ccl_test_emu_nu.c File Reference

#include "ccl.h"
#include "ccl_neutrinos.h"
#include "ctest.h"
#include <stdio.h>
#include <math.h>

Include dependency graph for ccl_test_emu_nu.c:

Go to the source code of this file.

Classes
struct	emu_nu_data

Macros
#define	EMU_TOLERANCE   3.0E-2

Functions
void	__attribute__ ((weak))
static int	linecount (FILE *f)
static void	compare_emu_nu (int i_model, struct emu_nu_data *data)
void	__ctest_emu_nu_model_1_run (struct emu_nu_data *data)
void	__ctest_emu_nu_model_2_run (struct emu_nu_data *data)
void	__ctest_emu_nu_model_3_run (struct emu_nu_data *data)
void	__ctest_emu_nu_model_4_run (struct emu_nu_data *data)

Variables
static struct emu_nu_data	__ctest_emu_nu_data

Macro Definition Documentation

#define EMU_TOLERANCE   3.0E-2

Definition at line 19 of file ccl_test_emu_nu.c.

Referenced by compare_emu_nu().

Function Documentation

void __attribute__

(

(weak)

)

Definition at line 36 of file ccl_test_emu_nu.c.

References ccl_mnu_list, ccl_nu_equal, ccl_nu_masses(), ccl_test_distances::h, ccl_test_distances::n_s, ccl_test_distances::Omega_b, ccl_test_distances::Omega_c, halomod_bm::params, and ccl_test_power::sigma8.

                    {
  
  data->Neff = 3.04;
  data->mnu_type = ccl_mnu_list;

  double *sigma8;
  double *Omega_c;
  double *Omega_b;
  double *Omega_nu;
  double *n_s;
  double *h;
  double *w_0;
  double *w_a;
  double *Mnu_out;
  int status=0;
  char fname[256],str[1024];
  char* rtn;
  FILE *f;
  int i;
  ccl_parameters * params;

  sigma8=malloc(4*sizeof(double));
  Omega_c=malloc(4*sizeof(double));
  Omega_b=malloc(4*sizeof(double));
  n_s=malloc(4*sizeof(double));
  h=malloc(4*sizeof(double));
  w_0=malloc(4*sizeof(double));
  w_a=malloc(4*sizeof(double));
  Omega_nu=malloc(4*sizeof(double));
  
  // Omeganuh2_to_mnu will output a pointer to an array of 3 neutrino masses.
  Mnu_out=malloc(3*sizeof(double));

  //Each line of this file corresponds to the cosmological parameters for
  //cosmologies {38,39,40,42} of the emulator set. Notice that Omega_i
  //are big Omegas and not little omegas (Omega_i*h**2=omega_i)
  sprintf(fname,"./tests/benchmark/emu_nu_cosmologies.txt");
  f=fopen(fname,"r");
  if(f==NULL) {
    fprintf(stderr,"Error opening file %s\n",fname);
    exit(1);
  }
  
  double tmp;
  int omnustatus=0;
  for(int i=0;i<4;i++) {
    
    status=fscanf(f,"%le %le %le %le %le %le %le %le\n",&Omega_c[i],&Omega_b[i],&h[i],&sigma8[i],&n_s[i],&w_0[i],&w_a[i],&Omega_nu[i]);
    if(status!=8) {
      fprintf(stderr,"Error reading file %s, line %d\n",fname,i);
      exit(1);
    }
    data->w_0[i] = w_0[i];
    data->w_a[i] = w_a[i];
    data->h[i] = h[i];
    data->sigma8[i] = sigma8[i];
    data->Omega_c[i] = Omega_c[i];
    data->Omega_b[i] = Omega_b[i];
    data->n_s[i] = n_s[i];
    // Number of neutrino species is fixed to 3
    Mnu_out = ccl_nu_masses(Omega_nu[i]*h[i]*h[i], ccl_nu_equal, 2.725, &omnustatus);
    /*if (omnustatus){
      printf("%s\n",cosmo->status_message);
      exit(1);
      }*/
    data->mnu[i]=Mnu_out;
  }
  fclose(f);
}

void __ctest_emu_nu_model_1_run

(

struct emu_nu_data *

data

)

Definition at line 177 of file ccl_test_emu_nu.c.

References compare_emu_nu().

                       {
  int model=1;
  compare_emu_nu(model,data);
}

void __ctest_emu_nu_model_2_run

(

struct emu_nu_data *

data

)

Definition at line 183 of file ccl_test_emu_nu.c.

References compare_emu_nu().

                       {
  int model=2;
  compare_emu_nu(model,data);
  }

void __ctest_emu_nu_model_3_run

(

struct emu_nu_data *

data

)

Definition at line 188 of file ccl_test_emu_nu.c.

References compare_emu_nu().

                       {
  int model=3;
  compare_emu_nu(model,data);
}

void __ctest_emu_nu_model_4_run

(

struct emu_nu_data *

data

)

Definition at line 193 of file ccl_test_emu_nu.c.

References compare_emu_nu().

                       {
  int model=4;
  compare_emu_nu(model,data);
  }

static void compare_emu_nu ( int  i_model, struct emu_nu_data *  data  )

static

Definition at line 118 of file ccl_test_emu_nu.c.

References ASSERT_DBL_NEAR_TOL, ASSERT_NOT_NULL, ccl_cosmology_create(), ccl_cosmology_free(), ccl_emu, ccl_emulator, ccl_nonlin_matter_power(), ccl_parameters_create(), cl_cmbl_bm::cosmo, default_config, EMU_TOLERANCE, emu_nu_data::h, linecount(), ccl_configuration::matter_power_spectrum_method, emu_nu_data::mnu, emu_nu_data::mnu_type, emu_nu_data::n_s, emu_nu_data::Neff, emu_nu_data::Omega_b, emu_nu_data::Omega_c, ccl_parameters::Omega_g, ccl_parameters::Omega_l, halomod_bm::params, emu_nu_data::sigma8, ccl_cosmology::status_message, ccl_configuration::transfer_function_method, emu_nu_data::w_0, emu_nu_data::w_a, and z.

Referenced by __ctest_emu_nu_model_1_run(), __ctest_emu_nu_model_2_run(), __ctest_emu_nu_model_3_run(), and __ctest_emu_nu_model_4_run().

{
  int nk,i,j;
  int status=0;
  char fname[256],str[1024];
  char* rtn;
  FILE *f;
  int i_model_vec[4]={38,39,40,42}; //The emulator cosmologies we can compare to 
  
  ccl_configuration config = default_config;
  config.transfer_function_method = ccl_emulator;
  config.matter_power_spectrum_method = ccl_emu;
 
  //None of the current cosmologies being checked include neutrinos
  ccl_parameters params = ccl_parameters_create(data->Omega_c[i_model-1],data->Omega_b[i_model-1],0.0,data->Neff, data->mnu[i_model-1], data->mnu_type, data->w_0[i_model-1],data->w_a[i_model-1],data->h[i_model-1],data->sigma8[i_model-1],data->n_s[i_model-1],-1,-1,-1,-1,NULL,NULL, &status);
  params.Omega_l=params.Omega_l+params.Omega_g;
  params.Omega_g=0;
  ccl_cosmology * cosmo = ccl_cosmology_create(params, config);
  ASSERT_NOT_NULL(cosmo);

  //These files contain the smoothed power spectra with neutrinos
  //These are obtained as follows:
  // (1) Find the z=0 P(k) corresponding to M038. This would be column 304 of the 
  //     'yalt...' file (with column numbering starting in 1).
  // (2) This column has log10(Delta_cb^2/k^1.5), so convert accordingly to Delta_cb^2.
  // (3) Take the power spectrum in the file ‘pk_lin...' for M038 (second column for P(k) in Mpc^3)
  //     and convert to Delta_nu^2 by multiplying by k^3/(2pi^2).
  // (4) Add to obtain Delta_tot=(sqrt(Delta_nu)+sqrt(Delta_cb))^2.
  // (5) Convert back to P(k)
  sprintf(fname,"./tests/benchmark/emu_nu_smooth_pk_M%d.txt",i_model_vec[i_model-1]);
  f=fopen(fname,"r");
  if(f==NULL) {
    fprintf(stderr,"Error opening file %s\n",fname);
    exit(1);
  }
  nk=linecount(f)-1; rewind(f);
  
  double k=0.,pk_bench=0.,pk_ccl,err;
  double z=0.; //Other redshift checks are possible but not currently implemented
  int stat=0;
  
  for(i=0;i<nk;i++) {      
    stat=fscanf(f,"%le %le\n",&k, &pk_bench);
    if(stat!=2) {
      fprintf(stderr,"Error reading file %s, line %d\n",fname,i);
      exit(1);
    }
    pk_ccl=ccl_nonlin_matter_power(cosmo,k,1./(1+z),&status);
    if (status) printf("%s\n",cosmo->status_message);
    err=fabs(pk_ccl/pk_bench-1);
    //printf("%le %le %le %le\n",k,pk_ccl,pk_bench,err);
    ASSERT_DBL_NEAR_TOL(err,0.,EMU_TOLERANCE);
  }

  fclose(f);

  ccl_cosmology_free(cosmo);
}

static int linecount ( FILE *  f )

static

Definition at line 106 of file ccl_test_emu_nu.c.

Referenced by compare_emu_nu().

{
  // Counts #lines from file
  int i0=0;
  char ch[1000];
  while((fgets(ch,sizeof(ch),f))!=NULL) {
    i0++;
  }
  return i0;
}

Variable Documentation

static struct emu_nu_data __ctest_emu_nu_data

static

Definition at line 177 of file ccl_test_emu_nu.c.