double halo_mass_function(double mass)
{
double sig,logm,a,slo,shi,rm,rlo,rhi,mlo,mhi,dsdM,n,nuprime,nufnu,p,A, fac;
static int flag=0,SO180=0,SO324=0,WARREN=0,ST=0,JENKINS=0;
static double pnorm, prev_delta, prev_cosmo;
double btemp = -1;
static double
a1 = 0.325277,
a2 = 0.492785,
a3 = 0.310289,
a4 = 1.317104,
a5 = 2.425681;
/* Jenkins et al. SO 180 best-fit
*/
if(SO180)
{
JENKINS_A = 0.301;
JENKINS_B = 0.64;
JENKINS_C = 3.82;
}
if(SO324)
{
JENKINS_A = 0.316;
JENKINS_B = 0.67;
JENKINS_C = 3.82;
}
if(JENKINS) //their .2 fof function
{
JENKINS_A = 0.315;
JENKINS_B = 0.61;
JENKINS_C = 3.8;
}
/* First normalize the power spectrum
*/
pnorm=SIGMA_8/sigmac(8.0);
rm=pow(3.0*mass/(4.0*PI*OMEGA_M*RHO_CRIT),1.0/3.0);
sig=pnorm*sigmac(rm);
logm=log10(mass);
mlo=0.99*mass;
mhi=1.01*mass;
rlo=pow(3.0*mlo/(4.0*PI*OMEGA_M*RHO_CRIT),1.0/3.0);
rhi=pow(3.0*mhi/(4.0*PI*OMEGA_M*RHO_CRIT),1.0/3.0);
slo=pnorm*sigmac(rlo);
shi=pnorm*sigmac(rhi);
dsdM=(shi-slo)/(mhi-mlo);
if(SO324)goto JENKINS_FUNCTION;
if(SO180)goto JENKINS_FUNCTION;
if(WARREN)goto WARREN_FUNCTION;
if(ST)goto ST_FUNCTION;
if(JENKINS)goto JENKINS_FUNCTION;
/* Tinker et al. (2008) for SO as a function of DELTA_HALO
*/
if(DELTA_HALO != prev_delta || prev_cosmo != RESET_COSMOLOGY)
{
initialize_mass_function(&a1,&a2,&a3,&a4);
prev_delta = DELTA_HALO;
prev_cosmo = RESET_COSMOLOGY;
//a4*=1.3;
//a1*=1.15;
fprintf(stderr,"MF PARAMS for DELTA=%f %f %f %f %f\n",DELTA_HALO,a1,a2,a3,a4);
}
n = -a1*(pow(sig/a3,-a2)+1)*exp(-a4/sig/sig)*OMEGA_M*RHO_CRIT/mass/sig*dsdM;
// NB! factor for accounting for satellites
mass = log10(mass)-11;
fac = 1.0;
//fac = 1.1;
//if(mass>0.15)
// fac = pow(mass-0.15,0.5)/(1+exp(pow(mass,1.1))*2)*wpl.satfac + 1;
//printf("NB! altering halo mass function by: %f %f\n",fac,mass);
n = n*fac;
return(n);
/* Jenkins et al. FOF .2 best-fit (unless SO180==1)
*/
JENKINS_FUNCTION:
a=-JENKINS_A*OMEGA_M*RHO_CRIT/mass/sig;
n=a*dsdM*exp(-pow(fabs(JENKINS_B-log(sig)),JENKINS_C));
return(n);
/* Warren et al. (calibrated only on concordance cosmology, FOF.2)
*/
WARREN_FUNCTION:
n = -0.7234*(pow(sig,-1.625)+0.2538)*exp(-1.198/sig/sig)*OMEGA_M*RHO_CRIT/mass/sig*dsdM;
return(n);
ST_FUNCTION:
/* This is a bunch of Sheth-Tormen stuff.
*/
nuprime=0.841*DELTA_CRIT/sig;
nufnu=0.644*(1+1.0/pow(nuprime,0.6))*(sqrt(nuprime*nuprime/2/PI))*exp(-nuprime*nuprime/2);
//n=RHO_CRIT*OMEGA_M/mass*mass*nufnu*fabs(dsdM);
n=RHO_CRIT*OMEGA_M/mass*nufnu*fabs(dsdM)/sig;
return(n);
}
double halo_mass_function(double mass)
{
double sig,logm,a,slo,shi,rm,rlo,rhi,mlo,mhi,dsdM,n,nuprime,nufnu,p,A;
static int flag=0,SO180=0,SO324=0,WARREN=0,ST=0,JENKINS=0,prev_cosmo=0;
static double pnorm, prev_delta;
double btemp = -1;
static double
a1 = 0.325277,
a2 = 0.492785,
a3 = 0.310289,
a4 = 1.317104,
a5 = 2.425681;
/* Jenkins et al. SO 180 best-fit
*/
if(SO180)
{
JENKINS_A = 0.301;
JENKINS_B = 0.64;
JENKINS_C = 3.82;
}
if(SO324)
{
JENKINS_A = 0.316;
JENKINS_B = 0.67;
JENKINS_C = 3.82;
}
if(JENKINS) //their .2 fof function
{
JENKINS_A = 0.315;
JENKINS_B = 0.61;
JENKINS_C = 3.8;
}
/* First normalize the power spectrum
*/
pnorm=SIGMA_8/sigmac(8.0);
rm=pow(3.0*mass/(4.0*PI*OMEGA_M*RHO_CRIT),1.0/3.0);
sig=pnorm*sigmac(rm);
logm=log10(mass);
mlo=0.99*mass;
mhi=1.01*mass;
rlo=pow(3.0*mlo/(4.0*PI*OMEGA_M*RHO_CRIT),1.0/3.0);
rhi=pow(3.0*mhi/(4.0*PI*OMEGA_M*RHO_CRIT),1.0/3.0);
slo=pnorm*sigmac(rlo);
shi=pnorm*sigmac(rhi);
dsdM=(shi-slo)/(mhi-mlo);
if(SO324)goto JENKINS_FUNCTION;
if(SO180)goto JENKINS_FUNCTION;
if(WARREN)goto WARREN_FUNCTION;
if(ST)goto ST_FUNCTION;
if(JENKINS)goto JENKINS_FUNCTION;
/* Tinker et al. (in prep) for SO 200
*/
if(DELTA_HALO != prev_delta || prev_cosmo != RESET_COSMOLOGY)
{
initialize_mass_function(&a1,&a2,&a3,&a4);
prev_delta = DELTA_HALO;
prev_cosmo = RESET_COSMOLOGY;
// if we're using systematic errors in an MCMC, adjust parameter a1 (amplitude)
if(USE_ERRORS)
a1 *= M2N.mf_amp;
fprintf(stderr,"MF PARAMS for DELTA=%f %f %f %f %f\n",DELTA_HALO,a1,a2,a3,a4);
}
n = -a1*(pow(sig/a3,-a2)+1)*exp(-a4/sig/sig)*OMEGA_M*RHO_CRIT/mass/sig*dsdM;
return(n);
/* Jenkins et al. FOF .2 best-fit (unless SO180==1)
*/
JENKINS_FUNCTION:
a=-JENKINS_A*OMEGA_M*RHO_CRIT/mass/sig;
n=a*dsdM*exp(-pow(fabs(JENKINS_B-log(sig)),JENKINS_C));
return(n);
/* Warren et al. (calibrated only on concordance cosmology, FOF.2)
*/
WARREN_FUNCTION:
n = -0.7234*(pow(sig,-1.625)+0.2538)*exp(-1.198/sig/sig)*OMEGA_M*RHO_CRIT/mass/sig*dsdM;
return(n);
/* Need to find the derivative dlog(sig)/dlog(M)
*/
mlo=0.99*logm;
mhi=1.01*logm;
rlo=pow(3.0*pow(10.0,mlo)/(4.0*PI*OMEGA_M*RHO_CRIT),1.0/3.0);
rhi=pow(3.0*pow(10.0,mhi)/(4.0*PI*OMEGA_M*RHO_CRIT),1.0/3.0);
slo=log10(pnorm*sigmac(rlo));
shi=log10(pnorm*sigmac(rhi));
dsdM=(shi-slo)/(mhi-mlo);
ST_FUNCTION:
/* This is a bunch of Sheth-Tormen stuff.
* NB! because I'm skipping the above derivative (dlogs/dlogM), i'm using the lower
*/
nuprime=0.841*DELTA_CRIT/sig;
nufnu=0.644*(1+1.0/pow(nuprime,0.6))*(sqrt(nuprime*nuprime/2/PI))*exp(-nuprime*nuprime/2);
//n=RHO_CRIT*OMEGA_M/mass*mass*nufnu*fabs(dsdM);
n=RHO_CRIT*OMEGA_M/mass*nufnu*fabs(dsdM)/sig;
return(n);
}
