/* Just like the halo mass function, we'll set this up such that
* you just need to interpolate.
*
* Now this has been changed to calculate the spatial-scale dependence
* of the bias factor. If you don't want the scale dep. b, then just
* input r<0.
*
* If the global flag LINEAR_PSP==0, uses the scale dependence calculated for
* for halo bias relative to the non-linear matter \xi_m(r):
*
* f^2(r) = (1.0+xi*1.17)^1.49/(1.0+xi*0.69)^2.09 --> b(r) = b0*f(r)
*
* For LINEAR_PSP==1, use scale dependence determined for the linear P(k):
*
* f(r) = 1 + exp[-(r/A)^0.7] --> where A is a parameter that we're gonna have to
* determine in more detail, but now A \approx 1
*/
double bias_interp(double m, double r)
{
static int flag=0,prev_cosmo=0, n;
static double *x,*y,*y2, pnorm;
int i;
double dm,max=16.3,min=9,a,b,m1,m2,dm1,xi,power,rm,sig,b1,b2,mass,rvir,a1;
double c1,c2,d1,d2;
if(!flag || RESET_COSMOLOGY!=prev_cosmo)
{
n = 100;
if(!ThisTask && OUTPUT)
fprintf(stdout,"RESET: resetting bias for %f %f\n",OMEGA_M,SIGMA_8);
if(!flag)
{
x=dvector(1,n);
y=dvector(1,n);
y2=dvector(1,n);
}
flag=1;
dm=(double)(max-min)/n;
for(i=1;i<=n;++i)
{
x[i]=pow(10.0,min+i*dm);
y[i]=log(bias(x[i]));
//printf("BIAS %e %e\n",x[i], exp(y[i]));
if(isinf(y[i])){ n = i-1; break; }
if(isnan(y[i])){ n = 1-1; break; }
x[i] = log(x[i]);
continue;
// no longer need to do this part, since we're taking into account
// halo overdensity in the bias formula.
/*
if(DELTA_HALO!=200)
{
x[i]=log(halo_mass_conversion2(x[i],halo_c200(x[i]),200.0,DELTA_HALO));
}
else
{
x[i]=log(x[i]);
}
*/
}
spline(x,y,n,2.0E+30,2.0E+30,y2);
prev_cosmo=RESET_COSMOLOGY;
pnorm=SIGMA_8/sigmac(8.0);
}
m=log(m);
splint(x,y,y2,n,m,&a);
a = exp(a);
// if we're using systematic errors in an MCMC, adjust parameter a1 (amplitude)
if(USE_ERRORS)
a *= M2N.bias_amp;
// if no scale-dependence required, return the large-scale value
if(r<0) return a;
/*
* SCALE DEPENDENT BIAS!!!
*----------------------------------------------------------------------
*/
/* FOR M/N analysis, use the Tinker etal 2005 result:
*/
xi = xi_interp(r);
if(M2N.scalebias_selfcal)
{
b = pow(1.0+xi*M2N.bias_amp1,M2N.bias_pow1)*pow(1.0+xi*0.69,-1.045);
}
else
{
//Attempting to correct scale-dep bias issue
//SCALE-DEP BIAS CORRECTION
rvir = pow(3*exp(m)/(4*PI*200*RHO_CRIT*OMEGA_M),THIRD);
// if(r<2.4*rvir)r=2.4*rvir;
if(r<2.8*rvir)r=2.8*rvir;
//rvir = pow(3*exp(m)/(4*PI*DELTA_HALO*RHO_CRIT*OMEGA_M),THIRD);
//if(r<2*rvir)r=2*rvir;
xi = xi_interp(r);
//parameters for scale-dep bias
//original values
//c1 = 1.17;
//c2 = 0.69;
//d1 = 1.49;
//d2 = -2.09;
c1 = HBIAS_C1;
c2 = HBIAS_C2;
d1 = HBIAS_D1;
d2 = (-1.)*HBIAS_D2;
/**
c1 = 1.52;
c2 = 0.84;
d1 = 1.49;
d2 = -2.09;
**/
b = pow(1.0+xi*c1,d1/2.)*pow(1.0+xi*c2,d2/2.0);
// if we're using systematic errors in an MCMC, adjust parameter a1 (amplitude)
if(USE_ERRORS) {
b = (b-1)*M2N.scalebias_amp + 1;
if(b<0)b=0;
}
}
return b*a;
/* first, calculate the standard Zheng-like, mass-independent scale bias
* based on the non-linear correlation function
* (re-calibrated using the SO catalogs)
*/
xi = xi_interp(r);
b = pow(1.0+xi*0.92,2.08)*pow(1.0+xi*0.74,-2.37);
if(b<0.6)b=0.6;
/* Now the mass-dependent term.
* Where the mass-dependence comes in the form of the large-scale bias itself
*/
sig = sigmac_radius_interp(r);
//if(a<0)
//b *= pow(1 + 0.028*pow(a,1.53)*pow(sig,1.57),2.59)/
//pow(1 + 0.253*pow(a,1.24)*pow(sig,1.71),0.397);
// if we're using systematic errors in an MCMC, adjust parameter a1 (amplitude)
if(USE_ERRORS) {
b = (b-1)*M2N.scalebias_amp + 1;
if(b<0)b=0;
}
return b*a;
}
int main(int argc, char **argv)
{
double s1, delta_vir, omega_m, x;
int i, j;
FILE *fp;
#ifdef PARALLEL
printf("STARTING>>>\n");
fflush(stdout);
MPI_Init(&argc, &argv);
MPI_Comm_rank(MPI_COMM_WORLD, &ThisTask);
MPI_Comm_size(MPI_COMM_WORLD, &NTask);
printf("TASK %d reporting for duty.\n",ThisTask);
fflush(stdout);
#endif
ARGC = argc;
ARGV = argv;
OUTPUT=0;
HOD.fredc = HOD.freds = 1.0;
for(i=1; i<=99; ++i)
HOD.free[i]=0;
wp.esys=0;
Work.chi2=0;
Work.imodel=1;
USE_ERRORS = 0;
ITRANS=4;
HUBBLE=0.7;
BEST_FIT = 0;
HOD.M_sat_break = 1.0e14;
HOD.alpha1 = 1.0;
if(argc==1)
endrun("./HOD.x hod.bat_file > output");
read_parameter_file(argv[1]);
if(REDSHIFT>0)
{
SIGMA_8 = SIGMA_8*growthfactor(REDSHIFT);
HUBBLEZ = sqrt(OMEGA_M*pow(1+REDSHIFT,3.0)+1-OMEGA_M);
OMEGA_Z = OMEGA_M*pow(1+REDSHIFT,3.0)/(OMEGA_M*pow(1+REDSHIFT,3.0)+(1-OMEGA_M));
fprintf(stdout,"SIGMA_8(Z=%.3f)= %.4f\n",REDSHIFT,SIGMA_8);
fprintf(stdout,"H(Z=%.3f)/H0= %.4f\n",REDSHIFT,HUBBLEZ);
HOD.M_min = 0;
RESET_COSMOLOGY++;
set_HOD_params();
}
/* Output the virial overdensity for reference.
*/
if(OUTPUT)
{
omega_m=OMEGA_M*pow(1+REDSHIFT,3.0)/(OMEGA_M*pow(1+REDSHIFT,3.0)+(1-OMEGA_M));
x=omega_m-1;
delta_vir=(18*PI*PI+82*x-39*x*x)/(1+x);
printf("DELTA_VIR(Omega_m,z) = %f\n",delta_vir);
}
/* Do some initialization if we're doing SHMR
*/
if(SHMR_FLAG)
{
if(SATELLITE_PARAMETERIZATION)SHMR_PARAMS = 14;
if(VARIABLE_ALPHA)SHMR_PARAMS += 2;
if(VARIABLE_EXCLUSION)wpl.a[SHMR_PARAMS+1] = EXCLUSION_RADIUS;
wpl.ncf = SHMR_PARAMS + VARIABLE_EXCLUSION;
HOD.pdfs = 100;
HOD.pdfc = 101;
wpx.calculate_two_halo = 1;
input_stellar_mass_bins();
// if we have input from the prompt, take that
if(argc>2 && atoi(argv[2])!=999)
{
fp = openfile(argv[2]);
fscanf(fp,"%d %d",&i,&j);
for(i=1; i<=wpl.ncf; ++i)
fscanf(fp,"%lf",&wpl.a[i]);
fclose(fp);
}
}
for(i=1; i<=wpl.ncf; ++i)
printf("wpl.a[%d]= %e\n",i,wpl.a[i]);
/* LENSING TESTING FOR ALEXIE
*/
if(argc>2)
IDUM_MCMC=atoi(argv[2]);
SIGMA_8Z0 = 0.8;
if(argc>2)
if(atoi(argv[2])==999)
test(argc,argv);
/* If there's no cross-correlation function,
* set the second number density equal to the first
*/
if(!XCORR)
GALAXY_DENSITY2 = GALAXY_DENSITY;
/* Initialize the non-linear power spectrum.
*/
nonlinear_sigmac(8.0);
sigmac_interp(1.0E13);
sigmac_radius_interp(1.0);
/* Skip the HOD stuff if we're SHMR-ing it:
*/
if(SHMR_FLAG)
{
if(argc>2 && atoi(argv[2])==999)test(argc, argv);
if(argc>3 && atoi(argv[3])==999)test(argc, argv);
goto TASKS;
}
/* Get the galaxy bias factor
*/
s1=qromo(func_galaxy_bias,log(HOD.M_low),log(HOD.M_max),midpnt);
GALAXY_BIAS=s1/GALAXY_DENSITY;
if(OUTPUT)
fprintf(stdout,"Galaxy Bias bg= %f\n",GALAXY_BIAS);
fflush(stdout);
/* Get the galaxy satellite fraction
*/
s1=qromo(func_satellite_density,log(HOD.M_low),log(HOD.M_max),midpnt)/
GALAXY_DENSITY;
if(OUTPUT)
fprintf(stdout,"fsat %e\n",s1);
fflush(stdout);
/* Mean halo mass.
*/
if(OUTPUT)
fprintf(stdout,"M_eff %e\n",number_weighted_halo_mass());
fflush(stdout);
/* Set up BETA for wp integration.
*/
BETA = pow(OMEGA_M,0.6)/GALAXY_BIAS;
if(OUTPUT)
printf("BETA = %f\n",BETA);
TASKS:
tasks(argc,argv);
}
