ccl_massfunc.h File Reference

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Functions
CCL_BEGIN_DECLS void	ccl_cosmology_compute_sigma (ccl_cosmology *cosmo, int *status)
double	ccl_massfunc (ccl_cosmology *cosmo, double smooth_mass, double a, double odelta, int *status)
double	ccl_halo_bias (ccl_cosmology *cosmo, double smooth_mass, double a, double odelta, int *status)
double	ccl_massfunc_m2r (ccl_cosmology *cosmo, double smooth_mass, int *status)
double	ccl_sigmaM (ccl_cosmology *cosmo, double smooth_mass, double a, int *status)
double	dc_NakamuraSuto (ccl_cosmology *cosmo, double a, int *status)
double	Dv_BryanNorman (ccl_cosmology *cosmo, double a, int *status)
double	r_delta (ccl_cosmology *cosmo, double halomass, double a, double odelta, int *status)

Function Documentation

CCL_BEGIN_DECLS void ccl_cosmology_compute_sigma	(	ccl_cosmology *	cosmo,
		int *	status
	)

Definition at line 431 of file ccl_massfunc.c.

References ccl_data::accelerator_m, ccl_cosmology_set_status_message(), CCL_ERROR_LINSPACE, CCL_ERROR_SPLINE, ccl_linear_spacing(), ccl_massfunc_m2r(), ccl_raise_gsl_warning(), ccl_sigmaR(), ccl_splines, ccl_cosmology::computed_sigma, ccl_cosmology::data, ccl_data::dlnsigma_dlogm, ccl_spline_params::LOGM_SPLINE_DELTA, ccl_spline_params::LOGM_SPLINE_MAX, ccl_spline_params::LOGM_SPLINE_MIN, ccl_spline_params::LOGM_SPLINE_NM, ccl_data::logsigma, m, M_SPLINE_TYPE, and pow().

Referenced by ccl_dlninvsig_dlogm(), ccl_halo_bias(), and ccl_sigmaM().

{
  if(cosmo->computed_sigma)
    return;

  // create linearly-spaced values of the mass.
  int nm=ccl_splines->LOGM_SPLINE_NM;
  double * m = ccl_linear_spacing(ccl_splines->LOGM_SPLINE_MIN, ccl_splines->LOGM_SPLINE_MAX, nm);

  // create space for y, to be filled with sigma and dlnsigma_dlogm
  double * y = malloc(sizeof(double)*nm);
  double smooth_radius;
  double na, nb;

  // start up of GSL pointers
  int gslstatus = 0;
  gsl_spline *logsigma;
  gsl_spline *dlnsigma_dlogm;

  if (m==NULL ||
      (fabs(m[0]-ccl_splines->LOGM_SPLINE_MIN)>1e-5) ||
      (fabs(m[nm-1]-ccl_splines->LOGM_SPLINE_MAX)>1e-5) ||
      (m[nm-1]>10E17)
      ) {
    *status = CCL_ERROR_LINSPACE;
    ccl_cosmology_set_status_message(cosmo,"ccl_cosmology_compute_sigmas(): Error creating linear spacing in m\n");
  }

  // fill in sigma, if no errors have been triggered at this time.
  if (*status == 0) {
    for (int i=0; i<nm; i++) {
      smooth_radius = ccl_massfunc_m2r(cosmo, pow(10,m[i]), status);
      y[i] = log10(ccl_sigmaR(cosmo, smooth_radius, 1., status));
    }
    logsigma = gsl_spline_alloc(M_SPLINE_TYPE, nm);
    *status = gsl_spline_init(logsigma, m, y, nm);
  }

  if (*status !=0 ) {
    *status = CCL_ERROR_SPLINE ;
    ccl_cosmology_set_status_message(cosmo, "ccl_massfunc.c: ccl_cosmology_compute_sigma(): Error creating sigma(M) spline\n");
  }

  // again, making splines assuming nothing bad has happened to this point

  if (*status == 0 ) {
    for (int i=0; i<nm; i++) {
      if(i==0) {
        gslstatus |= gsl_spline_eval_e(logsigma, m[i], NULL,&na);
        gslstatus |= gsl_spline_eval_e(logsigma, m[i]+ccl_splines->LOGM_SPLINE_DELTA/2., NULL,&nb);
        y[i] = (na-nb)*log(10.);
        y[i] = 2.*y[i] / ccl_splines->LOGM_SPLINE_DELTA;
      }
      else if (i==nm-1) {
        gslstatus |= gsl_spline_eval_e(logsigma, m[i]-ccl_splines->LOGM_SPLINE_DELTA/2., NULL,&na);
        gslstatus |= gsl_spline_eval_e(logsigma, m[i], NULL,&nb);
        y[i] = (na-nb)*log(10.);
        y[i] = 2.*y[i] / ccl_splines->LOGM_SPLINE_DELTA;
      }
      else {
        gslstatus |= gsl_spline_eval_e(logsigma, m[i]-ccl_splines->LOGM_SPLINE_DELTA/2., NULL,&na);
        gslstatus |= gsl_spline_eval_e(logsigma, m[i]+ccl_splines->LOGM_SPLINE_DELTA/2., NULL,&nb);
        y[i] = (na-nb)*log(10.);
        y[i] = y[i] / ccl_splines->LOGM_SPLINE_DELTA;
      }
    }
  }

  if(gslstatus != GSL_SUCCESS) {
    ccl_raise_gsl_warning(gslstatus, "ccl_massfunc.c: ccl_cosmology_compute_sigma():");
    *status |= gslstatus;
    *status = CCL_ERROR_SPLINE ;
    ccl_cosmology_set_status_message(cosmo, "ccl_massfunc.c: ccl_cosmology_compute_sigma(): Error evaluating grid points for dlnsigma/dlogM spline\n");
  }

  if(*status==0) {
    dlnsigma_dlogm = gsl_spline_alloc(M_SPLINE_TYPE, nm);
    *status = gsl_spline_init(dlnsigma_dlogm, m, y, nm);
    if(cosmo->data.accelerator_m==NULL)
      cosmo->data.accelerator_m=gsl_interp_accel_alloc();
  }

  if(*status!=0) {
    *status = CCL_ERROR_SPLINE ;
    ccl_cosmology_set_status_message(cosmo, "ccl_massfunc.c: ccl_cosmology_compute_sigma(): Error creating dlnsigma/dlogM spline\n");
  }
  

  cosmo->data.logsigma = logsigma;
  cosmo->data.dlnsigma_dlogm = dlnsigma_dlogm;
  cosmo->computed_sigma = true;

  free(m);
  free(y);
  if(*status != 0) {
    gsl_spline_free(logsigma);
    gsl_spline_free(dlnsigma_dlogm);
  }
  return;
}

double ccl_halo_bias	(	ccl_cosmology *	cosmo,
		double	smooth_mass,
		double	a,
		double	odelta,
		int *	status
	)

Definition at line 582 of file ccl_massfunc.c.

References ccl_check_status(), ccl_cosmology_compute_sigma(), ccl_cosmology_set_status_message(), CCL_ERROR_NOT_IMPLEMENTED, ccl_halo_b1(), ccl_cosmology::computed_sigma, ccl_parameters::N_nu_mass, and ccl_cosmology::params.

Referenced by main(), and two_halo_integrand().

{
  if (cosmo->params.N_nu_mass>0){
      *status = CCL_ERROR_NOT_IMPLEMENTED;
      ccl_cosmology_set_status_message(cosmo, "ccl_background.c: ccl_cosmology_compute_growth(): Support for the halo bias in cosmologies with massive neutrinos is not yet implemented.\n");
      return NAN;
  }


  if (!cosmo->computed_sigma) {
    ccl_cosmology_compute_sigma(cosmo, status);
    ccl_check_status(cosmo, status);
  }

  double f;
  f = ccl_halo_b1(cosmo,halomass,a,odelta, status);
  ccl_check_status(cosmo, status);
  return f;
}

double ccl_massfunc	(	ccl_cosmology *	cosmo,
		double	smooth_mass,
		double	a,
		double	odelta,
		int *	status
	)

Definition at line 562 of file ccl_massfunc.c.

References ccl_cosmology_set_status_message(), ccl_dlninvsig_dlogm(), CCL_ERROR_NOT_IMPLEMENTED, ccl_parameters::h, massfunc_f(), ccl_parameters::N_nu_mass, ccl_parameters::Omega_m, ccl_cosmology::params, and RHO_CRITICAL.

Referenced by compare_massfunc(), main(), one_halo_integrand(), and two_halo_integrand().

{
  if (cosmo->params.N_nu_mass>0){
      *status = CCL_ERROR_NOT_IMPLEMENTED;
      ccl_cosmology_set_status_message(cosmo, "ccl_background.c: ccl_cosmology_compute_growth(): Support for the halo mass function in cosmologies with massive neutrinos is not yet implemented.\n");
      return NAN;
  }

  double f, rho_m;

  rho_m = RHO_CRITICAL*cosmo->params.Omega_m*cosmo->params.h*cosmo->params.h;
  f=massfunc_f(cosmo,halomass,a,odelta,status);

  return f*rho_m*ccl_dlninvsig_dlogm(cosmo,halomass,status)/halomass;
}

double ccl_massfunc_m2r	(	ccl_cosmology *	cosmo,
		double	smooth_mass,
		int *	status
	)

Definition at line 606 of file ccl_massfunc.c.

References ccl_rho_x(), ccl_species_m_label, M_PI, and pow().

Referenced by ccl_cosmology_compute_sigma().

{
  double rho_m, smooth_radius;

  // Comoving matter density
  //rho_m = RHO_CRITICAL*cosmo->params.Omega_m*cosmo->params.h*cosmo->params.h;
  rho_m = ccl_rho_x(cosmo, 1., ccl_species_m_label, 1, status);

  smooth_radius = pow((3.0*halomass) / (4*M_PI*rho_m), (1.0/3.0));

  return smooth_radius;
}

double ccl_sigmaM	(	ccl_cosmology *	cosmo,
		double	smooth_mass,
		double	a,
		int *	status
	)

Definition at line 624 of file ccl_massfunc.c.

References ccl_data::accelerator_m, ccl_check_status(), ccl_cosmology_compute_sigma(), ccl_cosmology_set_status_message(), CCL_ERROR_NOT_IMPLEMENTED, ccl_growth_factor(), ccl_raise_gsl_warning(), ccl_cosmology::computed_sigma, ccl_cosmology::data, ccl_data::logsigma, ccl_parameters::N_nu_mass, ccl_cosmology::params, and pow().

Referenced by ccl_halo_b1(), ccl_halo_concentration(), compare_massfunc(), compare_sigmam(), and massfunc_f().

{
  if (cosmo->params.N_nu_mass>0){
      *status = CCL_ERROR_NOT_IMPLEMENTED;
      ccl_cosmology_set_status_message(cosmo, "ccl_background.c: ccl_cosmology_compute_growth(): Support for the sigma(M) function in cosmologies with massive neutrinos is not yet implemented.\n");
      return NAN;
  }

  double sigmaM;
  // Check if sigma has already been calculated
  if (!cosmo->computed_sigma) {
    ccl_cosmology_compute_sigma(cosmo, status);
    ccl_check_status(cosmo, status);
  }

  double lgsigmaM;

  int gslstatus = gsl_spline_eval_e(cosmo->data.logsigma, 
                                    log10(halomass), 
                                    cosmo->data.accelerator_m,&lgsigmaM);

  if(gslstatus != GSL_SUCCESS) {
    ccl_raise_gsl_warning(gslstatus, "ccl_massfunc.c: ccl_sigmaM():");
    *status |= gslstatus;
  }

  // Interpolate to get sigma
  sigmaM = pow(10,lgsigmaM)*ccl_growth_factor(cosmo, a, status);
  ccl_check_status(cosmo, status);
  return sigmaM;
}

double dc_NakamuraSuto	(	ccl_cosmology *	cosmo,
		double	a,
		int *	status
	)

Definition at line 21 of file ccl_massfunc.c.

References ccl_omega_x(), ccl_species_m_label, M_PI, and pow().

Referenced by ccl_halo_b1(), and massfunc_f().

                                                                   {

  double Om_mz = ccl_omega_x(cosmo, a, ccl_species_m_label, status);
  double dc0 = (3./20.)*pow(12.*M_PI,2./3.);
  double dc = dc0*(1.+0.012299*log10(Om_mz));

  return dc;

}

double Dv_BryanNorman	(	ccl_cosmology *	cosmo,
		double	a,
		int *	status
	)

Definition at line 37 of file ccl_massfunc.c.

References ccl_omega_x(), ccl_species_m_label, M_PI, pow(), and x.

Referenced by ccl_halo_b1(), ccl_halo_concentration(), ccl_twohalo_matter_power(), massfunc_f(), one_halo_integrand(), and two_halo_integrand().

                                                                  {

  double Om_mz = ccl_omega_x(cosmo, a, ccl_species_m_label, status);
  double x = Om_mz-1.;
  double Dv0 = 18.*pow(M_PI,2);
  double Dv = (Dv0+82.*x-39.*pow(x,2))/Om_mz;

  return Dv;

}

double r_delta	(	ccl_cosmology *	cosmo,
		double	halomass,
		double	a,
		double	odelta,
		int *	status
	)

Definition at line 52 of file ccl_massfunc.c.

References ccl_rho_x(), M_PI, and pow().

Referenced by window_function().

                                                                                           {

  double rho_matter = ccl_rho_x(cosmo, 1., 1, 1, status);

  return pow(halomass*3.0/(4.0*M_PI*rho_matter*odelta),1.0/3.0);

}