ModelFunction_NumberCounts2D_RedshiftMass.cpp

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/********************************************************************
 *  Copyright (C) 2016 by Federico Marulli and Alfonso Veropalumbo  *
 *  federico.marulli3@unibo.it                                      *
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#include "ModelFunction_NumberCounts2D_RedshiftMass.h"
 
using namespace std;
 
using namespace cbl;
 
 
// ===========================================================================================
 
 
std::vector<std::vector<double>> cbl::modelling::numbercounts::mass_function_redshift_mass (const std::vector<double> redshift, const std::vector<double> mass, const std::shared_ptr<void> inputs, std::vector<double> &parameter)
{
  // structure contaning the required input data
  shared_ptr<STR_NC_data_model> pp = static_pointer_cast<STR_NC_data_model>(inputs);
 
  // redefine the cosmology
  cbl::cosmology::Cosmology cosmo = *pp->cosmology;
 
  // input likelihood parameters
 
  // set the cosmological parameters used to compute the dark matter
  // two-point correlation function in real space
  for (size_t i=0; i<pp->Cpar.size(); ++i)
    cosmo.set_parameter(pp->Cpar[i], parameter[i]);
 
  // compute the power spectrum
  std::vector<double> Pk = cosmo.Pk_matter(pp->kk, pp->method_Pk, false, 0., pp->store_output, pp->output_root, pp->norm, pp->k_min, pp->k_max, pp->prec, pp->file_par);
 
  return cbl::modelling::numbercounts::mass_function(redshift, mass, cosmo, pp->model_MF, pp->store_output, pp->Delta, pp->isDelta_critical, pp->kk, Pk, "Spline", pp->k_max);
}
 
 
// ===========================================================================================
 
 
std::vector<std::vector<double>> cbl::modelling::numbercounts::number_density_redshift_mass (const std::vector<double> redshift, const std::vector<double> mass, const std::shared_ptr<void> inputs, std::vector<double> &parameter)
{
  (void)redshift; (void)mass;
  
  // structure contaning the required input data
  shared_ptr<STR_NC_data_model> pp = static_pointer_cast<STR_NC_data_model>(inputs);
 
  // redefine the cosmology
  cbl::cosmology::Cosmology cosmo = *pp->cosmology;
 
  // input likelihood parameters
 
  // set the cosmological parameters used to compute the dark matter
  // two-point correlation function in real space
  for (size_t i=0; i<pp->Cpar.size(); ++i)
    cosmo.set_parameter(pp->Cpar[i], parameter[i]);
 
  // compute the power spectrum
  std::vector<double> Pk = cosmo.Pk_matter(pp->kk, pp->method_Pk, false, 0., pp->store_output, pp->output_root, pp->norm, pp->k_min, pp->k_max, pp->prec, pp->file_par);
 
  std::vector<std::vector<double>> mass_function = cbl::modelling::numbercounts::mass_function (pp->z_vector, pp->Mass_vector, cosmo, pp->model_MF, pp->store_output, pp->Delta, pp->isDelta_critical, pp->kk, Pk, "Spline", pp->k_max);
 
  glob::FuncGrid2D interp_MF (pp->z_vector, pp->Mass_vector, mass_function, "Linear");
 
  std::vector<std::vector<double>> number_density(pp->edges_x.size()-1, std::vector<double>(pp->edges_y.size()-1));
  for (size_t i=0; i<pp->edges_x.size()-1; i++) {
    for (size_t j=0; j<pp->edges_y.size()-1; j++) {
      number_density[i][j] = interp_MF.IntegrateVegas(pp->edges_x[i], pp->edges_x[i+1], pp->edges_y[j], pp->edges_y[j+1]);
    }
  }
 
  return number_density;
}
 
 
// ===========================================================================================
 
 
std::vector<std::vector<double>> cbl::modelling::numbercounts::number_counts_redshift_mass (const std::vector<double> redshift, const std::vector<double> mass, const std::shared_ptr<void> inputs, std::vector<double> &parameter)
{
  (void)redshift; (void)mass;
  
  // structure contaning the required input data
  shared_ptr<STR_NC_data_model> pp = static_pointer_cast<STR_NC_data_model>(inputs);
 
  // redefine the cosmology
  cbl::cosmology::Cosmology cosmo = *pp->cosmology;
 
  // input likelihood parameters
 
  // set the cosmological parameters used to compute the dark matter
  // two-point correlation function in real space
  const size_t npar = (pp->is_sigma8_free) ? pp->Cpar.size() : pp->Cpar.size()-1;
  for (size_t i=0; i<npar; ++i)
    cosmo.set_parameter(pp->Cpar[i], parameter[i]);
  
  // Moved below for convenience...
  //if (!pp->is_sigma8_free) parameter[pp->Cpar.size()-1] = cosmo.sigma8();
 
  // compute the power spectrum
  const std::vector<double> Pk = cosmo.Pk_matter(pp->kk, pp->method_Pk, false, 0., pp->store_output, pp->output_root, pp->norm, pp->k_min, pp->k_max, pp->prec, pp->file_par, true);
  
  const std::vector<cbl::glob::FuncGrid> interp = cbl::modelling::numbercounts::sigmaM_dlnsigmaM(pp->Mass_vector, cosmo, pp->kk, Pk, "Spline", pp->k_max);
 
  // SigmaM has been computed in the previous line, just take sigma8 from it -> M8 = Mass(8., cosmo.rho_m()), probably...
  if (!pp->is_sigma8_free) parameter[pp->Cpar.size()-1] = interp[0](Mass(8., cosmo.rho_m())); 
 
  std::vector<std::vector<double>> number_counts(pp->edges_x.size()-1, std::vector<double>(pp->edges_y.size()-1));
  for (size_t i=0; i<pp->edges_x.size()-1; i++) {
    for (size_t j=0; j<pp->edges_y.size()-1; j++) {
      number_counts[i][j] = cbl::modelling::numbercounts::number_counts(pp->edges_x[i], pp->edges_x[i+1], pp->edges_y[j], pp->edges_y[j+1], cosmo, pp->area_rad, pp->model_MF, pp->store_output, pp->Delta, pp->isDelta_critical, interp[0], interp[1]);
    }
  }
    
  return number_counts;
}