter power spectrum without BAO wiggles.

This function provides the No Wiggles dark matter power spectrum. It follows the method proposed in Vlah et al. 2015 (https://arxiv.org/abs/1509.02120, Appendix A). The no wiggles power spectrum is obtained by smoothing the oscillatory part of the linear power spectrum with gaussian filter.

It implements two methods:

Gaussian 3D:

\[ P_{\mathrm{nw}}(k) &=\int d^{3} q P(q) \mathcal{F}_{G}(|\mathbf{k}-\mathbf{q}|) \\ &=\frac{\sqrt{2}}{\sqrt{\pi} \lambda} \int d q q^{2} P(q) \exp \left(-\frac{1}{2 \lambda^{2}}\left(q^{2}+k^{2}\right)\right) \frac{\sinh \left(k q / \lambda^{2}\right)}{k q} \]
Gaussian 1D:

\[ P_{\mathrm{nw}}\left(10^{k_{\mathrm{log}}}\right)=\frac{1}{\sqrt{2 \pi} \lambda} \int d q_{\mathrm{log}} P\left(10^{q_{\mathrm{log}}}\right) \exp \left(-\frac{1}{2 \lambda^{2}}\left(k_{\mathrm{log}}-q_{\mathrm{log}}\right)^{2}\right) \]

Author: Alfonso Veropalumbo; alfon.nosp@m.so.v.nosp@m.eropa.nosp@m.lumb.nosp@m.o@uni.nosp@m.bo.i.nosp@m.t

Parameters

kk	array containing the wave vector module
PkLin	array that contains the linear power spectrum
PkApprox	array that contains the approximated no-wiggle power spectrum
lambda	size of the kernel
method	gaussian smoothing method; it can be "gaussian_1d" or "gaussian_3d"

Returns: P;_NW(k): the No-Wiggle par of the power spectrum of dark matter

Definition at line 2063 of file PkXi.cpp.

◆ Pk_output_file()

std::string cbl::cosmology::Cosmology::Pk_output_file	(	const std::string	code,
		const bool	NL,
		const double	redshift,
		const bool	run = `0`,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const double	k_max = `100.`,
		const std::string	file_par = `par::defaultString`
	)

return the path to the power spectrum output

Parameters

code	method used to compute the power spectrum
NL	0 \(\rightarrow\) linear power spectrum; 1 \(\rightarrow\) non-linear power spectrum
redshift	the redshift
run	true \(\rightarrow\) write or read the table where the dark matter power spectrum is stored
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	the output_root parameter of the parameter file used to compute the power spectrum; it can be any name. If this parameter is different from the default value it will be used also in the output directory name
k_max	the maximum wave vector module up to which the power spectrum is computed
file_par	name of the parameter file; if a parameter file is provided (i.e. file_par!=NULL), it will use be used, ignoring the cosmological parameters of the object

Returns: the path to the power spectrum output

Definition at line 71 of file PkXi.cpp.

◆ Pk_ThetaTheta() [1/2]

double cbl::cosmology::Cosmology::Pk_ThetaTheta	(	const double	kk,
		const std::shared_ptr< cbl::glob::FuncGrid >	Pk,
		const double	qmin,
		const double	qmax,
		const double	prec = `1.e-3`
	)

the real-space matter non-linear power spectrum \(P_{\theta\theta}(k)\), computed at 1-loop

this function computes the real-space non-linear matter power spectrum \(P_{\delta\delta}(k)\) at 1-loop, following the MPTbreeze scheme (Crocce et al. 2012, https://arxiv.org/pdf/1207.1465.pdf):

\[ P_{\theta\theta} (k) = \left(\exp(g(k)\right)^2 (P^{lin}(k)+P^{1loop}(k; G_2, G_2)) \]

where \(P^{lin}(k)\) is the linear power spectrum, \(f(k)\) is the second-order correction of the non-linear propagator computed by cbl::cosmology::Cosmology::g_k, and \(P^{1loop}\) is the one-loop power spectrum correction, computed by cbl::cosmology::Cosmology::Pk_1loop

Parameters

kk	the wavevector module
Pk	pointer to a FuncGrid object to interpolate the linear power spectrum
qmin	the lower integration limit
qmax	the upper integration limit
prec	the integral precision

Returns: \(P_{\theta\theta}(k)\)

Definition at line 153 of file PkXiNonLinear.cpp.

◆ Pk_ThetaTheta() [2/2]

std::vector< double > cbl::cosmology::Cosmology::Pk_ThetaTheta	(	const std::vector< double >	kk,
		const double	redshift,
		const std::string	method_Pk,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const int	norm = `-1`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`,
		const std::string	file_par = `par::defaultString`,
		const bool	unit1 = `false`
	)

the real-space matter non-linear power spectrum \(P_{\theta\theta}(k)\), computed at 1-loop

this function computes the real-space non-linear matter power spectrum \(P_{\delta\delta}(k)\) at 1-loop, following the MPTbreeze scheme (Crocce et al. 2012, https://arxiv.org/pdf/1207.1465.pdf):

\[ P_{\theta \theta}(k) = \left(2\pi\right)^3\left(\exp(g(k)\right)^2 (P^{lin}(k)+P^{1loop}(k; G_2, G_2)) \]

where \(P^{lin}(k)\) is the linear power spectrum, \(g(k)\) is the second-order correction of the non-linear propagator computed by cbl::cosmology::Cosmology::g_k, and \(P^{1loop}\) is the one-loop power spectrum correction, computed by cbl::cosmology::Cosmology::Pk_1loop

Parameters

kk	vector of wavevector modules
redshift	the redshift
method_Pk	method used to compute the power spectrum (i.e. the Boltzmann solver); valid choices for method_Pk are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	the output_root parameter of the parameter file used to compute the power spectrum; it can be any name. If this parameter is different from the default value it will be used also in the output directory name
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
prec	accuracy of the integration
file_par	name of the parameter file; if a parameter file is provided (i.e. file_par!=NULL), it will use be used, ignoring the cosmological parameters of the object
unit1	true \(\rightarrow\) force cosmological units

Returns: \(P_{\theta\theta}(k)\)

Definition at line 203 of file PkXiNonLinear.cpp.

◆ Pk_ThetaTheta_fitting_function()

double cbl::cosmology::Cosmology::Pk_ThetaTheta_fitting_function	(	const double	kk,
		const std::string	method_Pk,
		const double	redshift,
		const std::string	author,
		const bool	store_output,
		const std::string	output_root,
		const bool	NL,
		const int	norm,
		double	k_min,
		double	k_max,
		const double	prec,
		const std::string	file_par,
		const bool	unit1
	)

the dark matter velocity divergence power spectrum

the dark matter velocity divergence power spectrum, P_θθ, is computed using the fitting functions given by Bel et. al (2019) [https://arxiv.org/abs/1809.09338].

\[ P_{\theta\theta}(k) = P^{Lin}_{\theta\theta}(k)e^{-k(a_1+a_2k+a_3k^2)} \]

with

\[a_1 = -0.817 + 3.198*\sigma_8\]

\[a_2 = 0.877 - 4.191*\sigma_8\]

\[a_3 = -1.199 + 4.629*\sigma_8\]

Author: J.E. Garcia-Farieta; joega.nosp@m.rcia.nosp@m.fa@un.nosp@m.al.e.nosp@m.du.co

Parameters

kk	the wave vector module
method_Pk	method used to compute the power spectrum (i.e. the Boltzmann solver); valid choices for method_Pk are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
redshift	the redshift
author	author(s) who proposed the fitting functions; valid authors are: Pezzotta (Pezzotta, et.al, 2017), Bel (Bel et.al., 2019)
store_output	if true the output files created by CAMB are stored; if false the output files created by CAMB are removed
output_root	the output_root parameter of the parameter file used to compute the power spectrum; it can be any name. If this parameter is different from the default value it will be used also in the output directory name
NL	false \(\rightarrow\) linear power spectrum; true \(\rightarrow\) non-linear power spectrum
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
prec	accuracy of the integration
file_par	name of the parameter file; if a parameter file is provided (i.e. file_par!=NULL), it will be used, ignoring the cosmological parameters of the object
unit1	true \(\rightarrow\) force cosmological units

Returns: P_θθ: the velocity divergence power spectrum using fitting functions

Definition at line 174 of file RSD.cpp.

◆ Pk_TNS_AB_1loop() [1/2]

std::vector< std::vector< double > > cbl::cosmology::Cosmology::Pk_TNS_AB_1loop	(	std::vector< double >	kk,
		const double	mu,
		const double	linear_growth_rate,
		const double	bias,
		const std::string	method,
		const double	redshift,
		const bool	store_output,
		const std::string	output_root,
		const int	norm,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`
	)

the expanded A and B correction terms for the TNS model

the expanded A and B correction terms are computed at 1-loop using (Standard) Perturbation Theory implemented in the CPT Library [http://www2.yukawa.kyoto-u.ac.jp/~atsushi.taruya/cpt_pack.html]. Details can be found in (Taruya et.al, 2010) [https://arxiv.org/abs/1006.0699].

\[ A(k,\mu,\beta) = \beta\mu^2A_{11} + \beta^2(\mu^2A_{12} + \mu^4A_{22}) + \beta^3(\mu^4A_{23} + \mu^6A_{33}) \]

\[ B(k,\mu,\beta) = \mu^2(\beta^2B_{12} + \beta^3B_{13} + \beta^4B_{14}) + \mu^4(\beta^2B_{22} + \beta^3B_{23} + \beta^4B_{24}) + \mu^6(\beta^3B_{33} + \beta^4B_{34}) + \mu^8\beta^4B_{44} \]

Author: J.E. Garcia-Farieta; joega.nosp@m.rcia.nosp@m.fa@un.nosp@m.al.e.nosp@m.du.co

Parameters

kk	the wave vector module
mu	the cosine of the angle between the separation and the line of sight
linear_growth_rate	the linear growth rate
bias	the bias
method	method used to compute the power spectrum; valid choices for method_Pk are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
redshift	the redshift
store_output	if true the output files created by CAMB are stored; if false the output files created by CAMB are removed
output_root	the output_root parameter of the parameter file used to compute the power spectrum; it can be any name. If this parameter is different from the default value it will be used also in the output directory name
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
prec	accuracy of the integration

Returns: A and B terms (total contribution) for TNS model

Definition at line 460 of file PkXiNonLinear.cpp.

◆ Pk_TNS_AB_1loop() [2/2]

std::vector< std::vector< double > > cbl::cosmology::Cosmology::Pk_TNS_AB_1loop	(	std::vector< double >	kk,
		const double	mu,
		const std::string	method,
		const double	redshift,
		const bool	store_output,
		const std::string	output_root,
		const int	norm,
		const double	k_min,
		const double	k_max,
		const double	prec
	)

the A and B correction terms for the TNS model at 1-loop from the multipole expansion

the A and B correction terms for the TNS model at 1-loop from the multipole expansion are computed using the Standard Perturbation Theory implemented in the CPT Library [http://www2.yukawa.kyoto-u.ac.jp/~atsushi.taruya/cpt_pack.html]. Details can be found in Taruya et al. (2010) [https://arxiv.org/abs/1006.0699].

\[ A(k,\mu) = A_0(k)L_0(\mu) + A_2(k)L_2(\mu) + A_4(k)L_4(\mu) \]

\[ B(k,\mu) = B_0(k)L_0(\mu) + B_2(k)L_2(\mu) + B_4(k)L_4(\mu) \]

where \(L_l\) represents the Legendre polynomial of order \(l\).

Author: J.E. Garcia-Farieta; joega.nosp@m.rcia.nosp@m.fa@un.nosp@m.al.e.nosp@m.du.co

Parameters

kk	the wave vector module
mu	the cosine of the angle between the separation and the line of sight
method	method used to compute the power spectrum; valid choices for method_Pk are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
redshift	the redshift
store_output	if true the output files created by CAMB are stored; if false the output files created by CAMB are removed
output_root	the output_root parameter of the parameter file used to compute the power spectrum; it can be any name. If this parameter is different from the default value it will be used also in the output directory name
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed
prec	accuracy of the integration

Returns: A and B terms (total contribution) from multipoles

Definition at line 305 of file PkXiNonLinear.cpp.

◆ Pk_TNS_AB_multipoles()

std::vector< std::vector< double > > cbl::cosmology::Cosmology::Pk_TNS_AB_multipoles	(	std::vector< double >	kk,
		const std::string	method,
		const double	redshift,
		const bool	store_output,
		const std::string	output_root,
		const int	norm,
		const double	k_min,
		const double	k_max,
		const double	prec
	)

the multipoles of the A and B correction terms for the TNS model

the multipoles of the A and B correction terms for the TNS model are computed at 1-loop using the Standard Perturbation Theory implemented in the CPT Library [http://www2.yukawa.kyoto-u.ac.jp/~atsushi.taruya/cpt_pack.html]. Details can be found in Taruya et al. (2010) [https://arxiv.org/abs/1006.0699].

\[ A(k,\mu) = A_0(k)L_0(\mu) + A_2(k)L_2(\mu) + A_4(k)L_4(\mu) \]

\[ B(k,\mu) = B_0(k)L_0(\mu) + B_2(k)L_2(\mu) + B_4(k)L_4(\mu) \]

where \(L_l\) represents the Legendre polynomial of order \(l\).

Author: J.E. Garcia-Farieta; joega.nosp@m.rcia.nosp@m.fa@un.nosp@m.al.e.nosp@m.du.co

Parameters

kk	the wave vector module
method	method used to compute the power spectrum; valid choices for method_Pk are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
redshift	the redshift
store_output	if true the output files created by CAMB are stored; if false the output files created by CAMB are removed
output_root	the output_root parameter of the parameter file used to compute the power spectrum; it can be any name. If this parameter is different from the default value it will be used also in the output directory name
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
prec	accuracy of the integration

Returns: multipoles of A and B terms for TNS model (A0, A2, A4, B0, B2, B4)

Definition at line 224 of file PkXiNonLinear.cpp.

◆ Pk_TNS_AB_terms_1loop()

std::vector< std::vector< double > > cbl::cosmology::Cosmology::Pk_TNS_AB_terms_1loop	(	std::vector< double >	kk,
		const std::string	method,
		const double	redshift,
		const bool	store_output,
		const std::string	output_root,
		const int	norm,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`
	)

the expanded A and B correction terms for the TNS model

the expanded A and B correction terms for the TNS model are computed at 1-loop using the Standard Perturbation Theory implemented in the CPT Library [http://www2.yukawa.kyoto-u.ac.jp/~atsushi.taruya/cpt_pack.html]. Details can be found in Taruya et al. (2010) [https://arxiv.org/abs/1006.0699].

\[ A(k,\mu,\beta) = \beta\mu^2A_{11} + \beta^2(\mu^2A_{12} + \mu^4A_{22}) + \beta^3(\mu^4A_{23} + \mu^6A_{33}) \]

\[ B(k,\mu,\beta) = \mu^2(\beta^2B_{12} + \beta^3B_{13} + \beta^4B_{14}) + \mu^4(\beta^2B_{22} + \beta^3B_{23} + \beta^4B_{24}) + \mu^6(\beta^3B_{33} + \beta^4B_{34}) + \mu^8\beta^4B_{44} \]

Author: J.E. Garcia-Farieta; joega.nosp@m.rcia.nosp@m.fa@un.nosp@m.al.e.nosp@m.du.co

Parameters

kk	the wave vector module
method	method used to compute the power spectrum; valid choices for method_Pk are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
redshift	the redshift
store_output	if true the output files created by CAMB are stored; if false the output files created by CAMB are removed
output_root	the output_root parameter of the parameter file used to compute the power spectrum; it can be any name. If this parameter is different from the default value it will be used also in the output directory name
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed
prec	accuracy of the integration

Returns: A and B terms (expanded) for TNS model: A11, A12, A22, A23, A33, B12, B13, B14, B22, B23, B24, B33, B34, B44

Definition at line 322 of file PkXiNonLinear.cpp.

◆ Pk_TNS_dd_dt_tt()

std::vector< std::vector< double > > cbl::cosmology::Cosmology::Pk_TNS_dd_dt_tt	(	std::vector< double >	kk,
		const std::string	method,
		const double	redshift,
		const bool	store_output,
		const std::string	output_root,
		const int	norm,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`
	)

the non-linear \(\delta-\delta\), \(\delta-\theta\), \(\theta-\theta\) matter power spectra

the non-linear \(\delta-\delta\), \(\delta-\theta\), \(\theta-\theta\) matter power spectra are computed at 1-loop using (Standard) Perturbation Theory as implemented in the CPT Library [http://www2.yukawa.kyoto-u.ac.jp/~atsushi.taruya/cpt_pack.html]. Details can be found in Taruya et al. (2010) [https://arxiv.org/abs/1006.0699]. The density, density-velocity divergence and velocity divergence-velocity divergence power spectra are defined as:

\[ < \delta(k)\delta(k')> = (2\pi)^3\delta(k + k')P_{\delta\delta}(k) \]

\[ < \delta(k)\theta(k')> = (2\pi)^3\delta(k + k')P_{\delta\theta}(k) \]

\[ < \theta(k)\theta(k')> = (2\pi)^3\delta(k + k')P_{\theta\theta}(k) \]

Author: J.E. Garcia-Farieta; joega.nosp@m.rcia.nosp@m.fa@un.nosp@m.al.e.nosp@m.du.co

Parameters

kk	the wave vector module
method	method used to compute the power spectrum; valid choices for method_Pk are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
redshift	the redshift
store_output	if true the output files created by CAMB are stored; if false the output files created by CAMB are removed
output_root	the output_root parameter of the parameter file used to compute the power spectrum; it can be any name. If this parameter is different from the default value it will be used also in the output directory name
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed
prec	accuracy of the integration

Returns: a vector of vectors containing \(\left[P_{\delta\delta}(k), P_{\delta\theta}(k), P_{\theta\theta}(k)\right]\)

Definition at line 479 of file PkXiNonLinear.cpp.

◆ potential_spectral_amplitude()

double cbl::cosmology::Cosmology::potential_spectral_amplitude	(	const std::string	method_Pk,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const int	norm = `-1`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`,
		const std::string	file_par = `par::defaultString`
	)

the potential spectral amplitude

Author: Cosimo Fedeli; cosim.nosp@m.o.fe.nosp@m.deli@.nosp@m.oabo.nosp@m..inaf.nosp@m..it

Parameters

method_Pk	method used to compute the power spectrum (i.e. the Boltzmann solver); valid choices for method_Pk are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	the output_root parameter of the parameter file used to compute the power spectrum; it can be any name. If this parameter is different from the default value it will be used also in the output directory name
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
prec	accuracy of the integration
file_par	name of the parameter file; if a parameter file is provided (i.e. file_par!=NULL), it will use be used, ignoring the cosmological parameters of the object

Returns: the potential spectral amplitude

Definition at line 59 of file NG.cpp.

◆ pw()

double cbl::cosmology::Cosmology::pw	(	const double	ww,
		const double	ff,
		const std::string	author
	)		const

differential distribution

this function provides the differential rescaled and generalized formation redshift distribution

Author: Carlo Giocoli; cgioc.nosp@m.oli@.nosp@m.gmail.nosp@m..com

Parameters

ww	rescaled variable w as in Lacey and Coles 1993
ff	assembled fraction
author	valid authors are: NS (Nusser and Sheth), GTS (Giocoli et al. 2012)

Returns: p(w): differential distribution

Definition at line 51 of file MassGrowth.cpp.

◆ pz()

double cbl::cosmology::Cosmology::pz	(	const double	m0,
		const double	z0,
		const double	frac,
		const double	redshift,
		const std::string	model_model,
		const std::string	method_SS,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`
	)		const

formation probability

this function provides the probability that a halo of a given mass m0 at redshift z0 make a mass fraction f at redshift z

Author: Carlo Giocoli; cgioc.nosp@m.oli@.nosp@m.gmail.nosp@m..com

Parameters

m0	halo mass
z0	redshift when the halo has a mass m0
frac	mass fraction
redshift	the redshift
model_model	valid authors are: NS (Nusser and Sheth), GTS (Giocoli et al. 2012)
method_SS	method used to compute the power spectrum and σ(mass); valid method_SS are: CAMB [http://camb.info/], CLASS [http://class-code.net/], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name

Returns: p(z): formation probability

Definition at line 71 of file MassGrowth.cpp.

◆ Q_DM()

std::vector< double > cbl::cosmology::Cosmology::Q_DM	(	const double	r1,
		const double	r2,
		const std::vector< double >	theta,
		const std::string	model,
		const std::vector< double >	kk,
		const std::vector< double >	Pk_matter
	)		const

the dark matter reduced three-point correlation function

this function computes the dark matter reduced three-point reduced correlation function with either the Slepian et al. 2015 or the Barriga & Gatzagnaga 2002 model

Parameters

r1	the first side of the triangle
r2	the second side of the triangle
theta	vector containing angles between r1 and r2, in radians
model	the model to compute the three-point correlation function, can be "Slepian" or "BarrigaGatzanaga"
kk	vector of the wave vector modules
Pk_matter	the dark matter power spectrum

Returns: vector containing the dark matter reduced three-point correlation function

Definition at line 471 of file 3PCF.cpp.

◆ Q_DM_BarrigaGatzanaga()

double cbl::cosmology::Cosmology::Q_DM_BarrigaGatzanaga	(	const double	r1,
		const double	r2,
		const double	theta,
		std::vector< double > &	rr,
		std::vector< double > &	xi_matter,
		std::vector< double > &	Phi,
		const std::vector< double >	kk,
		const std::vector< double >	Pk_matter
	)		const

the dark matter reduced three-point correlation function model by Barriga & Gatzanaga et al. 2002

this functions computes \(Q_{DM} (r_1, r_2, \hat{r_1} \cdot \hat{r_2})\), as described in Barriga & Gatzanaga et al. 2002:

\[ Q_{DM} (r_1, r_2, \hat{r_1} \cdot \hat{r_2}) = \frac{\zeta_{DM} (r_1, r_2, \hat{r_1} \cdot \hat{r_2})} {\left( \xi(r_1)\xi(r_2)+\xi(r_2)\xi(r_3)+\xi(r_3)\xi(r_1)\right)} \]

see cbl::cosmology::Cosmology::zeta_DM_BarrigaGatzanaga for more details

Parameters

[in]	r1	the first side of the triangle
[in]	r2	the second side of the triangle
[in]	theta	the angle between r1 and r2
[out]	rr	vector or scales
[out]	xi_matter	vector containing the dark matter two-point correlation function
[out]	Phi	vector containing \( \Phi(r)\)
[in]	kk	vector of the wave vector modules
[in]	Pk_matter	the dark matter power spectrum

Returns: the dark matter reduced three-point correlation function

Definition at line 437 of file 3PCF.cpp.

◆ Q_DM_eq()

std::vector< double > cbl::cosmology::Cosmology::Q_DM_eq	(	const std::vector< double >	rr,
		const std::string	model,
		const std::vector< double >	kk,
		const std::vector< double >	Pk_matter
	)		const

the dark matter equilateral reduced three-point correlation function

this function computes the dark matter equilateral reduced three-point correlation function with either the Slepian et al 2015 or the Barriga & Gatzagnaga 2002 model

Parameters

rr	vector of sides
model	the model to compute the three-point correlation function, can be "Slepian" or "BarrigaGatzanaga"
kk	vector of the wave vector modules
Pk_matter	the dark matter power spectrum

Returns: vector containing the dark matter three-point correlation function

Definition at line 586 of file 3PCF.cpp.

◆ Q_DM_Slepian()

double cbl::cosmology::Cosmology::Q_DM_Slepian	(	const double	r1,
		const double	r2,
		const double	theta,
		std::vector< double > &	rr,
		std::vector< double > &	xi_matter,
		std::vector< double > &	xi_matter_m1,
		std::vector< double > &	xi_matter_p1,
		std::vector< double > &	xi_matter_2,
		const std::vector< double >	kk,
		const std::vector< double >	Pk_matter,
		const int	norders = `9`,
		const double	prec = `1.e-3`
	)		const

the dark matter reduced three-point correlation function model by Slepian et al. 2015

this function computes \(Q_{DM} (r_1, r_2, \hat{r_1} \cdot \hat{r_2})\) as described in Slepian et al. 2015:

\[ Q_{DM} (r_1, r_2, \hat{r_1} \cdot \hat{r_2}) = \frac{\zeta_{DM} (r_1, r_2, \hat{r_1} \cdot \hat{r_2})} {\left( \xi(r_1)\xi(r_2)+\xi(r_2)\xi(r_3)+\xi(r_3)\xi(r_1)\right)} \]

see cbl::cosmology::Cosmology::zeta_DM_Slepian for more details

Parameters

[in]	r1	the first side of the triangle
[in]	r2	the second side of the triangle
[in]	theta	the angle between r1 and r2
[out]	rr	vector or scales
[out]	xi_matter	vector containing the dark matter two-point orrelation function
[out]	xi_matter_m1	vector containing \(\xi^{[1-]}_{DM}(r)\)
[out]	xi_matter_p1	vector containing \(\xi^{[1+]}_{DM}(r)\)
[out]	xi_matter_2	vector containing \(\xi^{[2]}_{DM}(r)\)
[out]	kk	vector of the wave vector modules
[out]	Pk_matter	the dark matter power spectrum
[in]	norders	the maximum numbers of orders
[in]	prec	the integral precision

Returns: the dark matter reduced three-point correlation function

Definition at line 335 of file 3PCF.cpp.

◆ Q_halo() [1/2]

std::vector< double > cbl::cosmology::Cosmology::Q_halo	(	const double	r1,
		const double	r2,
		const std::vector< double >	theta,
		const double	b1,
		const double	b2,
		const double	g2,
		const std::string	model,
		const std::vector< double >	kk,
		const std::vector< double >	Pk_matter
	)		const

the non-local-bias model of the three-point correlation function of dark matter haloes

this function computes the reduced three-point correlation function of dark matter haloes, with non-local bias corrections, with either the Slepian et al. 2015 or the Barriga & Gatzagnaga 2002 model, as follows:

\[ Q_h (r_1, r_2, \hat{r_1} \cdot \hat{r_2}) = \frac{Q_{DM}(r_1, r_2, \hat{r_1} \cdot \hat{r_2})}{b_1}+ \frac{b_2}{b_1^2}+\frac{g_2}{b_1}Q_{non-local} \]

\(Q_{DM}\) is compute by cbl::cosmology::Cosmology::Q_DM and \(Q_{non-local}\) is the non-local contirbuion term, computed by cbl::cosmology::Cosmology::Q_nonLocal

Parameters

r1	the first side of the triangle
r2	the second side of the triangle
theta	vector containing angles between r1 and r2, in radians
b1	the linear bias
b2	the non-linear bias
g2	the non-local bias
model	the model to compute the three-point correlation function, can be "Slepian" or "BarrigaGatzanaga"
kk	vector of the wave vector modules
Pk_matter	the dark matter power spectrum

Returns: vector containing the reduced three-point correlation function of dark matter haloes

Definition at line 542 of file 3PCF.cpp.

◆ Q_halo() [2/2]

std::vector< double > cbl::cosmology::Cosmology::Q_halo	(	const double	r1,
		const double	r2,
		const std::vector< double >	theta,
		const double	b1,
		const double	b2,
		const std::string	model,
		const std::vector< double >	kk,
		const std::vector< double >	Pk_matter
	)		const

the local-bias model of the reduced three-point correlation function of dark matter haloes

this function computes the reduced three-point correlation function of dark matter haloes with either the Slepian et al. 2015 or the Barriga & Gatzagnaga 2002 model, as follows:

\[ Q_h (r_1, r_2, \hat{r_1} \cdot \hat{r_2}) = \frac{Q_{DM}(r_1, r_2, \hat{r_1} \cdot \hat{r_2})}{b_1}+\frac{b_2}{b_1^2}\]

\(Q_{DM}\) is compute by cbl::cosmology::Cosmology::Q_DM

Parameters

r1	the first side of the triangle
r2	the second side of the triangle
theta	vector containing angles between r1 and r2, in radians
b1	the linear bias
b2	the non-linear bias
model	the model to compute the three-point correlation function, can be "Slepian" or "BarrigaGatzanaga"
kk	vector of the wave vector modules
Pk_matter	the dark matter power spectrum

Returns: vector containing the reduced three-point correlation function of dark matter haloes

Definition at line 526 of file 3PCF.cpp.

◆ Q_nonLocal() [1/2]

double cbl::cosmology::Cosmology::Q_nonLocal	(	const double	r1,
		const double	r2,
		const double	theta,
		std::vector< double > &	rr,
		std::vector< double > &	xi_matter,
		std::vector< double > &	Phi,
		const std::vector< double >	kk,
		const std::vector< double >	Pk_matter
	)		const

the non-local contribution to the reduced dark matter three-point correlation function

this function computes the non-local contribution to three-point correlation function; specifically, it implements Eq. 22 of Bel el et al. 2015, MNRAS, 453, 259:

\[ Q_{non-local}(r_1, r_2, \theta) = \frac{2}{3} \left( \frac{\Gamma_{123} + \Gamma_{312} + \Gamma_{231}} {\xi(r_1)\cdot\xi(r_2) + \xi(r_2)\cdot\xi(r_3) + \xi(r_3)\cdot\xi(r_1)}-1 \right) \]

where the prime indicates the derivative with respect to \(r\), and \(\xi(r), \Phi(r)\) are the integrals of the power spectrum computed by cbl::cosmology::Cosmology::integrals_Q_nonLocal

Parameters

[in]	r1	the first side of the triangle
[in]	r2	the second side of the triangle
[in]	theta	the angle betwee r1 and r2
[out]	rr	vector or scales at which the dark matter two-point correlation function is computed
[out]	xi_matter	vector containing the dark matter two-point correlation function values
[out]	Phi	vector containing the \( \Phi(r)\) values, estimated at the scales given in rr
[in]	kk	vector of the wave vector modules at which the power spectrum is computed
[in]	Pk_matter	vector of containing the dark matter power spectrum values, estimated at the wave vector modules given in kk

Returns: the value of non-local Q

Definition at line 99 of file 3PCF.cpp.

◆ Q_nonLocal() [2/2]

std::vector< double > cbl::cosmology::Cosmology::Q_nonLocal	(	const double	r1,
		const double	r2,
		const std::vector< double >	theta,
		const std::vector< double >	kk,
		const std::vector< double >	Pk_matter
	)		const

all the non-local contribution terms of the reduced dark matter three-point correlation function

this function computes all the the non-local contribution terms of the reduced three-point correlation function, computed by cbl::cosmology::Cosmology::Q_nonLocal

Parameters

r1	the first side of the triangle
r2	the second side of the triangle
theta	the angle betwee r1 and r2
kk	vector of the wave vector modules at which the power spectrum is computed
Pk_matter	vector of containing the dark matter power spectrum values, estimated at the wave vector modules given in kk

Returns: vector containing the DM reduced three-point correlation function

Definition at line 145 of file 3PCF.cpp.

◆ qq()

double cbl::cosmology::Cosmology::qq ( const double redshift = 0. ) const

the deceleration parameter at a given redshift

Parameters

redshift the redshift

Returns: q

Definition at line 973 of file Cosmology.cpp.

◆ quadrupole() [1/2]

double cbl::cosmology::Cosmology::quadrupole	(	const double	Mass_min,
		const double	Mass_max,
		const double	redshift,
		const std::string	model_bias,
		const std::string	model_MF,
		const std::string	method_SS,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const double	Delta = `200.`,
		const double	kk = `-1.`,
		const std::string	interpType = `"Linear"`,
		const int	norm = `-1`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`
	)

the normalised quadrupole Q

Parameters

Mass_min	minimum halo mass
Mass_max	maximum halo mass
redshift	the redshift
model_bias	author(s) who proposed the bias; valid authors are: ST99 (Sheth & Tormen 1999), SMT01 (Sheth, Mo & Tormen 2001), SMT01_WL04 (Sheth, Mo & Tormen 2001 with the correction of Warren 2004), Tinker (Tinker et al. 2010)
model_MF	author(s) who proposed the mass function; valid authors are: PS (Press & Schechter), ST (Sheth & Tormen), Jenkins (Jenkins et al. 2001), Warren (Warren et al. 2006), ShenH (halo MF, Shen et al. 2006), ShenF (filament MF, Shen et al. 2006), ShenS (sheet MF, Shen et al. 2006), Pan (Pan 2007), Peacock (Peacock at al. 2007), Reed (Reed et al. 2007), Tinker (Tinker et al. 2008), Crocce (Crocce et al. 2010), Manera (Manera et al. 2010), Courtin (Courtin et al. 2010), Bhattacharya (Bhattacharya et al. 2011), Angulo_FOF (FoF MF, Angulo et al. 2012), Angulo_Sub (SUBFIND MF, Angulo et al. 2012), Watson_FOF (FoF MF, Watson et al. 2012), Watson_SOH (Spherical Overdensity halo MF, Watson et al. 2012), Despali_Z0, Despali_AllZ, Despali_AllZAllCosmo, Despali_HighM (Despali et al. 2016)
method_SS	method used to compute the power spectrum and σ(mass); valid method_SS are: CAMB [http://camb.info/], CLASS [http://class-code.net/], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
Delta	\(\Delta\), the overdensity
kk	wave vector module
interpType	method to interpolate the power spectrum
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed
prec	accuracy of the integration
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum

Returns: Q: the normalised quadrupole

Warning: the input parameter \(\Delta\) is the background overdensity, not the critical overdensity \(\Delta_{crit}\); divide \(\Delta_{crit}\) by \(\Omega_M(z)\) (see cbl::cosmology::Cosmology::OmegaM) to obtain the background overdensity; the mass function by Manera et al. (2010) has been tested only for z=0 and z=0.5; the mass function by Despali et al. (2016) is currently implemented only for virial masses and at \(z<1.25\)

Definition at line 121 of file RSD.cpp.

◆ quadrupole() [2/2]

double cbl::cosmology::Cosmology::quadrupole	(	const std::vector< double >	MM,
		const std::vector< double >	MF,
		const double	redshift,
		const std::string	model_bias,
		const std::string	method_SS,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const double	Delta = `200.`,
		const double	kk = `-1.`,
		const std::string	interpType = `"Linear"`,
		const int	norm = `-1`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`
	)

the normalised quadrupole Q

Parameters

MM	vector of halo masses
MF	vector of mass function values, dΦ/dM=dn(M)/dM
redshift	the redshift
model_bias	author(s) who proposed the bias; valid authors are: ST99 (Sheth & Tormen 1999), SMT01 (Sheth, Mo & Tormen 2001), SMT01_WL04 (Sheth, Mo & Tormen 2001 with the correction of Warren 2004), Tinker (Tinker et al. 2010)
method_SS	method used to compute the power spectrum and σ(mass); valid method_SS are: CAMB [http://camb.info/], CLASS [http://class-code.net/], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
Delta	\(\Delta\), the overdensity
kk	wave vector module
interpType	method to interpolate the power spectrum
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed
prec	accuracy of the integration
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum

Returns: Q: the normalised quadrupole

Warning: the input parameter \(\Delta\) is the background overdensity, not the critical overdensity \(\Delta_{crit}\); divide \(\Delta_{crit}\) by \(\Omega_M(z)\) (see cbl::cosmology::Cosmology::OmegaM) to obtain the background overdensity

Definition at line 131 of file RSD.cpp.

◆ r_rL()

double cbl::cosmology::Cosmology::r_rL ( const double deltav = -2.71 ) const

expansion factor

Author: Tommaso Ronconi; tomma.nosp@m.so.r.nosp@m.oncon.nosp@m.i@st.nosp@m.udio..nosp@m.unib.nosp@m.o.it

Parameters

deltav the linear density contrast: \(\delta_v^L\) (default value set to \(-2.71\))

Returns: the expansion factor: \(\frac{r}{r_L} = \bigl((1 - C^{-1}\delta_v^L\bigr)^{C/3}\) where \(C = 1.594\)

Definition at line 65 of file SizeFunction.cpp.

◆ r_vir()

double cbl::cosmology::Cosmology::r_vir	(	const double	M_vir,
		const double	redshift,
		const std::string	author = `"BryanNorman"`,
		const bool	unit1 = `false`
	)		const

the virial radius, given the virial mass and the redshift

this function computes the virial halo radius as follows:

\[r_{vir}(z) = \left(\frac{3 M_{vir}}{4\pi\Delta_c(z)\rho_{crit}(z)}\right)^{1/3}\]

where \(\Delta_c(z)\) is computed by cbl::cosmology::Cosmology::Delta_c and \(\rho_{crit}(z)\) is computed by cbl::cosmology::Cosmology::rho_crit

Parameters

M_vir	the virial mass
redshift	the redshift
author	the author of the \(\Delta_c(z)\) equation (see cbl::cosmology::Cosmology::Delta_c)
unit1	true \(\rightarrow\) force cosmological units

Returns: \(r_{vir}\)

Definition at line 1331 of file Cosmology.cpp.

◆ Redshift() [1/2]

double cbl::cosmology::Cosmology::Redshift	(	const double	d_c = `1.`,
		const double	z1_guess = `0.`,
		const double	z2_guess = `10.`,
		const double	prec = `0.0001`
	)		const

redshift at a given comoving distance

this method provides the redshift for a given comoving distance

Parameters

d_c	line-of-sight comoving distance
z1_guess	minimum prior on the redshift
z2_guess	maximum prior on the redshift
prec	precision of the computation ( prec = min(prec,1.e-5) )

Returns: redshift

Definition at line 1045 of file Cosmology.cpp.

◆ Redshift() [2/2]

double cbl::cosmology::Cosmology::Redshift	(	const double	mm,
		const double	redshift,
		const double	ff,
		const std::string	method_SS,
		const double	wwf,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`
	)		const

redshift at a given wf

this routine estimates the redshift from wf, given the parent halo mass at z=z', z', and its assembled fraction f

Author: Carlo Giocoli; cgioc.nosp@m.oli@.nosp@m.gmail.nosp@m..com

Parameters

mm	mass
redshift	the redshift
ff	assembled fraction
method_SS	method used to compute the power spectrum and σ(mass) const; valid method_SS are: CAMB [http://camb.info/], CLASS [http://class-code.net/], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
wwf	rescaled variable w as in Lacey and Coles 1993
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name

Returns: redshift

Definition at line 168 of file MassGrowth.cpp.

◆ redshift_distribution_haloes()

std::vector< double > cbl::cosmology::Cosmology::redshift_distribution_haloes	(	const double	z_min,
		const double	z_max,
		const int	step_z,
		const double	Area_degrees,
		const double	Mass_min,
		const double	Mass_max,
		const std::string	model_MF,
		const std::string	method_SS,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const double	Delta = `200`,
		const bool	isDelta_critical = `false`,
		const std::string	interpType = `"Linear"`,
		const double	k_max = `100.`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`
	)

redshift distribution of dark matter haloes

Author: Alfonso Veropalumbo; alfon.nosp@m.so.v.nosp@m.eropa.nosp@m.lumb.nosp@m.o@uni.nosp@m.bo.i.nosp@m.t

Parameters

z_min	minimum redshift
z_max	maximum redshift
step_z	redshift step
Area_degrees	the survey area, in degrees
Mass_min	minimum halo mass
Mass_max	maximum halo mass
model_MF	author(s) who proposed the mass function; valid authors are: PS (Press & Schechter), ST (Sheth & Tormen), Jenkins (Jenkins et al. 2001), Warren (Warren et al. 2006), ShenH (halo MF, Shen et al. 2006), ShenF (filament MF, Shen et al. 2006), ShenS (sheet MF, Shen et al. 2006), Pan (Pan 2007), Peacock (Peacock at al. 2007), Reed (Reed et al. 2007), Tinker (Tinker et al. 2008), Crocce (Crocce et al. 2010), Manera (Manera et al. 2010), Courtin (Courtin et al. 2010), Bhattacharya (Bhattacharya et al. 2011), Angulo_FOF (FoF MF, Angulo et al. 2012), Angulo_Sub (SUBFIND MF, Angulo et al. 2012), Watson_FOF (FoF MF, Watson et al. 2012), Watson_SOH (Spherical Overdensity halo MF, Watson et al. 2012), Despali_Z0, Despali_AllZ, Despali_AllZAllCosmo, Despali_HighM (Despali et al. 2016)
method_SS	method used to compute the power spectrum and σ(mass); valid method_SS are: CAMB [http://camb.info/], CLASS [http://class-code.net/], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
Delta	\(\Delta\), the overdensity
isDelta_critical	\(\rightarrow\) \(\Delta\) is the overdensity defined with respect to the critical density
interpType	method to interpolate the power spectrum
k_max	maximum wave vector module up to which the power spectrum is computed
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum

Returns: the redshift distribution of dark matter haloes

Warning: the input parameter \(\Delta\) is the background overdensity, not the critical overdensity \(\Delta_{crit}\); divide \(\Delta_{crit}\) by \(\Omega_M(z)\) (see cbl::cosmology::Cosmology::OmegaM) to obtain the background overdensity; the mass function by Manera et al. (2010) has been tested only for z=0 and z=0.5; the mass function by Despali et al. (2016) is currently implemented only for virial masses and at \(z<1.25\)

Definition at line 761 of file MassFunction.cpp.

◆ redshift_distribution_haloes_selection_function()

std::vector< double > cbl::cosmology::Cosmology::redshift_distribution_haloes_selection_function	(	const std::vector< double >	redshift,
		const double	Area_degrees,
		const double	Mass_min,
		const double	Mass_max,
		const std::string	model_MF,
		const std::string	method_SS,
		const std::string	selection_function_file,
		const std::vector< int >	column = `{}`,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const double	Delta = `200`,
		const bool	isDelta_critical = `false`,
		const std::string	interpType = `"Linear"`,
		const double	k_max = `100.`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`
	)

redshift distribution of dark matter haloes, given a selection function

Author: Alfonso Veropalumbo; alfon.nosp@m.so.v.nosp@m.eropa.nosp@m.lumb.nosp@m.o@uni.nosp@m.bo.i.nosp@m.t

Parameters

redshift	vector containing the redshift at which the halo distribution will be computed
Area_degrees	the survey area, in degrees
Mass_min	minimum halo mass
Mass_max	maximum halo mass
model_MF	author(s) who proposed the mass function; valid authors are: PS (Press & Schechter), ST (Sheth & Tormen), Jenkins (Jenkins et al. 2001), Warren (Warren et al. 2006), ShenH (halo MF, Shen et al. 2006), ShenF (filament MF, Shen et al. 2006), ShenS (sheet MF, Shen et al. 2006), Pan (Pan 2007), Peacock (Peacock at al. 2007), Reed (Reed et al. 2007), Tinker (Tinker et al. 2008), Crocce (Crocce et al. 2010), Manera (Manera et al. 2010), Courtin (Courtin et al. 2010), Bhattacharya (Bhattacharya et al. 2011), Angulo_FOF (FoF MF, Angulo et al. 2012), Angulo_Sub (SUBFIND MF, Angulo et al. 2012), Watson_FOF (FoF MF, Watson et al. 2012), Watson_SOH (Spherical Overdensity halo MF, Watson et al. 2012), Despali_Z0, Despali_AllZ, Despali_AllZAllCosmo, Despali_HighM (Despali et al. 2016)
method_SS	method used to compute the power spectrum and σ(mass); valid method_SS are: CAMB [http://camb.info/], CLASS [http://class-code.net/], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
selection_function_file	input file where the selection function is stored
column	the columns to be read
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
Delta	\(\Delta\), the overdensity
isDelta_critical	\(\rightarrow\) \(\Delta\) is the overdensity defined with respect to the critical density
interpType	method to interpolate the power spectrum
k_max	maximum wave vector module up to which the power spectrum is computed
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum

Returns: the redshift distribution of dark matter haloes

Warning: the input parameter \(\Delta\) is the background overdensity, not the critical overdensity \(\Delta_{crit}\); divide \(\Delta_{crit}\) by \(\Omega_M(z)\) (see cbl::cosmology::Cosmology::OmegaM) to obtain the background overdensity; the mass function by Manera et al. (2010) has been tested only for z=0 and z=0.5; the mass function by Despali et al. (2016) is currently implemented only for virial masses and at \(z<1.25\)

Definition at line 820 of file MassFunction.cpp.

◆ Redshift_LCDM()

double cbl::cosmology::Cosmology::Redshift_LCDM	(	const double	d_c = `1.`,
		const double	z1_guess = `0.`,
		const double	z2_guess = `10.`,
		const bool	go_fast = `1`,
		const double	prec = `0.0001`
	)		const

redshift at a given comoving distance

this method provides the redshift for a given comoving distance; the iteration process exploits the properties of the f=d(z) function (i.e. f'=1/E(z), f"<0)

Author: Mauro Roncarelli; mauro.nosp@m..ron.nosp@m.carel.nosp@m.li@u.nosp@m.nibo..nosp@m.it

Parameters

d_c	line-of-sight comoving distance
z1_guess	minimum redshift of the region explored to search the redshift
z2_guess	maximum redshift used to search the redshift
go_fast	0 \(\rightarrow\) the method uses the function Cosmology::D_C; 1 \(\rightarrow\) the method uses the function Cosmology::D_C_LCDM (much faster than D_C)
prec	precision of the computation; ( prec = min(prec,1.e-5) )

Returns: redshift

Warning: if go_fast=1, the method works correctly only for a flat ΛCDM universe at low enough redshifts where Ω_r is negligible;; wrong redshift interval limits do not lead to an error, but just slow down the computation

Definition at line 1101 of file Cosmology.cpp.

◆ Redshift_time()

double cbl::cosmology::Cosmology::Redshift_time	(	const double	time,
		const double	z1_guess,
		const double	z2_guess
	)		const

redshift at a given cosmic time

Parameters

time	cosmic time
z1_guess	minimum redshift used to search the redshift
z2_guess	maximum redshift used to search the redshift

Returns: redshift

Definition at line 1169 of file Cosmology.cpp.

◆ remove_output_Pk_tables()

void cbl::cosmology::Cosmology::remove_output_Pk_tables	(	const std::string	code,
		const bool	NL,
		const double	redshift,
		const std::string	output_root = `"test"`
	)		const

remove the output generated by the methods CAMB, MPTbreeze or CLASS

Parameters

code	method used to compute the power spectrum; valid codes are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465]
NL	false \(\rightarrow\) linear power spectrum; true \(\rightarrow\) non-linear power spectrum
redshift	redshift
output_root	output_root of the parameter file used to compute the power spectrum; it can be any name. If this parameter is different from the default value it will be used also in the output directory name

Definition at line 1030 of file PkXi.cpp.

◆ rho_crit()

double cbl::cosmology::Cosmology::rho_crit	(	const double	redshift,
		const bool	unit1 = `false`
	)		const

the critical cosmic density

this function computes the critical cosmic density at a given redshift:

\[\rho_{crit}(z)=\frac{3H^2(z)}{8\pi G}\]

Parameters

redshift	the redshift
unit1	true \(\rightarrow\) force cosmological units

Returns: the critical cosmic density [Msun*Mpc^-3(*h^2)]

Definition at line 1257 of file Cosmology.cpp.

◆ rho_m()

double cbl::cosmology::Cosmology::rho_m	(	const double	redshift = `0.`,
		const bool	unit1 = `false`,
		const bool	nu = `false`
	)		const

the mean cosmic background density

\[\rho_m(z) = \rho_{crit}(z)\Omega_M(z) = \frac{3H^2(z)}{8\pi G}\Omega_M(z)\]

Parameters

redshift	the redshift
unit1	true \(\rightarrow\) force cosmological units
nu	true \(\rightarrow\) compute \(\rho_m(z) = \rho_{crit}(z)[\Omega_M(z)-\Omega_\nu(z)]\)

Returns: ρ_mean: the mean cosmic background density [Msun*Mpc^-3(*h^2)]

Definition at line 1274 of file Cosmology.cpp.

◆ RhoZero()

double cbl::cosmology::Cosmology::RhoZero ( ) const

inline

get the private member Cosmology::m_RhoZero

Returns: ρ₀: the mean density of the Universe at z=0 [Msun*Mpc^-3]

Definition at line 1258 of file Cosmology.h.

◆ rs() [1/3]

double cbl::cosmology::Cosmology::rs ( ) const

inline

get the sound horizon at recombination

Returns: \(r_s\); the sound horizon at recombination epoch

Definition at line 1289 of file Cosmology.h.

◆ rs() [2/3]

double cbl::cosmology::Cosmology::rs	(	const double	redshift,
		const double	T_CMB = `2.7255`
	)		const

the sound horizon

Parameters

redshift	the redshift
T_CMB	the temperature of the Cosmic Microwave Background

Returns: the sound horizon

Definition at line 252 of file BAO.cpp.

◆ rs() [3/3]

double cbl::cosmology::Cosmology::rs	(	const std::string	method_Pk,
		const double	T_CMB = `par::TCMB`
	)		const

the sound horizon at the drag epoch r_s(z_d), valid choices for method_Pk are: EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html], CAMB [http://camb.info/]

Author: Alfonso Veropalumbo; alfon.nosp@m.so.v.nosp@m.eropa.nosp@m.lumb.nosp@m.o@uni.nosp@m.bo.i.nosp@m.t

Parameters

method_Pk	the method to compute the sound horizon
T_CMB	T_CMB: the present day CMB temperature [K]

Returns: r_s

Definition at line 141 of file BAO.cpp.

◆ rs_CAMB()

double cbl::cosmology::Cosmology::rs_CAMB ( ) const

the sound horizon at the drag epoch estimated with CAMB [http://camb.info/], analytical formula by Aubourg et al. 2014

see Anderson et al 2014, Eq. 16

Author: Alfonso Veropalumbo; alfon.nosp@m.so.v.nosp@m.eropa.nosp@m.lumb.nosp@m.o@uni.nosp@m.bo.i.nosp@m.t

Returns: r_s

Definition at line 183 of file BAO.cpp.

◆ rs_EH()

double cbl::cosmology::Cosmology::rs_EH ( const double T_CMB = par::TCMB ) const

the sound horizon at the drag epoch predicted by Eisentein & Hu 1998

see Eisentein & Hu 1998, Section 2.1

Author: Alfonso Veropalumbo; alfon.nosp@m.so.v.nosp@m.eropa.nosp@m.lumb.nosp@m.o@uni.nosp@m.bo.i.nosp@m.t

Parameters

T_CMB CMB temperature

Returns: r_s

Definition at line 158 of file BAO.cpp.

◆ rs_integrand()

double cbl::cosmology::Cosmology::rs_integrand	(	const double	redshift,
		const double	T_CMB = `2.7255`
	)		const

the sound horizon integrand

Parameters

redshift	the redshift
T_CMB	the temperature of the Cosmic Microwave Background

Returns: the sound horizon integrand

Definition at line 232 of file BAO.cpp.

◆ run_CAMB() [1/2]

void cbl::cosmology::Cosmology::run_CAMB	(	const bool	NL,
		const double	redshift,
		const std::string	output_root = `par::defaultString`,
		const std::string	output_dir = `par::defaultString`,
		const double	k_max = `100.`,
		const std::string	file_par = `par::defaultString`
	)		const

run CAMB [http://camb.info/]

this function runs CAMB [http://camb.info/], after editing the parameter file appropriately (if file_par=NULL)

Parameters

NL	0 \(\rightarrow\) linear power spectrum; 1 \(\rightarrow\) non-linear power spectrum
redshift	the redshift
output_root	the output_root parameter of the parameter file used to compute the power spectrum; it can be any name. If NULL, the output will be deleted after running CAMB
output_dir	std::string containing the output directory
k_max	maximum wave vector module up to which the power spectrum is computed
file_par	name of the parameter file; if a parameter file is provided (i.e. file_par!=NULL), it will use be used, ignoring the cosmological parameters of the object

Definition at line 106 of file PkXi.cpp.

◆ run_CAMB() [2/2]

void cbl::cosmology::Cosmology::run_CAMB	(	std::vector< double > &	lgkk,
		std::vector< double > &	lgPk,
		const bool	NL,
		const double	redshift,
		const std::string	output_root = `"test"`,
		const std::string	output_dir = `par::defaultString`,
		const double	k_max = `100.`,
		const std::string	file_par = `par::defaultString`
	)		const

run CAMB [http://camb.info/] and read the matter power spectrum

this function runs CAMB [http://camb.info/], after editing the parameter file appropriately (if file_par=NULL) and store the matter power spectrum in two vectors

Parameters

[out]	lgkk	vector of log(k)
[out]	lgPk	vector of log(P(k))
	NL	0 \(\rightarrow\) linear power spectrum; 1 \(\rightarrow\) non-linear power spectrum
	redshift	the redshift
	output_root	the output_root parameter of the parameter file used to compute the power spectrum; it can be any name. If NULL, the output will be deleted after running CAMB
	output_dir	std::string containing the output directory
	k_max	maximum wave vector module up to which the power spectrum is computed
	file_par	name of the parameter file; if a parameter file is provided (i.e. file_par!=NULL), it will use be used, ignoring the cosmological parameters of the object

Definition at line 176 of file PkXi.cpp.

◆ scalar_amp()

double cbl::cosmology::Cosmology::scalar_amp ( ) const

inline

get the private member Cosmology::m_scalar_amp

Returns: \(A_s\): the initial scalar amplitude of the power spectrum

Definition at line 1220 of file Cosmology.h.

◆ scalar_pivot()

double cbl::cosmology::Cosmology::scalar_pivot ( ) const

inline

get the private member Cosmology::m_scalar_pivot

Returns: the scalar pivot k in \(Mpc^{-1}\)

Definition at line 1227 of file Cosmology.h.

◆ set_fNL()

void cbl::cosmology::Cosmology::set_fNL ( const double fNL = 0. )

inline

set the value of f_NL

Parameters

fNL	f_NL: the non-Gaussian amplitude

Definition at line 1600 of file Cosmology.h.

◆ set_H0()

void cbl::cosmology::Cosmology::set_H0	(	const double	H0 = `70.`,
		const bool	warn = `true`
	)

inline

set the value of H₀

Parameters

H0	H₀: Hubble constant [km/sec/Mpc]
warn	true \(\rightarrow\) print a warning message if m_unit is true

Definition at line 1533 of file Cosmology.h.

◆ set_hh()

void cbl::cosmology::Cosmology::set_hh	(	const double	hh = `0.7`,
		const bool	warn = `true`
	)

inline

set the value of h

Parameters

hh	the Hubble constant H0/100
warn	true \(\rightarrow\) print a warning message if m_unit is true

Definition at line 1516 of file Cosmology.h.

◆ set_model()

void cbl::cosmology::Cosmology::set_model ( const std::string model = "LCDM" )

inline

set the cosmologial model used to compute distances

Parameters

model the cosmologial model used to compute distances

Definition at line 1630 of file Cosmology.h.

◆ set_n_spec()

void cbl::cosmology::Cosmology::set_n_spec ( const double n_spec )

inline

set the value of n_spec

Parameters

n_spec n_spec: the primordial spectral index

Definition at line 1569 of file Cosmology.h.

◆ set_Omega()

void cbl::cosmology::Cosmology::set_Omega ( const double Omega_matter = 0.27 )

inline

set the value of Ω_M, keeping Ω_DE=1-Ω_M-Ω_rad-Ω_k

Parameters

Omega_matter Ω_M: density of baryons, cold dark matter and massive neutrinos (in units of the critical density)

Definition at line 1419 of file Cosmology.h.

◆ set_Omega_all()

void cbl::cosmology::Cosmology::set_Omega_all	(	const double	OmegaB,
		const double	OmegaCDM,
		const double	OmegaNu,
		const double	OmegaR,
		const double	OmegaDE
	)

inline

set the value of \(\Omega_{\rm b}\), \(\Omega_{\rm cdm}\), \(\Omega_{\nu}\), \(\Omega_{\rm rad}\), \(\Omega_{\rm DE}\), and consequently the values of

\(\Omega_{\rm M} = \Omega_{\rm b}+\Omega_{\rm cdm}+\Omega_{\nu}, \)

and

\(\Omega_{\rm k} = 1-\Omega_{\rm M}-\Omega_{\rm rad}-\Omega_{\rm DE}\)

Parameters

OmegaB	density of baryons, \(\Omega_{\rm M}\), in units of the critical density
OmegaCDM	density of cold dark matter, \(\Omega_{\rm cdm}\), in units of the critical density
OmegaNu	density of massive neutrinos, \(\Omega_{\nu}\), in units of the critical density
OmegaR	density of radiation, \(\Omega_{\rm rad}\), in units of the critical density
OmegaDE	density of dark energy, \(\Omega_{\rm DE}\), in units of the critical density

Definition at line 1399 of file Cosmology.h.

◆ set_Omega_radiation()

void cbl::cosmology::Cosmology::set_Omega_radiation ( const double Omega_radiation )

inline

set the private member Cosmology::m_Omega_radiation

Parameters

Omega_radiation \(\Omega_{rad}\): the radiation density

Definition at line 1502 of file Cosmology.h.

◆ set_OmegaB()

void cbl::cosmology::Cosmology::set_OmegaB ( const double Omega_baryon = 0.046 )

inline

set the value of Ω_b, keeping Ω_CDM=Ω_M-Ω_b

Parameters

Omega_baryon Ω_b: density of baryons, (in units of the critical density)

Definition at line 1432 of file Cosmology.h.

◆ set_OmegaB_h2()

void cbl::cosmology::Cosmology::set_OmegaB_h2 ( const double Omega_baryonh2 = 0.0222 )

inline

set the value of Ω_b, keeping Ω_CDM=Ω_M-Ω_b

Parameters

Omega_baryonh2 Ω_bh²: density of baryons, (in units of the critical density) times h²

Definition at line 1446 of file Cosmology.h.

◆ set_OmegaDE()

void cbl::cosmology::Cosmology::set_OmegaDE ( const double Omega_DE = 0.73 )

inline

set the value of Ω_DE

Parameters

Omega_DE Ω_DE: density of dark energy

Definition at line 1471 of file Cosmology.h.

◆ set_OmegaM()

void cbl::cosmology::Cosmology::set_OmegaM ( const double Omega_matter = 0.27 )

inline

set the value of Ω_M

Parameters

Omega_matter Ω_M: density of baryons, cold dark matter and massive neutrinos (in units of the critical density)

Definition at line 1459 of file Cosmology.h.

◆ set_OmegaNu()

void cbl::cosmology::Cosmology::set_OmegaNu	(	const double	Omega_neutrinos = `0.`,
		const double	massless_neutrinos = `3.04`,
		const int	massive_neutrinos = `0`
	)

inline

set the value of Ω_ν

Parameters

Omega_neutrinos	Ω_ν: density of massive neutrinos
massless_neutrinos	N_eff: the effective number (for QED + non-instantaneous decoupling)
massive_neutrinos	the number of degenerate massive neutrino species

Definition at line 1486 of file Cosmology.h.

◆ set_parameter()

void cbl::cosmology::Cosmology::set_parameter	(	const CosmologicalParameter	parameter,
		const double	value
	)

set the value of one cosmological paramter

Parameters

parameter	cosmological parameter to set
value	the new value for the parameter

Definition at line 424 of file Cosmology.cpp.

◆ set_parameters()

void cbl::cosmology::Cosmology::set_parameters	(	const std::vector< CosmologicalParameter >	parameter,
		const std::vector< double >	value
	)

set the value of some cosmological paramters

Parameters

parameter	vector containing the cosmological parameters to set
value	vector containing the new values for the parameters

Examples: model_2pt_monopole_BAO.cpp.

Definition at line 525 of file Cosmology.cpp.

◆ set_RhoZero()

void cbl::cosmology::Cosmology::set_RhoZero ( const double RhoZero = 7.5e10 )

inline

set the value of ρ₀

Parameters

RhoZero the mean density of the Universe at z=0 [Msun*Mpc^-3]

Definition at line 1593 of file Cosmology.h.

◆ set_rs()

void cbl::cosmology::Cosmology::set_rs ( const double rs = -1 )

inline

set the value of the \(r_s\);

Parameters

rs	the sound horizon

Definition at line 1623 of file Cosmology.h.

◆ set_scalar_amp()

void cbl::cosmology::Cosmology::set_scalar_amp ( const double scalar_amp = 2.46e-9 )

inline

set the value of A_s

Parameters

scalar_amp \(A_s\): initial scalar amplitude of the power spectrum

Definition at line 1555 of file Cosmology.h.

◆ set_scalar_pivot()

void cbl::cosmology::Cosmology::set_scalar_pivot ( const double scalar_pivot = 0.05 )

inline

set the value of the scalar pivot

Parameters

scalar_pivot the scalar pivot k in \(Mpc^{-1}\)

Definition at line 1562 of file Cosmology.h.

◆ set_sigma8()

void cbl::cosmology::Cosmology::set_sigma8 ( const double sigma8 = -1. )

inline

set the value of σ₈

Parameters

sigma8 σ₈: power spectrum normalisation

Examples: model_2pt_2D.cpp, model_2pt_monopole_RSD.cpp, model_2pt_projected.cpp, and modelling_VoidAbundances.cpp.

Definition at line 1547 of file Cosmology.h.

◆ set_tau()

void cbl::cosmology::Cosmology::set_tau ( const double tau = 0.09 )

inline

set the value of the τ

Parameters

τ	the Thomson scattering optical depth due to reionization

Definition at line 1616 of file Cosmology.h.

◆ set_type_NG()

void cbl::cosmology::Cosmology::set_type_NG ( const int type_NG = 1 )

inline

set the value of the non-Gaussian shape

Parameters

type_NG the non-Gaussian shape (type=1 local, type=2 equilateral, type=3 enfolded, type=4 orthogonal)

Definition at line 1608 of file Cosmology.h.

◆ set_unit()

void cbl::cosmology::Cosmology::set_unit ( const bool unit = true )

inline

set the value of unit

Parameters

unit	false \(\rightarrow\) phyical units; true \(\rightarrow\) cosmological units (i.e. in units of h)

Definition at line 1638 of file Cosmology.h.

◆ set_w0()

void cbl::cosmology::Cosmology::set_w0 ( const double w0 = -1. )

inline

set the value of w₀

Parameters

w0	w₀: parameter of the dark energy equation of state (CPL parameterisation)

Definition at line 1577 of file Cosmology.h.

◆ set_wa()

void cbl::cosmology::Cosmology::set_wa ( const double wa = 0. )

inline

set the value of w_a

Parameters

wa	w_a: parameter of the dark energy equation of state (CPL parameterisation)

Definition at line 1585 of file Cosmology.h.

◆ sigma2M()

double cbl::cosmology::Cosmology::sigma2M	(	const double	mass,
		const std::string	method_Pk,
		const double	redshift,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const std::string	interpType = `"Linear"`,
		const double	k_max = `100.`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`,
		const bool	unit1 = `false`
	)		const

the mass variance, \(\sigma^2(M)\)

this function computes the variance of the linear density field:

\[ \sigma^2(M) = \frac{1}{2\pi^2}\int_0^\infty {\rm d}k\, k^2 P_{lin}(k, z) W^2(k, R)\]

where \(W(x)=(3/x)^3(\sin x-x\cos x)\) and \(R=(3M/4\pi\rho_m)^{1/3}\)

Parameters

mass	the mass
method_Pk	the method used to compute the power spectrum; valid choices for method_Pk are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
redshift	the redshift
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	the output_root parameter of the parameter file used to compute the power spectrum; it can be any name. If this parameter is different from the default value it will be used also in the output directory name
interpType	method to interpolate the power spectrum
k_max	maximum wave vector module up to which the power spectrum is computed
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum
unit1	true \(\rightarrow\) force cosmological units

Returns: \(\sigma^2(M)\)

Definition at line 230 of file Sigma.cpp.

◆ sigma2R()

double cbl::cosmology::Cosmology::sigma2R	(	const double	radius,
		const std::string	method_Pk,
		const double	redshift,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const std::string	interpType = `"Linear"`,
		const double	k_max = `100.`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`,
		const bool	unit1 = `false`
	)		const

the mass variance, \(\sigma^2(R)\)

this function computes the variance of the linear density field:

\[ \sigma^2(R)=\frac{1}{2\pi^2}\int_0^\infty {\rm d}k\, k^2 P_{lin}(k, z) W^2(k, R)\]

where \(W(x)=(3/x)^3(\sin x-x\cos x)\)

Parameters

radius	the radius, \(R\)
method_Pk	method used to compute the power spectrum (i.e. the Boltzmann solver); valid choices for method_Pk are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
redshift	the redshift
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	the output_root parameter of the parameter file used to compute the power spectrum; it can be any name. If this parameter is different from the default value it will be used also in the output directory name
interpType	method to interpolate the power spectrum
k_max	maximum wave vector module up to which the power spectrum is computed
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum
unit1	true \(\rightarrow\) force cosmological units

Returns: \(\sigma^2(R)\)

Definition at line 152 of file Sigma.cpp.

◆ sigma8() [1/2]

double cbl::cosmology::Cosmology::sigma8 ( ) const

inline

get the private member Cosmology::m_sigma8

Returns: σ₈: the power spectrum normalisation

Examples: model_2pt_2D.cpp.

Definition at line 1212 of file Cosmology.h.

◆ sigma8() [2/2]

double cbl::cosmology::Cosmology::sigma8 ( const double redshift ) const

σ₈ at a given redshift

Parameters

redshift the redshift

Returns: σ₈

Definition at line 729 of file Cosmology.cpp.

◆ sigma8_interpolated()

double cbl::cosmology::Cosmology::sigma8_interpolated ( const double redshift ) const

σ₈

this function provides an approximate value of σ₈, at a given redshift, from Aubourg et al. 2015, eq.(32)

Warning: it is valid only without massive neutrinos! To account for non-zero neutrino mass authors multiplies by an extra factor of 0.995

Parameters

redshift the redshift

Returns: σ₈

Definition at line 58 of file PkXi.cpp.

◆ sigma8_Pk()

double cbl::cosmology::Cosmology::sigma8_Pk	(	const std::string	method_Pk,
		const double	redshift,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const bool	NL = `0`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`,
		const std::string	file_par = `par::defaultString`
	)		const

the dark matter rms mass fluctuation within 8 Mpc/h

this function provides the rms mass fluctuation within 8 Mpc/h, estimated directly from the power spectrum

Parameters

method_Pk	method used to compute the power spectrum (i.e. the Boltzmann solver); valid choices for method_Pk are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
redshift	the redshift
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
NL	0 \(\rightarrow\) linear power spectrum; 1 \(\rightarrow\) non-linear power spectrum
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed
prec	accuracy of the integration
file_par	name of the parameter file; if a parameter file is provided (i.e. file_par!=NULL), it will be used, ignoring the cosmological parameters of the object

Returns: σ₈: the dark matter rms mass fluctuation within 8 Mpc/h

Definition at line 1764 of file PkXi.cpp.

◆ sigma_v()

double cbl::cosmology::Cosmology::sigma_v	(	const double	redshift = `0.`,
		const std::string	method_Pk = `"CAMB"`,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const int	norm = `-1`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const int	bin_k = `512`,
		const double	prec = `1.e-2`,
		const std::string	file_par = `par::defaultString`,
		const bool	unit1 = `false`
	)

the linear-order one-dimensional pairwise velocity dispersion, \(\sigma_{\mathrm{v}, \mathrm{lin}}\)

This function computes the linear-order one-dimensional pairwise velocity dispersion, \(\sigma_{\mathrm{v}, \mathrm{lin}}\), as defined in Taruya et al. (2010) (Eq. 7 of https://arxiv.org/abs/1006.0699)

\[ \sigma_{\mathrm{v}, \mathrm{lin}}^{2} = \frac{1}{3} \int \frac{d^{3} \boldsymbol{q}}{(2 \pi)^{3}} \frac{P_{\mathrm{lin}}(q, z)}{q^{2}} \]

where \(P_{\mathrm{lin}}(q, z)\) is the linear power spectrum at a given redshift

Parameters

redshift	the redshift
method_Pk	method used to compute the power spectrum (i.e. the Boltzmann solver); valid choices for method_Pk are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	the output_root parameter of the parameter file used to compute the power spectrum; it can be any name. If this parameter is different from the default value it will be used also in the output directory name
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed to estimate the power spectrum normalisation; this parameter is used only if norm=1
bin_k	number of wave vector modules used for the integration
prec	accuracy of the integration
file_par	name of the parameter file; if a parameter file is provided (i.e. file_par!=NULL), it will be used, ignoring the cosmological parameters of the object
unit1	true \(\rightarrow\) force cosmological units

Returns: \(\sigma_{\mathrm{v}, \mathrm{lin}}\)

Definition at line 199 of file RSD.cpp.

◆ Sigman_PT()

double cbl::cosmology::Cosmology::Sigman_PT	(	const int	nn,
		const double	RR,
		const std::string	method_SS,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const std::string	interpType = `"Linear"`,
		const double	k_max = `100.`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`
	)		const

the deprojected hierarchical moments Σ_n

this function provides the deprojected hierarchical moments Σ_n given by the perturbation theory (see e.g. Juszkiewicz et al. 1993, Bernardeau 1994, Wolk 2013)

Parameters

nn	order of the moment
RR	comoving separation
method_SS	method used to compute the power spectrum and σ(mass); valid method_SS are: CAMB [http://camb.info/], CLASS [http://class-code.net/], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
interpType	method to interpolate the power spectrum
k_max	maximum wave vector module up to which the power spectrum is computed
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum

Returns: the deprojected hierarchical moments, Σ_n, given by the perturbation theory

Definition at line 1861 of file PkXi.cpp.

◆ sigmaR_DM()

double cbl::cosmology::Cosmology::sigmaR_DM	(	const double	RR,
		const int	corrType,
		const std::string	method_Pk,
		const double	redshift,
		const double	pimax = `40`,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const bool	NL = `1`,
		const int	norm = `-1`,
		const double	r_min = `1.e-3`,
		const double	r_max = `350.`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	aa = `0.`,
		const bool	GSL = `false`,
		const double	prec = `1.e-2`,
		const std::string	file_par = `par::defaultString`
	)

the dark matter rms mass fluctuation

Parameters

RR	radius inside which the dark matter rms mass fluctuation is computed
corrType	0 \(\rightarrow\) the projected correlation function, w(θ), is used; 1 \(\rightarrow\) the spherically averaged correlation function, ξ(r), is used
method_Pk	method used to compute the power spectrum (i.e. the Boltzmann solver); valid choices for method_Pk are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
redshift	the redshift
pimax	the upper limit of the line-of-sight integration
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
NL	0 \(\rightarrow\) linear power spectrum; 1 \(\rightarrow\) non-linear power spectrum
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
r_min	minimum separation up to which the correlation function is computed
r_max	maximum separation up to which the correlation function is computed
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed
aa	parameter a of Eq. 24 of Anderson et al. 2012
GSL	false \(\rightarrow\) FFTlog is used; true \(\rightarrow\) the GSL libraries are used
prec	accuracy of the integration
file_par	name of the parameter file; if a parameter file is provided (i.e. file_par!=NULL), it will be used, ignoring the cosmological parameters of the object

Returns: σ_R: the dark matter rms mass fluctuation

Definition at line 1686 of file PkXi.cpp.

◆ size_function() [1/3]

double cbl::cosmology::Cosmology::size_function	(	const double	RV,
		const double	redshift,
		const std::string	model,
		const double	b_eff,
		double	slope = `0.854`,
		double	offset = `0.420`,
		const double	deltav_NL = `-0.795`,
		const double	del_c = `1.69`,
		const std::string	method_Pk = `"EisensteinHu"`,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const std::string	interpType = `"Linear"`,
		const double	k_max = `100.`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`
	)		const

the void size function

Author: Tommaso Ronconi; tomma.nosp@m.so.r.nosp@m.oncon.nosp@m.i@st.nosp@m.udio..nosp@m.unib.nosp@m.o.it

Parameters

RV	radius
redshift	the redshift
model	size function model name; valid choices for model name are SvdW (Sheth and van de Weygaert, 2004), linear and Vdn (Jennings et al., 2013)
b_eff	the effective bias of the sample
slope	first coefficent to convert the effective bias (default value set to \(0.854\))
offset	second coefficent to convert the effective bias (default value set to \(0.420\))
deltav_NL	the non linear density contrast: \(\rho_v/\rho_m\) (default value set to \(-0.795\))
del_c	critical value of the linear density field (default value set to \(1.06\))
method_Pk	method used to compute the power spectrum (i.e. the Boltzmann solver); valid choices for method_Pk are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
interpType	method to interpolate the power spectrum
k_max	maximum wave vector module up to which the power spectrum is computed
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum

Returns: the number density of voids as a function of radius. Volume Conserving Model, equation (17) from Jennings et al.(2013)

Definition at line 112 of file SizeFunction.cpp.

◆ size_function() [2/3]

double cbl::cosmology::Cosmology::size_function	(	const double	RV,
		const double	redshift,
		const std::string	model_mf,
		const double	del_v,
		const std::string	model_sf,
		const std::string	method_Pk = `"EisensteinHu"`,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const double	Delta = `200.`,
		const std::string	interpType = `"Linear"`,
		const int	norm = `-1`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`
	)

the void size function

Author: Tommaso Ronconi; tomma.nosp@m.so.r.nosp@m.oncon.nosp@m.i@st.nosp@m.udio..nosp@m.unib.nosp@m.o.it

Parameters

RV	radius
redshift	the redshift
model_mf	author(s) who proposed the mass function; valid authors are: PS (Press & Schechter), ST (Sheth & Tormen), Jenkins (Jenkins et al. 2001), Warren (Warren et al. 2006), Reed, (Reed et al. 2007), Pan (Pan 2007), ShenH (halo MF by Shen et al. 2006), ShenF (filaments MF by Shen et al. 2006), ShenS (sheets MF by Shen et al. 2006), Tinker (Tinker et al. 2008), Crocce (Crocce et al. 2010), Angulo_FOF (FOF MF by Angulo et al. 2012), Angulo_Sub (SUBFIND MF by Angulo et al. 2012), Watson_FOF(FOF MF by Watson et al. 2012), Watson_SOH (MF for Spherical Overdensity Haloes by Watson et al. 2012), Manera (Manera et al. 2010), Bhattacharya (Bhattacharya et al. 2011), Courtin (Courtin et al. 2010), Peacock (by Peacock at al. 2007)
del_v	linear density contrast defining a void
model_sf	size function model name; valid choices for model name are SvdW (Sheth and van de Weygaert, 2004), linear and Vdn (Jennings et al., 2013)
method_Pk	method used to compute the power spectrum (i.e. the Boltzmann solver); valid choices for method_Pk are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
Delta	\(\Delta\), the overdensity
interpType	method to interpolate the power spectrum
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
prec	accuracy of the integration
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum

Returns: the number density of voids as a function of radius. Volume Conserving Model, equation (17) from Jennings et al.(2013)

Definition at line 306 of file SizeFunction.cpp.

◆ size_function() [3/3]

std::vector< double > cbl::cosmology::Cosmology::size_function	(	const std::vector< double >	RV,
		const double	redshift,
		const std::string	model,
		const double	b_eff,
		double	slope = `0.854`,
		double	offset = `0.420`,
		const double	deltav_NL = `-0.795`,
		const double	del_c = `1.69`,
		const std::string	method_Pk = `"EisensteinHu"`,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const std::string	interpType = `"Linear"`,
		const double	k_max = `100.`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`
	)		const

the void size function

Author: Sofia Contarini; sofia.nosp@m..con.nosp@m.tarin.nosp@m.i3@u.nosp@m.nibo..nosp@m.it

Parameters

RV	vector of radii
redshift	the redshift
model	size function model name; valid choices for model name are SvdW (Sheth and van de Weygaert, 2004), linear and Vdn (Jennings et al., 2013)
b_eff	the effective bias of the sample
slope	first coefficent to convert the effective bias (default value set to \(0.854\))
offset	second coefficent to convert the effective bias (default value set to \(0.420\))
deltav_NL	the non linear density contrast: \(\rho_v/\rho_m\) (default value set to \(-0.795\))
del_c	critical value of the linear density field (default value set to \(1.06\))
method_Pk	method used to compute the power spectrum (i.e. the Boltzmann solver); valid choices for method_Pk are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
interpType	method to interpolate the power spectrum
k_max	maximum wave vector module up to which the power spectrum is computed
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum

Returns: the number density of voids as a function of radius. Volume Conserving Model, equation (17) from Jennings et al.(2013) for each radius

Definition at line 144 of file SizeFunction.cpp.

◆ skewness()

double cbl::cosmology::Cosmology::skewness	(	const double	mass,
		const std::string	method_Pk,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const std::string	interpType = `"Linear"`,
		const int	norm = `-1`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`
	)

the skewness

Author: Cosimo Fedeli; cosim.nosp@m.o.fe.nosp@m.deli@.nosp@m.oabo.nosp@m..inaf.nosp@m..it

Parameters

mass	halo mass
method_Pk	method used to compute the power spectrum (i.e. the Boltzmann solver); valid choices for method_Pk are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	the output_root parameter of the parameter file used to compute the power spectrum; it can be any name. If this parameter is different from the default value it will be used also in the output directory name
interpType	method to interpolate the power spectrum
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
prec	accuracy of the integration
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum

Returns: skewness

Definition at line 414 of file NG.cpp.

◆ Sn_PT()

double cbl::cosmology::Cosmology::Sn_PT	(	const int	nn,
		const double	RR,
		const std::string	method_SS,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const std::string	interpType = `"Linear"`,
		const double	k_max = `100.`,
		const std::string	input_file = `par::defaultString`,
		const bool	is_parameter_file = `true`
	)		const

the hierarchical moments S_n

this function provides the hierarchical moments S_n given by the perturbation theory (see e.g. Juszkiewicz et al. 1993, Bernardeau 1994, Wolk 2013)

Parameters

nn	order of the moment
RR	comoving separation
method_SS	method used to compute the power spectrum and σ(mass); valid method_SS are: CAMB [http://camb.info/], CLASS [http://class-code.net/], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
interpType	method to interpolate the power spectrum
k_max	maximum wave vector module up to which the power spectrum is computed
input_file	either the parameter file or the power spectrum file; if a parameter file is provided, i.e. input_file!=NULL and is_parameter_file=true, it will be used to compute the power spectrum; if a power spectrum file is provided, i.e. input_file!=NULL and is_parameter_file=false, then the provided power spectrum will be used directly; in both cases σ²(M) is computed by integrating the computed/provided power spectrum ignoring the cosmological parameters of the object
is_parameter_file	true \(\rightarrow\) the input_file is a parameter file, used to compute the power spectrum with the method specified by method_Pk; false \(\rightarrow\) the input_file is a file containing the power spectrum

Returns: the hierarchical moments, S_n, given by the perturbation theory

Definition at line 1826 of file PkXi.cpp.

◆ sound_speed()

double cbl::cosmology::Cosmology::sound_speed	(	const double	redshift,
		const double	T_CMB = `2.7255`
	)		const

the sound speed

Parameters

redshift	the redshift
T_CMB	the temperature of the Cosmic Microwave Background

Returns: the sound speed

Definition at line 215 of file BAO.cpp.

◆ square_bulk_flow()

double cbl::cosmology::Cosmology::square_bulk_flow	(	const double	rr,
		const double	k_int_min,
		const std::string	method_Pk,
		const double	redshift,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`,
		const std::string	file_par = `par::defaultString`
	)

the mean square bulk flow

Parameters

rr	comoving radius
k_int_min	minimum wave vector module up to which the integral is computed
method_Pk	method used to compute the power spectrum and σ(mass) (i.e. the Boltzmann solver); valid choices for method_Pk are: CAMB [http://camb.info/], CLASS [http://class-code.net/], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
redshift	the redshift
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed
prec	accuracy of the integration
file_par	name of the parameter file; if a parameter file is provided (i.e. file_par!=NULL), it will be used, ignoring the cosmological parameters of the object

Returns: the mean square bulk flow

Definition at line 45 of file Velocities.cpp.

◆ square_bulk_flow_Table()

double cbl::cosmology::Cosmology::square_bulk_flow_Table	(	const double	rr,
		const double	k_int_min,
		const std::vector< double >	lgkk,
		const std::vector< double >	lgPk,
		const double	redshift
	)		const

the mean square bulk flow

Parameters

rr	comoving radius
k_int_min	minimum wave vector module up to which the integral is computed
lgkk	vector of log(k)
lgPk	vector of log(P(k))
redshift	the redshift

Returns: the mean square bulk flow

Definition at line 82 of file Velocities.cpp.

◆ square_velocity_dispersion()

double cbl::cosmology::Cosmology::square_velocity_dispersion	(	const double	rr,
		const double	k_int_min,
		const std::string	method_Pk,
		const double	redshift,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`,
		const std::string	file_par = `par::defaultString`
	)

the mean square velocity dispersion

Parameters

rr	comoving radius
k_int_min	minimum wave vector module up to which the integral is computed
method_Pk	method used to compute the power spectrum and σ(mass) (i.e. the Boltzmann solver); valid choices for method_Pk are: CAMB [http://camb.info/], CLASS [http://class-code.net/], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
redshift	the redshift
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed
prec	accuracy of the integration
file_par	name of the parameter file; if a parameter file is provided (i.e. file_par!=NULL), it will be used, ignoring the cosmological parameters of the object

Returns: the mean square velocity dispersion

Definition at line 98 of file Velocities.cpp.

◆ t_H()

double cbl::cosmology::Cosmology::t_H ( ) const

inline

get the private member Cosmology::m_t_H

Returns: t_H: the Hubble time

Definition at line 1198 of file Cosmology.h.

◆ Table_PkCodes() [1/2]

void cbl::cosmology::Cosmology::Table_PkCodes	(	const std::string	code,
		const bool	NL,
		std::vector< double > &	lgkk,
		std::vector< double > &	lgPk,
		const double	redshift,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const double	k_max = `100.`,
		const std::string	file_par = `par::defaultString`
	)		const

write or read the table where the dark matter power spectrum is stored

Parameters

[in]	code	method used to compute the power spectrum; valid codes are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465]
[in]	NL	false \(\rightarrow\) linear power spectrum; true \(\rightarrow\) non-linear power spectrum
[out]	lgkk	vector of log(k)
[out]	lgPk	vector of log(P(k))
[in]	redshift	redshift
[in]	store_output	if true the output files created are stored; if false the output files created are removed
[in]	output_root	output_root of the parameter file used to compute the power spectrum; it can be any name. If this parameter is different from the default value it will be used also in the output directory name
[in]	k_max	maximum wave vector module up to which the power spectrum is computed
[in]	file_par	name of the parameter file; if a parameter file is provided (i.e. file_par!=NULL), it will be used, ignoring the cosmological parameters of the object

Definition at line 258 of file PkXi.cpp.

◆ Table_PkCodes() [2/2]

void cbl::cosmology::Cosmology::Table_PkCodes	(	const std::string	code,
		const bool	NL,
		std::vector< std::vector< double >> &	lgkk,
		std::vector< std::vector< double >> &	lgPk,
		const std::vector< double >	redshift,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const double	k_max = `100.`,
		const std::string	file_par = `par::defaultString`
	)		const

write or read the table where the dark matter power spectrum is stored

Parameters

[in]	code	method used to compute the power spectrum; valid codes are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465]
[in]	NL	false \(\rightarrow\) linear power spectrum; true \(\rightarrow\) non-linear power spectrum
[out]	lgkk	vector of vectors containing the log(k) at each redshift
[out]	lgPk	vector of vectors containing the log(P(k)) at each redshift
[in]	redshift	vector of redshifts
[in]	store_output	if true the output files created are stored; if false the output files created are removed
[in]	output_root	output_root of the parameter file used to compute the power spectrum; it can be any name. If this parameter is different from the default value it will be used also in the output directory name
[in]	k_max	maximum wave vector module up to which the power spectrum is computed
[in]	file_par	name of the parameter file; if a parameter file is provided (i.e. file_par!=NULL), it will be used, ignoring the cosmological parameters of the object

Definition at line 290 of file PkXi.cpp.

◆ Table_XiCodes()

void cbl::cosmology::Cosmology::Table_XiCodes	(	const std::string	code,
		const bool	NL,
		std::vector< double > &	rr,
		std::vector< double > &	xi,
		const double	redshift,
		const bool	store_output,
		const std::string	output_root,
		const double	k_max,
		std::string	file_par
	)		const

write or read the table where the dark matter two-point correlation function is stored

Parameters

[in]	code	method used to compute the power spectrum; valid codes are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
[in]	NL	0 \(\rightarrow\) linear power spectrum; 1 \(\rightarrow\) non-linear power spectrum
[out]	rr	vector of comoving separations
[out]	xi	vector of the binned values of ξ(r)
[in]	redshift	redshift
[in]	store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
[in]	output_root	output_root of the parameter file used to compute the power spectrum; it can be any name. If this parameter is different from the default value it will be used also in the output directory name
[in]	k_max	maximum wave vector module up to which the power spectrum is computed
[in]	file_par	name of the parameter file; if a parameter file is provided (i.e. file_par!=NULL), it will be used, ignoring the cosmological parameters of the object

Definition at line 1164 of file PkXi.cpp.

◆ tau()

double cbl::cosmology::Cosmology::tau ( ) const

inline

get the private member Cosmology::m_tau

Returns: τ the Thomson scattering optical depth due to reionization

Definition at line 1281 of file Cosmology.h.

◆ type_NG()

int cbl::cosmology::Cosmology::type_NG ( ) const

inline

get the private member Cosmology::m_type_NG

Returns: the non-Gaussian shape (type=1 local, type=2 equilateral, type=3 enfolded, type=4 orthogonal)

Definition at line 1273 of file Cosmology.h.

◆ unevolved_mass_function()

double cbl::cosmology::Cosmology::unevolved_mass_function ( const double mass_accr ) const

the unevolved mass function

Author: Carlo Giocoli; cgioc.nosp@m.oli@.nosp@m.gmail.nosp@m..com

Parameters

mass_accr mass accreted

Returns: the unevolved mass function

Definition at line 579 of file MassFunction.cpp.

◆ unit()

bool cbl::cosmology::Cosmology::unit ( ) const

inline

get the private member Cosmology::m_unit

Returns: unit: false \(\rightarrow\) quantities are provided in phyical units; true \(\rightarrow\) quantities are provided in cosmological units (i.e. in units of h, e.g. Mpc/h)

Definition at line 1338 of file Cosmology.h.

◆ value()

double cbl::cosmology::Cosmology::value ( const CosmologicalParameter parameter ) const

get the private member specified by the enum CosmologicalParameter

Parameters

parameter the cosmological parameter

Returns: value of the cosmological parameter

Definition at line 319 of file Cosmology.cpp.

◆ Volume() [1/3]

double cbl::cosmology::Cosmology::Volume	(	const double	z1,
		const double	z2,
		const double	Area
	)		const

comoving volume for a given redshift range and sky area

this function provides an approximated expression of the comoving volume valid only for a ΛCDM model

Parameters

z1	minimum redshift
z2	maximum redshift
Area	sky area [square degrees]

Returns: comoving volume [m_unit=true \(\rightarrow (\mbox{Mpc}/h)^3\); m_unit=false \(\rightarrow \mbox{Mpc}^3\)]

Definition at line 1183 of file Cosmology.cpp.

◆ Volume() [2/3]

double cbl::cosmology::Cosmology::Volume	(	const double	z1,
		const double	z2,
		const double	RA_min,
		const double	RA_max,
		const double	Dec_min,
		const double	Dec_max
	)		const

comoving volume for a given redshift range and R.A.-Dec limits

this function provides an approximated expression of the comoving volume valid only for a ΛCDM model

Parameters

z1	minimum redshift
z2	maximum redshift
RA_min	minimum Right ascension [radians]
RA_max	maximum Right ascension [radians]
Dec_min	minimum Declination [radians]
Dec_max	minimum Declination [radians]

Returns: comoving volume [m_unit=true \(\rightarrow (\mbox{Mpc}/h)^3\); m_unit=false \(\rightarrow \mbox{Mpc}^3\)]

Definition at line 1194 of file Cosmology.cpp.

◆ Volume() [3/3]

double cbl::cosmology::Cosmology::Volume ( const double zz ) const

total comoving volume from z=0 to z

from Hogg 2000, Eq. 29

Author: Alfonso Veropalumbo; alfon.nosp@m.so.v.nosp@m.eropa.nosp@m.lumb.nosp@m.o@uni.nosp@m.bo.i.nosp@m.t

Parameters

zz redshift

Returns: comoving volume [m_unit=true \(\rightarrow (\mbox{Mpc}/h)^3\); m_unit=false \(\rightarrow \mbox{Mpc}^3\)]

Definition at line 1205 of file Cosmology.cpp.

◆ w0()

double cbl::cosmology::Cosmology::w0 ( ) const

inline

get the private member Cosmology::m_w0

Returns: w₀: one of the parameters of the dark energy equation of state (CPL parameterisation)

Definition at line 1242 of file Cosmology.h.

◆ w_CPL()

double cbl::cosmology::Cosmology::w_CPL ( const double redshift = 0. ) const

the DE equation of state in the CPL parameterisation, as a function of redshift

Parameters

redshift the redshift

Returns: w: the DE equation of state in the CPL parameterisation

Definition at line 535 of file Cosmology.cpp.

◆ wa()

double cbl::cosmology::Cosmology::wa ( ) const

inline

get the private member Cosmology::m_wa

Returns: w_a: one of the parameters of the dark energy equation of state (CPL parameterisation)

Definition at line 1250 of file Cosmology.h.

◆ wf()

double cbl::cosmology::Cosmology::wf	(	const double	mm,
		const double	redshift,
		const double	ff,
		const double	zf,
		const std::string	method_SS,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`
	)		const

rescaled variable w as in Lacey and Coles 1993

this functions provides the conditional variable w=[δ_c(zf) - δ_c(z)] / √ [s(fm)-s(m)] whereδ_c(z) = δ_c0(z)/D+(z)

Author: Carlo Giocoli; cgioc.nosp@m.oli@.nosp@m.gmail.nosp@m..com

Parameters

mm	halo mass
redshift	the redshift
ff	assembled fraction
zf	redshift at which the mass is accreted
method_SS	method used to compute the power spectrum and σ(mass); valid method_SS are: CAMB [http://camb.info/], CLASS [http://class-code.net/], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name

Returns: the conditional variable w

Definition at line 153 of file MassGrowth.cpp.

◆ wp_DM()

double cbl::cosmology::Cosmology::wp_DM	(	const double	rp,
		const std::string	method_Pk,
		const bool	NL,
		const double	redshift,
		const double	pimax,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const int	norm = `-1`,
		const double	r_min = `1.e-3`,
		const double	r_max = `350.`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	aa = `0.`,
		const bool	GSL = `false`,
		const double	prec = `1.e-2`,
		const std::string	file_par = `cbl::par::defaultString`
	)

the dark matter projected correlation function

this function provides the dark matter projected correlation functions, obtained by Fourier transforming the matter power spectrum

Parameters

rp	r_p: projected separation
method_Pk	method used to compute the power spectrum (i.e. the Boltzmann solver); valid choices for method_Pk are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
NL	false \(\rightarrow\) linear DM two-point correlation function; true \(\rightarrow\) non-linear DM two-point correlation function
redshift	the redshift
pimax	the upper limit of the line-of-sight integration
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
r_min	minimum separation up to which the correlation function is computed
r_max	maximum separation up to which the correlation function is computed
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed
aa	parameter a of Eq. 24 of Anderson et al. 2012
GSL	false \(\rightarrow\) FFTlog is used; true \(\rightarrow\) the GSL libraries are used
prec	accuracy of the integration
file_par	name of the parameter file; if a parameter file is provided (i.e. file_par!=NULL), it will be used, ignoring the cosmological parameters of the object

Returns: w_p,DM(θ): the projected correlation function of dark matter

Definition at line 1614 of file PkXi.cpp.

◆ wtheta_DM() [1/2]

double cbl::cosmology::Cosmology::wtheta_DM	(	const double	theta,
		const std::vector< double >	kk,
		const std::vector< double >	Pk,
		const std::vector< double >	zz,
		const std::vector< double >	nz,
		const std::vector< double >	phiz,
		const std::string	interpolationType = `"Spline"`,
		const CoordinateUnits	coordUnits = `CoordinateUnits::_degrees_`,
		const bool	GSL = `false`,
		const double	redshift_Pk = `0`
	)

the dark matter angular two-point correlation function

this function provides the dark matter angular correlation function, obtained by integrating the 2PCF using Limber approximation (see Sawangwit et al. 2011, eqs. 14,15):

\[ w(\theta) = \frac{\int_{z_{min}}^{z_{max}} \mathrm{d}z_1 \int_{z_{min}}^{z_{max}} \mathrm{d}z_2 f(z_1) f(z_2) \xi(r,z)} { \left\{ \int_{z_{min}}^{z_{max}} f(z) dz \right\}^2} \]

where \( r = \sqrt{\chi(z_1)^2+\chi(z_2)^2 -2\chi(z_1)\chi(z_2)\cos(\theta)} \), \(\chi\) is the comoving distance and \(z = (z_1+z_2)/2 \).

The function \(f(z)\) is the number of objects per unitar volume:

\[ f(z) = \frac{\mathrm{d}V}{\mathrm{d}z \mathrm{d\Omega}} n(z) \phi(z) \]

where \(\frac{\mathrm{d}V}{\mathrm{d}z \mathrm{d\Omega}}\) is the comoving volume element, \(n(z)\) is the comoving number density and \(\phi(z)\) is the selection function

Parameters

theta	the angular separation
kk	the wave vector module
Pk	linear power spectrum
zz	the redshift range
nz	the comoving number density
phiz	the selection function
interpolationType	the method in interpolation
coordUnits	the angular separation units
GSL	false \(\rightarrow\) FFTlog is used; true \(\rightarrow\) the GSL libraries are used
redshift_Pk	the redshift of the input power spectrum

Returns: \(w_{DM}(\theta)\): the angular two point correlation function of dark matter

Definition at line 2559 of file PkXi.cpp.

◆ wtheta_DM() [2/2]

double cbl::cosmology::Cosmology::wtheta_DM	(	const double	theta,
		const std::vector< double >	zz,
		const std::vector< double >	phiz,
		const std::string	interpolationMethod,
		const CoordinateUnits	coordUnits = `CoordinateUnits::_degrees_`,
		const bool	GSL = `false`,
		const std::string	method_Pk = `"CAMB"`,
		const bool	NL = `false`,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const int	norm = `-1`,
		const double	k_min = `1.e-4`,
		const double	k_max = `100`,
		const double	prec = `1.e-2`,
		const std::string	file_par = `par::defaultString`
	)

the dark matter angular two-point correlation function

this function provides the dark matter angular correlation function, obtained by integrating the 2PCF using Limber approximation (see Salazar et al. 2014, eqs. 5-8):

\[ w(\theta) = \int_{z_{min}}^{z_{max}} \mathrm{d}z_1 \int_{z_{min}}^{z_{max}} \mathrm{d}z_2 \phi(z_1) \phi(z_2) \xi(r,z) \]

where \( r = \sqrt{\chi(z_1)^2+\chi(z_2)^2 -2\chi(z_1)\chi(z_2)\cos(\theta)} \), \(\chi\) is the comoving distance and \(z = (z_1+z_2)/2 \)

Parameters

theta	the angular separation
zz	the redshift range
phiz	the number density
interpolationMethod	the method in interpolation
coordUnits	the angular separation units
GSL	false \(\rightarrow\) FFTlog is used; true \(\rightarrow\) the GSL libraries are used
method_Pk	method used to compute the power spectrum (i.e. the Boltzmann solver); valid choices for method_Pk are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
NL	0 \(\rightarrow\) linear power spectrum; 1 \(\rightarrow\) non-linear power spectrum
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
norm	0 \(\rightarrow\) don't normalize the power spectrum; 1 \(\rightarrow\) normalize the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
prec	accuracy of the integration
file_par	name of the parameter file; if a parameter file is provided (i.e. file_par!=NULL), it will be used, ignoring the cosmological parameters of the object

Returns: \(w_{DM}(\theta)\): the angular two point correlation function of dark matter

Definition at line 2495 of file PkXi.cpp.

◆ xi0_Kaiser() [1/2]

double cbl::cosmology::Cosmology::xi0_Kaiser	(	const double	rad,
		const double	f_sigma8,
		const double	bias_sigma8,
		const std::string	method_Pk,
		const double	redshift,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const bool	xiType = `0`,
		const double	k_star = `-1.`,
		const bool	NL = `false`,
		const int	norm = `-1`,
		const double	r_min = `0.1`,
		const double	r_max = `150.`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	aa = `0.`,
		const bool	GSL = `false`,
		const double	prec = `1.e-2`,
		const std::string	file_par = `par::defaultString`
	)

monopole of the redshift-space two-point correlation function in the Kaiser limit

this function provides the monopole of the two-point correlation function of biased tracers, predicted at large scales in the Kaiser limit:

\[ \xi_0(s) = \xi_{DM}(s)\left(\frac{b\sigma_8}{\sigma_8}\right)^2 \left[ 1 + \frac{2}{3}\frac{f\sigma_8}{b\sigma_8} + \frac{1}{5}\left(\frac{f\sigma_8}{b\sigma_8}\right)^2 \right] \]

The Kaiser factor \( \left[ 1 + \frac{2}{3}\frac{f\sigma_8}{b\sigma_8} + \frac{1}{5}\left(\frac{f\sigma_8}{b\sigma_8}\right)^2 \right] \) is computed by cbl::xi_ratio

Parameters

rad	comoving separation
f_sigma8	f*σ₈
bias_sigma8	b*σ₈
method_Pk	method used to compute the power spectrum and σ(mass) (i.e. the Boltzmann solver); valid choices for method_Pk are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
redshift	the redshift
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
xiType	0 \(\rightarrow\) standard; 1 \(\rightarrow\) Chuang & Wang model
k_star	k_* of the Chuang & Wang model
NL	false \(\rightarrow\) linear power spectrum; true \(\rightarrow\) non-linear power spectrum
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
r_min	minimum separation up to which the correlation function is computed
r_max	maximum separation up to which the correlation function is computed
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed
aa	parameter a of Eq. 24 of Anderson et al. 2012
GSL	true \(\rightarrow\) the GSL libraries are used
prec	accuracy of the integration
file_par	name of the parameter file; if a parameter file is provided (i.e. file_par!=NULL), it will be used, ignoring the cosmological parameters of the object

Returns: ξ₀

Definition at line 46 of file PkXizSpace.cpp.

◆ xi0_Kaiser() [2/2]

std::vector< double > cbl::cosmology::Cosmology::xi0_Kaiser	(	const std::vector< double >	rad,
		const double	bias,
		const std::string	method_Pk,
		const double	redshift,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const bool	NL = `false`,
		const int	norm = `-1`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`,
		const std::string	file_par = `par::defaultString`
	)

monopole of the redshift-space two-point correlation function in the Kaiser limit

this function provides the monopole of the two-point correlation function of biased tracers, predicted at large scales in the Kaiser limit:

\[ \xi_0(s) = \xi_{DM}(s)b^2\left[1 + \frac{2\beta}{3} + \frac{\beta^2}{5}\right] \]

where \( \beta=\beta(z)=\frac{f(z)}{b(z)} \). The Kaiser factor \( \left[1 + \frac{2\beta}{3} + \frac{\beta^2}{5}\right] \) is computed by cbl::xi_ratio, while the linear growth rate \( f(z) \) is computed by cbl::cosmology::Cosmology::linear_growth_rate

Parameters

rad	comoving separations
bias	b
method_Pk	method used to compute the power spectrum and σ(mass) (i.e. the Boltzmann solver); valid choices for method_Pk are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
redshift	the redshift
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
NL	false \(\rightarrow\) linear power spectrum; true \(\rightarrow\) non-linear power spectrum
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed
prec	accuracy of the integration
file_par	name of the parameter file; if a parameter file is provided (i.e. file_par!=NULL), it will be used, ignoring the cosmological parameters of the object

Returns: ξ₀

Definition at line 62 of file PkXizSpace.cpp.

◆ xi2D_CW()

double cbl::cosmology::Cosmology::xi2D_CW	(	const double	rp,
		const double	pi,
		const double	beta,
		const double	bias_lin,
		const double	bA,
		const double	sigmav0,
		const double	cmu,
		const double	cs1,
		const double	cs2,
		const double	redshift,
		std::vector< double >	rr1,
		std::vector< double >	Xi1,
		std::vector< double >	rr2,
		std::vector< double >	Xi2,
		std::vector< double > &	Xi1_,
		std::vector< double > &	Xi1__,
		std::vector< double > &	Xi2_,
		std::vector< double > &	Xi2__,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const bool	BAO = `1`,
		const bool	xiType = `0`,
		const double	k_star = `-1`,
		const bool	xiNL = `0`,
		const double	r_min = `0.1`,
		const double	r_max = `150.`,
		const double	v_min = `-3000.`,
		const double	v_max = `3000.`,
		const int	step_v = `500`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	x_min = `-3000.`,
		const double	x_max = `3000.`,
		const int	step_x = `500`,
		const double	aa = `0.`,
		const bool	GSL = `false`,
		const double	prec = `1.e-2`,
		const std::string	file_par = `par::defaultString`
	)

2D correlation function, ξ(r_p,π), predicted by the Chuang & Wang model

Parameters

rp	r_p: the comoving separation perpendicular to the line-of-sight
pi	π: the comoving separation parallel to the line-of-sight
beta	β=f/b, where f is the linear growth rate and b is the bias
bias_lin	linear bias
bA	b_a non-linear bias parameter
sigmav0	σ₀(v): parameter of the velocity distribution function, f(v)
cmu	parameter of the velocity distribution function, f(v)
cs1	parameter of the velocity distribution function, f(v)
cs2	parameter of the velocity distribution function, f(v)
redshift	the redshift
rr1	vector of r, the module of the comoving separation
Xi1	vector of ξ(r), the two-point correlation function of dark matter
rr2	vector of r, the module of the comoving separation
Xi2	vector of ξ(r), the two-point correlation function of dark matter
Xi1_	vector of barred ξ(r),
Xi1__	vector of double-barred ξ(r)
Xi2_	vector of barred ξ(r),
Xi2__	vector of double-barred ξ(r)
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
BAO	0 \(\rightarrow\) no BAO convolution; 1 \(\rightarrow\) BAO convolution
xiType	0 \(\rightarrow\) standard; 1 \(\rightarrow\) Chuang & Wang model
k_star	k_* of the Chuang & Wang model
xiNL	0 \(\rightarrow\) linear power spectrum; 1 \(\rightarrow\) non-linear power spectrum
r_min	minimum separation up to which the correlation function is computed
r_max	maximum separation up to which the correlation function is computed
v_min	minimum velocity used in the convolution of the correlation function
v_max	maximum velocity used in the convolution of the correlation function
step_v	number of steps used in the convolution of the correlation function
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed
x_min	minimum velocity used in the integral of the Chuang & Wang model
x_max	maximum velocity used in the integral of the Chuang & Wang model
step_x	number of steps in the integral of the Chuang & Wang model
aa	parameter a of Eq. 24 of Anderson et al. 2012
GSL	true \(\rightarrow\) the GSL libraries are used
prec	accuracy of the integration
file_par	name of the parameter file; if a parameter file is provided (i.e. file_par!=NULL), it will be used, ignoring the cosmological parameters of the object

Returns: ξ(r_p,π)

Definition at line 187 of file PkXizSpace.cpp.

◆ xi2D_dispersionModel()

double cbl::cosmology::Cosmology::xi2D_dispersionModel	(	const double	rp,
		const double	pi,
		const double	f_sigma8,
		const double	bias_sigma8,
		const double	sigmav,
		const std::string	method_Pk,
		const double	redshift,
		const int	FV,
		const bool	NL,
		std::vector< double >	rr,
		std::vector< double > &	Xi,
		std::vector< double > &	Xi_,
		std::vector< double > &	Xi__,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const int	index = `-1`,
		const bool	bias_nl = `0`,
		const double	bA = `-1.`,
		const bool	xiType = `0`,
		const double	k_star = `-1.`,
		const bool	xiNL = `0`,
		const double	v_min = `-3000.`,
		const double	v_max = `3000.`,
		const int	step_v = `500`,
		const int	norm = `-1`,
		const double	r_min = `0.1`,
		const double	r_max = `150.`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	aa = `0.`,
		const bool	GSL = `false`,
		const double	prec = `1.e-2`,
		const std::string	file_par = `par::defaultString`
	)

2D correlation function, ξ(r_p,π), predicted by the dispersion model

Parameters

rp	r_p: the comoving separation perpendicular to the line-of-sight
pi	π: the comoving separation parallel to the line-of-sight
f_sigma8	f*σ₈
bias_sigma8	b*σ₈
sigmav	σ₁₂: pairwise peculiar velocity dispersion
method_Pk	method used to compute the power spectrum and σ(mass) (i.e. the Boltzmann solver); valid choices for method_Pk are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
redshift	the redshift
FV	0 \(\rightarrow\) exponential form for f(v); 1 \(\rightarrow\) Gaussian form for f(v); where f(v) is the velocity distribution function
NL	0 \(\rightarrow\) linear power spectrum; 1 \(\rightarrow\) non-linear power spectrum
rr	vector of r, the module of the comoving separation
Xi	vector of ξ(r), the two-point correlation function of dark matter
Xi_	vector of barred ξ(r),
Xi__	vector of double-barred ξ(r)
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
index	internal parameter used when minimizing the χ₂
bias_nl	0 \(\rightarrow\) linear bias; 1 \(\rightarrow\) non-linear bias
bA	b_a non-linear bias parameter
xiType	0 \(\rightarrow\) standard; 1 \(\rightarrow\) Chuang & Wang model
k_star	k_* of the Chuang & Wang model
xiNL	0 \(\rightarrow\) linear power spectrum; 1 \(\rightarrow\) non-linear power spectrum
v_min	minimum velocity used in the convolution of the correlation function
v_max	maximum velocity used in the convolution of the correlation function
step_v	number of steps used in the convolution of the correlation function
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
r_min	minimum separation up to which the correlation function is computed
r_max	maximum separation up to which the correlation function is computed
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed
aa	parameter a of Eq. 24 of Anderson et al. 2012
GSL	true \(\rightarrow\) the GSL libraries are used
prec	accuracy of the integration
file_par	name of the parameter file; if a parameter file is provided (i.e. file_par!=NULL), it will be used, ignoring the cosmological parameters of the object

Returns: ξ(r_p,π)

Definition at line 81 of file PkXizSpace.cpp.

◆ xi_matter()

double cbl::cosmology::Cosmology::xi_matter	(	const double	rr,
		const std::string	method_Pk,
		const bool	NL,
		const double	redshift,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const int	norm = `-1`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	aa = `0.`,
		const bool	GSL = `false`,
		const double	prec = `1.e-2`,
		const std::string	file_par = `par::defaultString`
	)

the dark matter two-point correlation function

this function provides the dark matter correlation function, obtained by Fourier transforming the matter power spectrum

Parameters

rr	the module of the comoving separation
method_Pk	method used to compute the power spectrum (i.e. the Boltzmann solver); valid choices for method_Pk are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
NL	false \(\rightarrow\) linear DM two-point correlation function; true \(\rightarrow\) non-linear DM two-point correlation function
redshift	the redshift
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
aa	parameter a of Eq. 24 of Anderson et al. 2012
GSL	false \(\rightarrow\) FFTlog is used; true \(\rightarrow\) the GSL libraries are used
prec	accuracy of the integration
file_par	name of the parameter file; if a parameter file is provided (i.e. file_par!=NULL), it will be used, const ignoring the cosmological parameters of the object

Returns: ξ_DM(r): the spherically averaged (monopole) of the two-point correlation function of dark matter

Definition at line 1509 of file PkXi.cpp.

◆ xi_matter_DeWiggle()

double cbl::cosmology::Cosmology::xi_matter_DeWiggle	(	const double	rr,
		const double	redshift,
		const double	sigma_NL,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const bool	norm = `1`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	aa = `1.`,
		const double	prec = `1.e-2`
	)

the dark matter two-point correlation function, de-wiggled (see e.g. Anderson et al 2014)

this function provides the dark matter correlation function, obtained by Fourier transforming the De-Wiggled matter power spectrum

Author: Alfonso Veropalumbo; alfon.nosp@m.so.v.nosp@m.eropa.nosp@m.lumb.nosp@m.o@uni.nosp@m.bo.i.nosp@m.t

Parameters

rr	the module of the comoving separation
redshift	the redshift
sigma_NL	the non linear BAO damping
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
norm	0 \(\rightarrow\) don't normalise the power spectrum; 1 \(\rightarrow\) normalise the power spectrum; -1 \(\rightarrow\) normalise only if sigma8 is set
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
aa	parameter a of Eq. 24 of Anderson et al. 2012
prec	accuracy of the integration

Returns: ξ_DW(r): the De-Wiggled spherically averaged (monopole) of the two-point correlation function of dark matter

Definition at line 2209 of file PkXi.cpp.

◆ xi_r_n()

void cbl::cosmology::Cosmology::xi_r_n	(	std::vector< double > &	xi_n,
		const std::vector< double >	rr,
		const int	nn,
		const std::vector< double >	kk,
		const std::vector< double >	Pk
	)

compute the power spectrum integral transform

this function computes the power spectrum integral transform:

\[ \xi^{[n]} (r) = \int \frac{k^2\mathrm{d}k}{2\pi^2} P(k) j_n(kr). \]

where n is the order of the transform.

Parameters

xi_n	the power spectrum transform \(\xi^{[n]} (r)\)
rr	vector of scales
nn	the order of the transform
kk	vector of wavevector modules
Pk	dark matter power spectrum

Definition at line 793 of file 3PCF.cpp.

◆ xi_r_n_pm()

void cbl::cosmology::Cosmology::xi_r_n_pm	(	std::vector< double > &	xi_n_p,
		std::vector< double > &	xi_n_m,
		const std::vector< double >	rr,
		const int	nn,
		const std::vector< double >	kk,
		const std::vector< double >	Pk
	)

compute the power spectrum integral transform

this function computes the power spectrum integral transform:

\[ \xi^{[n\pm]} (r) = \int \frac{k^2\mathrm{d}k}{2\pi^2} k^{\pm1} P(k) j_n(kr) \]

where n is the order of the transform.

Parameters

xi_n_p	the power spectrum transform \(\xi^{[n+]} (r)\)
xi_n_m	the power spectrum transform \(\xi^{[n-]} (r)\)
rr	vector of scales
nn	the order of the transform
kk	vector of wavevector modules
Pk	dark matter power spectrum

Definition at line 802 of file 3PCF.cpp.

◆ xi_star()

double cbl::cosmology::Cosmology::xi_star	(	const double	rr,
		const double	redshift,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const double	k_star = `-1.`,
		const double	k_min = `0.001`,
		const double	k_max = `100.`,
		const double	prec = `1.e-2`,
		const std::string	file_par = `par::defaultString`
	)

the function ξ_* of the Chuang & Wang 2012 model

see Chuang & Wang 2012, 1209.0210

Parameters

rr	comoving separation
redshift	the redshift
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
k_star	k_* of the Chuang & Wang model
k_min	minimum wave vector module up to which the power spectrum is computed in order to estimate the power spectrum normalisation; this parameter is used only if either norm=1, or norm=-1 and sigma8 is set
k_max	maximum wave vector module up to which the power spectrum is computed
prec	accuracy of the integration
file_par	name of the parameter file; if a parameter file is provided (i.e. file_par!=NULL), it will be used, ignoring the cosmological parameters of the object

Returns: ξ_*

Definition at line 122 of file PkXizSpace.cpp.

◆ XiMonopole_covariance()

std::vector< std::vector< double > > cbl::cosmology::Cosmology::XiMonopole_covariance	(	const int	nbins,
		const double	rMin,
		const double	rMax,
		const double	nn,
		const double	Volume,
		const std::vector< double >	kk,
		const std::vector< double >	Pk0,
		const int	IntegrationMethod = `1`
	)

the covariance matrix of the first three non-null multipoles of the two-point correlation function

Parameters

nbins	the number of bins of the two-point correlation function multipoles
rMin	the minimum scale
rMax	the maximum scale
nn	order of the moment
Volume	the volume
kk	vector containing the wave vector modules
Pk0	vector containing the monopole of the power spectrum
IntegrationMethod	the integration method

Returns: the covariance matrix of the first three non-null multipoles of the two-point correlation function

Definition at line 2235 of file PkXi.cpp.

◆ XiMultipoles()

std::vector< std::vector< double > > cbl::cosmology::Cosmology::XiMultipoles	(	const int	nbins,
		const double	rMin,
		const double	rMax,
		const std::vector< double >	kk,
		const std::vector< double >	Pk0,
		const std::vector< double >	Pk2,
		const std::vector< double >	Pk4,
		const int	IntegrationMethod = `1`
	)

the first three non-null multipoles of the two-point correlation function

Parameters

nbins	the number of bins of the two-point correlation function multipoles
rMin	the minimum scale
rMax	the maximum scale
kk	vector containing the wave vector modules
Pk0	vector containing the monopole of the power spectrum
Pk2	vector containing the quadrupole of the power spectrum
Pk4	vector containing the hexadecapole of the power spectrum
IntegrationMethod	the integration method

Returns: the matrix containing the first three non-null multipoles of the two-point correlation function

Definition at line 2403 of file PkXi.cpp.

◆ XiMultipoles_covariance()

std::vector< std::vector< double > > cbl::cosmology::Cosmology::XiMultipoles_covariance	(	const int	nbins,
		const double	rMin,
		const double	rMax,
		const double	nn,
		const double	Volume,
		const std::vector< double >	kk,
		const std::vector< double >	Pk0,
		const std::vector< double >	Pk2,
		const std::vector< double >	Pk4,
		const int	IntegrationMethod = `1`
	)

the covariance matrix of the first three non-null multipole moments of the two-point correlation function

Parameters

nbins	the number of bins of the two-point correlation function multipoles
rMin	the minimum scale
rMax	the maximum scale
nn	order of the moment
Volume	the volume
kk	vector containing the wave vector modules
Pk0	vector containing the monopole of the power spectrum
Pk2	vector containing the quadrupole of the power spectrum
Pk4	vector containing the hexadecapole of the power spectrum
IntegrationMethod	the integration method

Returns: the covariance matrix of the first three non-null multipole moments of the two-point correlation function

Definition at line 2311 of file PkXi.cpp.

◆ xis_gBAO()

double cbl::cosmology::Cosmology::xis_gBAO	(	const double	rp,
		const double	pi,
		const double	f_sigma8,
		const double	bias_sigma8,
		const double	redshift,
		std::vector< double >	rr,
		std::vector< double >	Xi,
		std::vector< double > &	Xi_,
		std::vector< double > &	Xi__,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const double	k_star = `-1.`,
		const double	x_min = `-3000.`,
		const double	x_max = `3000.`,
		const int	step_x = `500`
	)

the function ξ_g,BAO(s) of the Chuang & Wang 2012 model

see Chuang & Wang 2012, 1209.0210

Parameters

rp	r_p: the comoving separation perpendicular to the line-of-sight
pi	π: the comoving separation parallel to the line-of-sight
f_sigma8	f*σ₈
bias_sigma8	b*σ₈
redshift	the redshift
rr	vector of r, the module of the comoving separation
Xi	vector of ξ(r), the two-point correlation function of dark matter
Xi_	vector of barred ξ(r),
Xi__	vector of double-barred ξ(r)
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
k_star	k_* of the Chuang & Wang model
x_min	minimum velocity used in the integral of the Chuang & Wang model
x_max	maximum velocity used in the integral of the Chuang & Wang model
step_x	number of steps in the integral of the Chuang & Wang model

Returns: ξ_g,BAO(s)

Definition at line 156 of file PkXizSpace.cpp.

◆ xisnl_gnw()

double cbl::cosmology::Cosmology::xisnl_gnw	(	const double	rp,
		const double	pi,
		const double	f_sigma8,
		const double	bias_sigma8,
		const double	bA,
		const double	redshift,
		std::vector< double >	rr,
		std::vector< double >	Xi,
		std::vector< double > &	Xi_,
		std::vector< double > &	Xi__,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`
	)

the function ξ_g,nw(s) of the Chuang & Wang 2012 model

see Chuang & Wang 2012, 1209.0210

Parameters

rp	r_p: the comoving separation perpendicular to the line-of-sight
pi	π: the comoving separation parallel to the line-of-sight
f_sigma8	f*σ₈
bias_sigma8	b*σ₈
bA	b_a non-linear bias parameter
redshift	the redshift
rr	vector of r, the module of the comoving separation
Xi	vector of ξ(r), the two-point correlation function of dark matter
Xi_	vector of barred ξ(r),
Xi__	vector of double-barred ξ(r)
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name

Returns: ξ_g,nw(s)

Definition at line 145 of file PkXizSpace.cpp.

◆ ys()

double cbl::cosmology::Cosmology::ys	(	const double	redshift,
		const std::string	method_Pk,
		const double	T_CMB = `par::TCMB`
	)		const

the fiducial cosmology independent ratio r_s/D_V, valid choices for method_Pk are: EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html], CAMB [http://camb.info/]

both r_s and D_V are in Mpc

Author: Alfonso Veropalumbo; alfon.nosp@m.so.v.nosp@m.eropa.nosp@m.lumb.nosp@m.o@uni.nosp@m.bo.i.nosp@m.t

Parameters

redshift	the redshift
method_Pk	method used to compute the sound horizon (i.e. the Boltzmann solver)
T_CMB	CMB temperature

Returns: y_s

Definition at line 197 of file BAO.cpp.

◆ z_acc()

double cbl::cosmology::Cosmology::z_acc ( ) const

redshift at which the Universe begins to accelerate

see e.g. de Araujo 2005

Returns: z_acc

Definition at line 994 of file Cosmology.cpp.

◆ z_decoupling()

double cbl::cosmology::Cosmology::z_decoupling ( ) const

redshift at wich occurs baryon photon decoupling

see Hu & Sugiyama (1996)

Returns: z_dec

Definition at line 47 of file BAO.cpp.

◆ z_drag()

double cbl::cosmology::Cosmology::z_drag ( ) const

redshift of drag epoch

see Hu & Sugiyama (1996).

Returns: z_dec

Definition at line 62 of file BAO.cpp.

◆ z_eq()

double cbl::cosmology::Cosmology::z_eq ( ) const

redshift of matter-dark energy equality

see e.g. de Araujo 2005

Returns: z_eq

Definition at line 1008 of file Cosmology.cpp.

◆ z_eq_rad()

double cbl::cosmology::Cosmology::z_eq_rad ( const double T_CMB = 2.7255 ) const

redshift of matter-radiation equality

Parameters

T_CMB the temperature of the CMB

Returns: z_eq

Definition at line 1018 of file Cosmology.cpp.

◆ zeta_covariance()

std::vector< std::vector< double > > cbl::cosmology::Cosmology::zeta_covariance	(	const double	Volume,
		const double	nObjects,
		const std::vector< double >	theta,
		const double	r1,
		const double	r2,
		const double	deltaR,
		const std::vector< double >	kk,
		const std::vector< double >	Pk,
		const int	norders = `10`,
		const double	prec = `1.e-3`,
		const bool	method = `false`,
		const int	nExtractions = `10000`,
		const std::vector< double >	mean = `{}`,
		const int	seed = `543`
	)

the dark matter three-point correlation function covariance model

this function computes the dark matter three-point correlation function covariance model, by Slepian et al. 2015, as a function of \(\theta = r_1 \cdot r_2\):

\[ C(r_1, r_2, \vec{r_1}\cdot\vec{r_2} \equiv \cos(\theta) = \sum_{l=0}^{l=max_l} \sum_{l^'=0}^{l^'=max_l} C_{l, l^'}(r_1, r_2) P_l(\cos(\theta) P_{l^'}(\cos(theta) \]

where \(C_{l, l^'}(r_1, r_2)\) is computed by cbl::cosmology::Cosmology::zeta_multipoles_covariance

Parameters

Volume	the volume
nObjects	the number of objects
theta	vector of angles at which the covariance is computed
r1	the scale \(r_1\)
r2	the scale \(r_2\)
deltaR	the bin size, if non-positive, no bin average is computed
kk	vector of the wave vector modules
Pk	the pdark matter ower spectrum
norders	the maximum number of orders of multipoles of the three point correlation function expansion
prec	the integral precision
method	false \(\rightarrow\) apply method 1; true \(\rightarrow\) apply method 2
nExtractions	the number of mock extraction from zeta multipoles coefficient covariance matrix
mean	vector containing the mean values
seed	random number generator seed

Returns: the covariance of the dark matter three-point correlation function

Definition at line 753 of file 3PCF.cpp.

◆ zeta_DM()

std::vector< double > cbl::cosmology::Cosmology::zeta_DM	(	const double	r1,
		const double	r2,
		const std::vector< double >	theta,
		const std::string	model,
		const std::vector< double >	kk,
		const std::vector< double >	Pk_matter
	)		const

the dark matter three-point correlation function

this function computes the dark matter three-point correlation function with either the Slepian et al 2015 or the Barriga & Gatzagnaga 2002 model

Parameters

r1	the first side of the triangle
r2	the second side of the triangle
theta	vector containing angles between r1 and r2, in radians
model	the model to compute the three-point correlation function, can be "Slepian" or "BarrigaGatzanaga"
kk	vector of the wave vector modules
Pk_matter	the dark matter power spectrum

Returns: vector containing the dark matter three-point correlation function

Definition at line 446 of file 3PCF.cpp.

◆ zeta_DM_BarrigaGatzanaga()

double cbl::cosmology::Cosmology::zeta_DM_BarrigaGatzanaga	(	const double	r1,
		const double	r2,
		const double	theta,
		std::vector< double > &	rr,
		std::vector< double > &	xi_matter,
		std::vector< double > &	Phi,
		const std::vector< double >	kk,
		const std::vector< double >	Pk_matter
	)		const

the dark matter three-point correlation function model by Barriga & Gatzanaga et al. 2002

this functions computes the dark matter three-point correlation function model by Barriga & Gatzanaga et al 2002:

\[ f(r_1, r_2) = \frac{10}{7}\xi(r_1) \xi(r_2)+\frac{4}{7} \left\{ -3 \frac{\Phi^\prime(r_1) \Phi^\prime(r_2)}{r_1 r_2} -\frac{\xi(r1) \Phi^\prime(r_2)}{r_2}-\frac{\xi(r2) \Phi^\prime(r_1)}{r_1} +\mu^2\left[ \xi(r_1)+3\frac{\Phi^\prime(r_1)}{r1}\right]\left[ \xi(r_2)+3\frac{\Phi^\prime(r_2)}{r_3}\right] \right\} -\mu\left[ \xi^\prime(r_1)\Phi^\prime(r_2) + \xi^\prime(r_2)\Phi^\prime(r_1)\right] + \mathrm{permutations} \]

where the prime indicates the derivative with respect to \(r\), and \(\xi(r), \Phi(r)\) are the integrals of the power spectrum computed by cbl::cosmology::Cosmology::integrals_zeta_BarrigaGatzanaga.

Parameters

[in]	r1	the first side of the triangle
[in]	r2	the second side of the triangle
[in]	theta	the angle between r1 and r2
[out]	rr	vector or scales
[out]	xi_matter	vector containing the dark matter two-point correlation function
[out]	Phi	vector containing \( \Phi(r)\)
[in]	kk	vector of the wave vector modules
[in]	Pk_matter	the dark matter power spectrum

Returns: the dark matter three-point correlation function

Definition at line 387 of file 3PCF.cpp.

◆ zeta_DM_eq()

std::vector< double > cbl::cosmology::Cosmology::zeta_DM_eq	(	const std::vector< double >	rr,
		const std::string	model,
		const std::vector< double >	kk,
		const std::vector< double >	Pk_matter
	)		const

the dark matter equilateral three-point correlation function

this function computes the dark matter equilateral three-point correlation function with either the Slepian et al 2015 or the Barriga & Gatzagnaga 2002 model

Parameters

rr	vector of sides
model	the model to compute the three-point correlation function, can be "Slepian" or "BarrigaGatzanaga"
kk	vector of the wave vector modules
Pk_matter	the dark matter power spectrum

Returns: vector containing the dark matter three-point correlation function

Definition at line 558 of file 3PCF.cpp.

◆ zeta_DM_Slepian()

double cbl::cosmology::Cosmology::zeta_DM_Slepian	(	const double	r1,
		const double	r2,
		const double	theta,
		std::vector< double > &	rr,
		std::vector< double > &	xi_matter,
		std::vector< double > &	xi_matter_m1,
		std::vector< double > &	xi_matter_p1,
		std::vector< double > &	xi_matter_2,
		const std::vector< double >	kk,
		const std::vector< double >	Pk_matter,
		const int	norders = `9`,
		const double	prec = `1.e-3`
	)		const

the dark matter three-point correlation function model by Slepian et al. 2015

this function computes \(\zeta_{DM} (r_1, r_2, \hat{r_1} \cdot \hat{r_2})\), as described in Slepian et al. 2015:

\[ \zeta_{DM} (r_1, r_2, \hat{r_1} \cdot \hat{r_2}) = \sum_l \zeta_l(r_1, r_2) P_l(\hat{r_1} \cdot \hat{r_2}) .\]

The coefficients of the expansion are computed by cbl::cosmology::Cosmology::zeta_expansion_Slepian

Parameters

[in]	r1	the first side of the triangle
[in]	r2	the second side of the triangle
[in]	theta	the angle between r1 and r2
[out]	rr	vector or scales
[out]	xi_matter	vector containing the dark matter two-point correlation function
[out]	xi_matter_m1	vector containing \(\xi^{[1-]}_{DM}(r)\)
[out]	xi_matter_p1	vector containing \(\xi^{[1+]}_{DM}(r)\)
[out]	xi_matter_2	vector containing \(\xi^{[2]}_{DM}(r)\)
[in]	kk	vector of the wave vector modules
[in]	Pk_matter	the dark matter power spectrum
[in]	norders	the maximum number of orders
[in]	prec	the integral precision

Returns: the connected dark matter three-point correlation function

Definition at line 314 of file 3PCF.cpp.

◆ zeta_ell_0_factor()

double cbl::cosmology::Cosmology::zeta_ell_0_factor	(	const double	b1,
		const double	gamma,
		const double	beta
	)

the multiplicative factor for \( \zeta_0 \), with local bias

This function computes the multiplicative factor for \( \zeta_0 \), with local bias:

\[ l = 0 : b_1^3 \left( \frac{34}{21} \left[ 1+\frac{4}{3}\beta+\frac{1154}{1275}\beta^2+ \frac{936}{2975}\beta^3+\frac{21}{425}\beta^4\right]+ \gamma\left[ 1+\frac{2}{3}\beta+\frac{1}{9}\beta^2 \right ] \right) \]

with \(b_1\) the linear bias, \(\gamma\) the ratio of quadratic and linear bias, \(\gamma= 2 b_2 / b_1 \) and \( \beta = f/b_1 \) with \( f \) the linear growth rate

Parameters

b1	the linear bias
gamma	the ratio of quadratic and linear bias, \(\gamma= 2 b_2 / b_1 \),
beta	the kaiser factor \( \beta = f/b_1 \) with \( f \) the linear growth rate

Returns: the multiplicative factor for \( \zeta_0 \), with local bias

Definition at line 907 of file 3PCF.cpp.

◆ zeta_ell_0_factor_tidal()

double cbl::cosmology::Cosmology::zeta_ell_0_factor_tidal	(	const double	gamma_t,
		const double	beta
	)

the multiplicative factor for \( \zeta_l, l=0 \), with non-local bias

This function computes the multiplicative factor for \( \zeta_0 \), with non-local bias:

\[ l=0: \frac{16 \beta^2 \gamma_t} {675} \]

with \(\gamma_t\ = b_t/b_1\) the ratio between the tidal and the linear bias and \( \beta = f/b_1 \) with \( f \) the linear growth rate

Parameters

gamma_t	the ratio between the tidal and the linear bias
beta	the kaiser factor \( \beta = f/b_1 \) with \( f \) the linear growth rate

Returns: the multiplicative factor for \( \zeta_l, l=0 \), with non-local bias

Definition at line 916 of file 3PCF.cpp.

◆ zeta_ell_1_factor()

double cbl::cosmology::Cosmology::zeta_ell_1_factor	(	const double	b1,
		const double	beta
	)

the multiplicative factor for \( \zeta_1 \), with local bias

This function computes the multiplicative factor for \( \zeta_1 \), with local bias:

\[ l = 1 : -b_1^3 \left[ 1+\frac{4}{3}\beta+\frac{82}{75}\beta^2+\frac{12}{25}\beta^3+\frac{3}{35}\beta^5 \right] \]

with \(b_1\) the linear bias and \( \beta = f/b_1 \) with \( f \) the linear growth rate

Parameters

b1	the linear bias
beta	the kaiser factor \( \beta = f/b_1 \) with \( f \) the linear growth rate

Returns: the multiplicative factor for \( \zeta_1 \), with local bias

Definition at line 925 of file 3PCF.cpp.

◆ zeta_ell_2_factor()

double cbl::cosmology::Cosmology::zeta_ell_2_factor	(	const double	b1,
		const double	gamma,
		const double	beta
	)

the multiplicative factor for \( \zeta_2 \), with local bias

This function computes the multiplicative factor for \( \zeta_2 \), with local bias:

\[ l = 2 : b_1^3 \left( \frac{8}{21} \left[ 1+\frac{4}{3}\beta+\frac{52}{21}\beta^2 + \frac{81}{49}\beta^3 + \frac{12}{35}\beta^4\right]+\frac{32}{945}\gamma \beta^2 \right) \]

with \(b_1\) the linear bias, \(\gamma\) the ratio of quadratic and linear bias, \(\gamma= 2 b_2 / b_1 \) and \( \beta = f/b_1 \) with \( f \) the linear growth rate

Parameters

b1	the linear bias
gamma	the ratio of quadratic and linear bias, \(\gamma= 2 b_2 / b_1 \),
beta	the kaiser factor \( \beta = f/b_1 \) with \( f \) the linear growth rate

Returns: the multiplicative factor for \( \zeta_2 \), with local bias

Definition at line 934 of file 3PCF.cpp.

◆ zeta_ell_2_factor_tidal()

double cbl::cosmology::Cosmology::zeta_ell_2_factor_tidal	(	const double	gamma_t,
		const double	beta
	)

the multiplicative factor for \( \zeta_l, l=2 \), with non-local bias

This function computes the multiplicative factor for \( \zeta_2 \), with non-local bias:

\[ l=2: \frac{5}{2} \left(\frac{8}{15}+\frac{16\beta}{45}+\frac{344\beta^2}{4725} \right)\gamma_t \]

with \(\gamma_t\ = b_t/b_1\) the ratio between the tidal and the linear bias and \( \beta = f/b_1\) with \( f \) the linear growth rate

Parameters

gamma_t	the ratio between the tidal and the linear bias
beta	the kaiser factor \( \beta = f/b_1 \) with \( f \) the linear growth rate

Returns: the multiplicative factor for \( \zeta_l, l=2 \), with non-local bias

Definition at line 943 of file 3PCF.cpp.

◆ zeta_ell_3_factor()

double cbl::cosmology::Cosmology::zeta_ell_3_factor	(	const double	b1,
		const double	beta
	)

the multiplicative factor for \( \zeta_3 \), with local bias

This function computes the multiplicative factor for \( \zeta_3 \), with local bias:

\[ l=3: -b_1^3 \left[ \frac{8}{75}\beta^2+\frac{16}{175}\beta^3+\frac{8}{315}\beta^4 \right] \]

with \(b_1\) the linear bias and \( \beta = f/b_1 \) with \( f \) the linear growth rate

Parameters

b1	the linear bias
beta	the kaiser factor \( \beta = f/b_1 \) with \( f \) the linear growth rate

Returns: the multiplicative factor for \( \zeta_3 \), with local bias

Definition at line 952 of file 3PCF.cpp.

◆ zeta_ell_4_factor()

double cbl::cosmology::Cosmology::zeta_ell_4_factor	(	const double	b1,
		const double	beta
	)

the multiplicative factor for \( \zeta_4 \), with local bias

This function computes the multiplicative factor for \( \zeta_4 \), with local bias:

\[ l=4: -b_1^3 \left[ -\frac{32}{3675}\beta^2+\frac{32}{8575}\beta^3+\frac{128}{11025}\beta^4 \right] \]

with \( b_1\) the linear bias and \( \beta = f/b_1 \) with \( f \) the linear growth rate

Parameters

b1	the linear bias
beta	the kaiser factor \( \beta = f/b_1 \) with \( f \) the linear growth rate

Returns: the multiplicative factor for \( \zeta_4 \), with local bias

Definition at line 961 of file 3PCF.cpp.

◆ zeta_ell_4_factor_tidal()

double cbl::cosmology::Cosmology::zeta_ell_4_factor_tidal	(	const double	gamma_t,
		const double	beta
	)

the multiplicative factor for \( \zeta_l, l=4 \), with non-local bias

This function computes the multiplicative factor for \( \zeta_4 \), with non-local bias:

\[ l=4: \frac{32 \beta^2 \gamma_t} {525} \]

with \(\gamma_t\ = b_t/b_1\) the ratio between the tidal and the linear bias and \( \beta = f/b_1 \) with \( f \) the linear growth rate

Parameters

gamma_t	the ratio between the tidal and the linear bias
beta	the kaiser factor \( \beta = f/b_1\) with \( f \) the linear growth rate

Returns: the multiplicative factor for \( \zeta_l, l=4 \), with non-local bias

Definition at line 970 of file 3PCF.cpp.

◆ zeta_ell_k_factor()

double cbl::cosmology::Cosmology::zeta_ell_k_factor	(	const double	b1,
		const double	beta
	)

the multiplicative factor for \( \zeta_l, l>4 \), with local bias

This function computes the multiplicative factor for \( \zeta_k, l>4 \), with local bias:

\[ l>4: b_1^3(7\beta^2+3\beta^3) \]

with \(b_1\) the linear bias and \( \beta = f/b_1 \) with \( f \) the linear growth rate

Parameters

b1	the linear bias
beta	the kaiser factor \( \beta = f/b_1 \) with \( f \) the linear growth rate

Returns: the multiplicative factor for \( \zeta_l, l>4 \), with local bias

Definition at line 979 of file 3PCF.cpp.

◆ zeta_ell_precyclic()

double cbl::cosmology::Cosmology::zeta_ell_precyclic	(	const double	r1,
		const double	r2,
		const int	ell,
		const double	b1,
		const double	b2,
		const double	bt,
		const double	beta,
		std::vector< std::shared_ptr< glob::FuncGrid >>	interp_xi_ell,
		const bool	use_k,
		std::shared_ptr< glob::FuncGrid2D >	interp_k_ell
	)

the pre-cyclic \( \zeta_l \)

This function computes the legendre multipoles coefficients of the three-point correlation function using the tree-level expansion order of the biased and redshift space density field, as derived by Slepian&Eisenstein (2017) in configuration space, based on the work presented by Scoccimarro et al (1999) for the bispectrum.

The model is computed for a specific triangle configurations and order of the expansion given the biasing parameters and \(\beta\).

Parameters

r1	the first triangle side
r2	the second triangle side
ell	the order of the expansion
b1	the linear bias
b2	the quadratic bias
bt	the tidal bias
beta	the kaiser factor
interp_xi_ell	vector of interpolating function for terms \(\xi^{[n]}, \xi^{[n\pm]}\)
use_k	if true, use the \(k_l\) part of the model \(O(\beta^2)\)
interp_k_ell	interpolationg function for \( k_l\).

Returns: the pre-cyclic \( \zeta_l \)

Definition at line 988 of file 3PCF.cpp.

◆ zeta_expansion_Slepian()

std::vector< double > cbl::cosmology::Cosmology::zeta_expansion_Slepian	(	const double	r1,
		const double	r2,
		const double	b1,
		const double	b2,
		std::vector< double > &	rr,
		std::vector< double > &	xi_matter,
		std::vector< double > &	xi_matter_m1,
		std::vector< double > &	xi_matter_p1,
		std::vector< double > &	xi_matter_2,
		const int	norders = `9`,
		const double	prec = `1.e-3`
	)		const

the terms of the \(\zeta(r_1, r_2)\) expansion

this function computes the terms of the \(\zeta(r_1, r_2)\) expansion up to an arbitrary order \(l\) (the default value is \(l_{max}=9\)), as described in Slepian et al. 2015:

\[\zeta_l(r_1, r_2) = \frac{2l+1}{2} \int_{-1}^{1} \mathrm{d}\mu_{12} \left[\zeta_{pc}(r_1, r_2, \mu_{12})+\zeta_{pc}(r_2, r_3, \mu_{23})+ \zeta_{pc}(r_3, r_1, \mu_{31})\right] P_l(\mu_{12}) .\]

the terms in square brackets is computed by cbl::cosmology::Cosmology::zeta_precyclic_Slepian

Parameters

[in]	r1	the first side of the triangle
[in]	r2	the second side of the triangle
[in]	b1	the linear bias of the triangle
[in]	b2	the non-linear bias
[out]	rr	vector or scales
[out]	xi_matter	vector containing the dark matter two-point correlation function
[out]	xi_matter_m1	vector containing \(\xi^{[1-]}_{DM}(r)\)
[out]	xi_matter_p1	vector containing \(\xi^{[1+]}_{DM}(r)\)
[out]	xi_matter_2	vector containing \(\xi^{[2]}_{DM}(r)\)
[in]	norders	the maximum numbers of orders
[in]	prec	the integral precision

Returns: vector containing the terms of legendre expansion

Definition at line 291 of file 3PCF.cpp.

◆ zeta_halo()

std::vector< double > cbl::cosmology::Cosmology::zeta_halo	(	const double	r1,
		const double	r2,
		const std::vector< double >	theta,
		const double	b1,
		const double	b2,
		const std::string	model,
		const std::vector< double >	kk,
		const std::vector< double >	Pk_matter
	)		const

the local-bias model of the three-point correlation function of dark matter haloes

this function computes the three-point correlation function of dark matter haloes with either the Slepian et al. 2015 or the Barriga & Gatzagnaga 2002 model, as follows:

\[ \zeta_h (r_1, r_2, \hat{r_1} \cdot \hat{r_2}) = b_1^3 \zeta_{DM}(r_1, r_2, \hat{r_1} \cdot \hat{r_2}) + b_1^2 b_2 \left[ \xi(r_1)\cdot\xi(r_2) + \xi(r_2)\cdot\xi(r_3) + \xi(r_3)\cdot\xi(r_1) \right] \]

with \(r_3 = \sqrt{r_1^2+r_2^2-2 r_1 r_2 \cos(\theta)}\) and \(b_1, b_2\) the linear and non-linear halo bias, respectively; \(\zeta_{DM}\) is compute by cbl::cosmology::Cosmology::zeta_DM

Parameters

r1	the first side of the triangle
r2	the second side of the triangle
theta	vector containing angles between r1 and r2, in radians
b1	the linear bias
b2	the non-linear bias
model	the model to compute the three-point correlation function, can be "Slepian" or "BarrigaGatzanaga"
kk	vector of the wave vector modules
Pk_matter	the dark matter power spectrum

Returns: vector containing the three-point correlation function of dark matter haloes

Definition at line 499 of file 3PCF.cpp.

◆ zeta_multipoles_covariance()

double cbl::cosmology::Cosmology::zeta_multipoles_covariance	(	const double	Volume,
		const double	nObjects,
		const int	l,
		const int	l_prime,
		const double	r1,
		const double	r2,
		const double	r1_prime,
		const double	r2_prime,
		const double	deltaR,
		const std::vector< double >	kk,
		const std::vector< double >	Pk,
		const std::vector< double >	rr,
		const std::vector< double >	Xi,
		const double	prec = `1.e-3`
	)

the dark matter three-point correlation function multipoles covariance model, by Slepian et al. 2015

\[ C_{{\rm GRF}, ll'}(r_{1},r_{2};r_{1}',r_{2}')=\frac{4\pi}{V}(2l+1)(2l'+1)(-1)^{l+l'} \times\int r^{2}dr\sum_{l_{2}}(2l_{2}+1) \left(\begin{array}{ccc} l & l' & l_{2}\\ 0 & 0 & 0 \end{array}\right)^2\nonumber\\ \times\bigg\{(-1)^{l_2}\xi(r)\bigg[f_{l_{2}ll'}(r;r_{1},r_{1}')f_{l_{2}ll'}(r;r_{2},r_{2}') +f_{l_{2}ll'}(r;r_{2},r_{1}')f_{l_{2}ll'}(r;r_{1},r_{2}')\bigg]+(-1)^{(l+l'+l_{2})/2} \times\bigg[f_{ll}(r;r_{1})f_{l'l'}(r;r_{1}')f_{l_{2}ll'}(r;r_{2},r_{2}') +f_{ll}(r;r_{1})f_{l'l'}(r;r_{2}')f_{l_{2}ll'}(r;r_{2},r_{1}') +f_{ll}(r;r_{2})f_{l'l'}(r;r_{1}')f_{l_{2}ll'}(r;r_{1},r_{2}') +f_{ll}(r;r_{2})f_{l'l'}(r;r_{2}')f_{l_{2}ll'}(r;r_{1},r_{1}')\bigg]\bigg\} \]

with:

\[ f_{ll}(r;r_{1})=\int\frac{k^{2}dk}{2\pi^{2}}\left[P(k)+\frac{1}{n}\right]j_{l}(kr_{1})j_{l}(kr) \]

and:

\[ f_{l_{2}ll'}(r;r_{1},r_{1}')=\int\frac{k^{2}dk}{2\pi^{2}} \left[P(k)+\frac{1}{n}\right] j_{l}(kr_{1})j_{l'}(kr_{1}')j_{l_{2}}(kr), \]

where \(V\) is the effective survey volume, and \(n\) is the effective number density of the survey.

Parameters

Volume	the volume
nObjects	the number of objects
l	the order l of the multipoles expansion
l_prime	the order \(l'\) of the multipoles expansion
r1	the scale \(r_1\)
r2	the scale \(r_2\)
r1_prime	the scale \(r_1'\)
r2_prime	the scale \(r_2'\)
deltaR	the bin size, if non-positive, no bin average is computed
kk	vector of the wave vector modules
Pk	the pdark matter ower spectrum
rr	vector of scales
Xi	vector containing the two-point correlation function
prec	the integral precision

Returns: the covariance of the multipole expansion of the dark matter three-point correlation function

Definition at line 614 of file 3PCF.cpp.

◆ zeta_precyclic_Slepian() [1/2]

double cbl::cosmology::Cosmology::zeta_precyclic_Slepian	(	const double	r1,
		const double	r2,
		const double	mu,
		const double	b1,
		const double	b2,
		const glob::FuncGrid	interp_xi_matter,
		const glob::FuncGrid	interp_xi_matter_m1,
		const glob::FuncGrid	interp_xi_matter_p1,
		const glob::FuncGrid	interp_xi_matter_2
	)		const

the pre-cyclic three-point correlation function as described in Slepian et al. 2015

this function computes the pre-cyclic three-point correlation function as described in Slepian et al. 2015, as follows:

\[ \zeta_{pc} = \sum_{l=0}^2 \zeta_{pc l}(r_1, r_2) P_l(\hat{r_1}\cdot \hat{r_2})+ \sum_{l=0}^2 \zeta_{pc l}(r_2, r_3) P_l(\hat{r_2}\cdot \hat{r_3})+ \sum_{l=0}^2 \zeta_{pc l}(r_3, r_1) P_l(\hat{r_3}\cdot \hat{r_1}) \]

with

\[r_3 = \sqrt{r_1^2+r_2^2-2 r_1 r_2 \cos(\theta)}\]

and

\[ \zeta_{pc0}(r_i, r_j) = \left[ 2 b_1^2 b_2 + \frac{34}{21} b_1^3 \right] \xi(r_i) \xi(r_j), \]

\[ \zeta_{pc1}(r_i, r_j) = -b_1^3\left[ \xi^{[1-]}(r_i) \xi^{[1+]}(r_j) + \xi^{[1-]}(r_j) \xi^{[1+]}(r_i) \right] , \]

\[ \zeta_{pc2}(r_i, r_j) = \frac{8}{21} b_1^3\xi^{[2]}(r_i)\xi^{[2]}(r_j) . \]

where \( b_1, b_2 \) are the linear and non-linear bias, respectively, and \(\xi_{DM}(r), \xi^{[1\pm]}_{DM}(r), \xi^{[2]}_{DM}(r)\) are the integrals of the dark matter power spectrum computed by cbl::cosmology::Cosmology::integrals_zeta_Slepian

Parameters

r1	the first side
r2	the second side
mu	the cosine of the angle between r1 and r2
b1	the linear bias
b2	the non-linear bias
interp_xi_matter	interpolating function for \(\xi_matter\)
interp_xi_matter_m1	interpolating function for \(\xi^{[1-]}_{DM}(r)\)
interp_xi_matter_p1	interpolating function for \(\xi^{[1+]}_{DM}(r)\)
interp_xi_matter_2	interpolating function for \(\xi^{[2]}_{DM}(r)\)

Returns: the pre-cyclic three-point correlation function

Definition at line 181 of file 3PCF.cpp.

◆ zeta_precyclic_Slepian() [2/2]

double cbl::cosmology::Cosmology::zeta_precyclic_Slepian	(	const double	r1,
		const double	r2,
		const double	r3,
		const double	deltaR,
		const double	b1,
		const double	b2,
		const glob::FuncGrid	interp_xi_matter,
		const glob::FuncGrid	interp_xi_matter_m1,
		const glob::FuncGrid	interp_xi_matter_p1,
		const glob::FuncGrid	interp_xi_matter_2
	)		const

the pre-cyclic three-point correlation function as described in Slepian et al. 2015, for a triangle averaging in the bin

this function computes the pre-cyclic three-point correlation function as described in Slepian et al. 2015, as follows:

\[ \zeta_{pc} = \sum_{l=0}^2 \zeta_{pc l}(r_1, r_2) P_l(\hat{r_1}\cdot \hat{r_2})+ \sum_{l=0}^2 \zeta_{pc l}(r_2, r_3) P_l(\hat{r_2}\cdot \hat{r_3})+ \sum_{l=0}^2 \zeta_{pc l}(r_3, r_1) P_l(\hat{r_3}\cdot \hat{r_1}) \]

with

\[r_3 = \sqrt{r_1^2+r_2^2-2 r_1 r_2 \cos(\theta)}\]

and

\[ \zeta_{pc0}(r_i, r_j) = \left[ 2 b_1^2 b_2 + \frac{34}{21} b_1^3 \right] \xi(r_i) \xi(r_j), \]

\[ \zeta_{pc1}(r_i, r_j) = -b_1^3\left[ \xi^{[1-]}(r_i) \xi^{[1+]}(r_j) + \xi^{[1-]}(r_j) \xi^{[1+]}(r_i) \right] , \]

\[ \zeta_{pc2}(r_i, r_j) = \frac{8}{21} b_1^3\xi^{[2]}(r_i)\xi^{[2]}(r_j) . \]

where \( b_1, b_2 \) are the linear and non-linear bias, respectively, and \(\xi_{DM}(r), \xi^{[1\pm]}_{DM}(r), \xi^{[2]}_{DM}(r)\) are the integrals of the dark matter power spectrum computed by cbl::cosmology::Cosmology::integrals_zeta_Slepian

Parameters

r1	the first side
r2	the second side
r3	the third side
deltaR	the side width
b1	the linear bias
b2	the non-linear bias
interp_xi_matter	interpolating function for \(\xi_matter\)
interp_xi_matter_m1	interpolating function for \(\xi^{[1-]}_{DM}(r)\)
interp_xi_matter_p1	interpolating function for \(\xi^{[1+]}_{DM}(r)\)
interp_xi_matter_2	interpolating function for \(\xi^{[2]}_{DM}(r)\)

Returns: the pre-cyclic three-point correlation function

Definition at line 225 of file 3PCF.cpp.

◆ zeta_RSD() [1/2]

std::vector< double > cbl::cosmology::Cosmology::zeta_RSD	(	const double	r1,
		const double	r2,
		const int	ntheta,
		const double	b1,
		const double	b2,
		const double	bt,
		const double	beta,
		const std::vector< double >	rr,
		const std::vector< double >	kk,
		const std::vector< double >	Pk,
		const bool	include_limits = `false`,
		const int	max_ll = `4`,
		const bool	use_k = `false`
	)

the \( \zeta (r_1, r_2, \theta) \)

This function computes tree-level prediction for three-point correlation function of haloes in redshift space, as derived by Slepian&Eisenstein (2017) in configuration space, based on the work presented by Scoccimarro et al (1999) for the bispectrum.

Parameters

r1	the first triangle side
r2	the second triangle side
ntheta	the number of \(\theta\) bins
b1	the linear bias
b2	the quadratic bias
bt	the tidal bias
beta	the kaiser factor
rr	vector of scales
kk	vector of wavevector modules
Pk	dark matter power spectrum
include_limits	include the \(\theta\) limits
max_ll	maximum order in the model
use_k	if true, use the \(k_l\) part of the model \(O(\beta^2)\)

Returns: the halo redshift space three-point correlation function

Definition at line 1018 of file 3PCF.cpp.

◆ zeta_RSD() [2/2]

std::vector< double > cbl::cosmology::Cosmology::zeta_RSD	(	const double	r1,
		const double	r2,
		const int	ntheta,
		const double	b1,
		const double	b2,
		const double	bt,
		const double	redshift,
		const std::string	method_Pk,
		const int	step_r,
		const int	step_k,
		const bool	store_output = `true`,
		const std::string	output_root = `"test"`,
		const bool	force_RealSpace = `false`,
		const bool	include_limits = `false`,
		const int	max_ll = `4`,
		const bool	use_k = `false`
	)

the \( \zeta (r_1, r_2, \theta) \)

This function computes tree-level prediction for three-point correlation function of haloes in redshift space, as derived by Slepian&Eisenstein (2017) in configuration space, based on the work presented by Scoccimarro et al (1999) for the bispectrum.

Parameters

r1	the first triangle side
r2	the second triangle side
ntheta	the number of \(\theta\) bins
b1	the linear bias
b2	the quadratic bias
bt	the tidal bias
redshift	the redshift
method_Pk	method used to compute the power spectrum (i.e. the Boltzmann solver); valid choices for method_Pk are: CAMB [http://camb.info/], CLASS [http://class-code.net/], MPTbreeze-v1 [http://arxiv.org/abs/1207.1465], EisensteinHu [http://background.uchicago.edu/~whu/transfer/transferpage.html]
step_r	the number of bins for r
step_k	the number of bins for k
store_output	if true the output files created by the Boltzmann solver are stored; if false the output files are removed
output_root	output_root of the parameter file used to compute the power spectrum and σ(mass); it can be any name. If this parameter is different from the default value it will be used also in the output directory name
force_RealSpace	if true, force the computation to be in real space
include_limits	include the \(\theta\) limits
max_ll	maximum order in the model
use_k	if true, use the \(k_l\) part of the model \(O(\beta^2)\)

Returns: the halo redshift space three-point correlation function

Definition at line 1083 of file 3PCF.cpp.

◆ zeta_single_BarrigaGatzanaga()

double cbl::cosmology::Cosmology::zeta_single_BarrigaGatzanaga	(	const double	r1,
		const double	r2,
		const double	theta,
		const std::vector< double >	xi,
		const std::vector< double >	dxi,
		const std::vector< double >	dPhi
	)		const

the single term of the dark matter three-point correlation function model by Barriga & Gatzanaga et al. 2002

this function computes the single term of the dark matter three-point correlation function, following Barriga & Gatzanaga et al. 2002:

\[ f(r_1, r_2) = \frac{10}{7}\xi(r_1) \xi(r_2)+\frac{4}{7} \left\{ -3 \frac{\Phi^\prime(r_1) \Phi^\prime(r_2)}{r_1 r_2} -\frac{\xi(r_1) \Phi^\prime(r_2)}{r_2}-\frac{\xi(r_2) \Phi^\prime(r_1)}{r_1} +\mu^2\left[ \xi(r_1)+3\frac{\Phi^\prime(r_1)}{r1}\right]\left[ \xi(r_2)+3\frac{\Phi^\prime(r_2)}{r_3}\right] \right\} -\mu\left[ \xi^\prime(r_1)\Phi^\prime(r_2) + \xi^\prime(r_2)\Phi^\prime(r_1)\right] \]

where the prime indicates the derivative with respect to \(r\), and \(\xi(r), \Phi(r)\) are the integrals of the power spectrum computed by cbl::cosmology::Cosmology::integrals_zeta_BarrigaGatzanaga

Parameters

r1	the first side of the triangle
r2	the second side of the triangle
theta	the angle betwee r1 and r2
xi	vector containing the value of xi at r1, r2
dxi	vector containing the value of the derivative of xi at r1, r2
dPhi	vector containing the value of the derivative of Phi at r1, r2

Returns: the dark matter reduced three-point correlation function

Definition at line 362 of file 3PCF.cpp.

The documentation for this class was generated from the following files:

Headers/Cosmology.h
Cosmology/Lib/3PCF.cpp
Cosmology/Lib/BAO.cpp
Cosmology/Lib/Bias.cpp
Cosmology/Lib/Bias_vector.cpp
Cosmology/Lib/Cosmology.cpp
Cosmology/Lib/MassFunction.cpp
Cosmology/Lib/MassFunction_vector.cpp
Cosmology/Lib/MassGrowth.cpp
Cosmology/Lib/NG.cpp
Cosmology/Lib/PkXi.cpp
Cosmology/Lib/PkXiNonLinear.cpp
Cosmology/Lib/PkXizSpace.cpp
Cosmology/Lib/RSD.cpp
Cosmology/Lib/Sigma.cpp
Cosmology/Lib/SizeFunction.cpp
Cosmology/Lib/Velocities.cpp

Public Member Functions

Private Member Functions

Private Attributes

Detailed Description

Constructor & Destructor Documentation

◆ Cosmology() [1/2]

◆ Cosmology() [2/2]

Member Function Documentation

◆ Am()

◆ AP_corr()

◆ As()

◆ Az()

◆ beta() [1/3]

◆ beta() [2/3]

◆ beta() [3/3]

◆ bias_correction()

◆ bias_eff() [1/2]

◆ bias_eff() [2/2]

◆ bias_eff_mass() [1/2]

◆ bias_eff_mass() [2/2]

◆ bias_eff_mass_grid()

◆ bias_eff_selection_function() [1/3]

◆ bias_eff_selection_function() [2/3]

◆ bias_eff_selection_function() [3/3]

◆ bias_halo() [1/4]

◆ bias_halo() [2/4]

◆ bias_halo() [3/4]

◆ bias_halo() [4/4]

◆ bispectrum()

◆ C_l_DM()

◆ c_vir()

◆ CMN()

◆ concentration_NFW_Duffy()

◆ converted_mass()

◆ cosmic_time()

◆ create_grid_sigmaM()

◆ cumPw()

◆ D_A() [1/2]

◆ D_A() [2/2]

◆ D_C()

◆ D_C_LCDM()

◆ D_C_table()

◆ D_H()

◆ D_L()

◆ D_M()

◆ D_V()

◆ DD()

◆ Delta_c()

◆ deltac()

◆ deltav_L()

◆ deltav_NL()

◆ denominator_Q()

◆ Distance()

◆ DN()

◆ dnsigma2M()

◆ dnsigma2R()

◆ dskewnessdM()

◆ dV_dZdOmega()

◆ EE()

◆ EE2()

◆ EE_inv()

◆ EE_inv2()

◆ EE_inv3()

◆ eff_l_l1()

◆ error_beta() [1/3]

◆ error_beta() [2/3]

◆ error_beta() [3/3]

◆ error_beta_measured()

◆ F2()

◆ F_AP()

◆ f_DE()

◆ f_k()

◆ f_nu()

◆ fNL()

◆ frk()

◆ fsigma8()

◆ G2()

◆ g_k()

◆ Gamma_3PCF()

◆ generate_bias_eff_grid_one_cosmopar() [1/2]