/* THis is the integrand of the mean number integral:
* dM dn/dM P(N_gals|M) N_true(M)
*
* NB! need to do a correction for the fact that the radius for N
* isn't R200 exactly for all masses-- it's R200 for the mean mass in the bin.
*
*/
double m2n_func2(double m)
{
int i;
double x, logm, mu, sig, c, rvir, rs, rhos, nsat, logj;
logm = m;
m = exp(m);
i = M2N.current_bin;
logj = log(M2N.current_Ngals);
//mu = exp(-0.12)*pow(M2N.current_Ngals/40.0,1.15);
//mu = B_rozo + alpha_rozo*log(M2N.current_Ngals/40.0) + log(4e14*HUBBLE);
sig = sig_rozo;
mu = B_rozo - sig*sig/2 + alpha_rozo*(logm-log(1.0e14*HUBBLE)) + log(40.0);
x = exp(-(mu - logj)*(mu - logj)/(2*sig*sig))/(RT2PI*sig)/m;
// extrapolate the HOD profile out/in to the mean radius of the bin
c = CVIR_FAC*halo_concentration(m);
rvir = pow(3*m/(4*PI*RHO_CRIT*OMEGA_M*DELTA_HALO),THIRD);
rs = rvir/c;
rhos = N_sat(m)/(4*PI*rvir*rvir*rvir*HK_func(rs/rvir));
nsat = 4*PI*rhos*pow(M2N.radius[i],3.0)*HK_func(rs/M2N.radius[i]);
//printf("%e %e %e %e\n",m,rvir,M2N.radius[i],nsat/N_sat(m));
return m*nsat*dndM_interp(m)*x;
}
/* Same as above, only now we're calculating the number of pairs
* in the cross-correlation.
*
* NB! -- We're assuming that the satellite galaxy profiles
* of both HODs are the same.
*/
double func1_xcorr(double m)
{
double N,n,fac2,rvir,f_ss=0,f_cs=0,cvir,x,rfof,ncen1,nsat1,ncen2,nsat2;
m=exp(m);
cvir=halo_concentration(m)*CVIR_FAC;
n=dndM_interp(m);
nsat1=N_sat(m);
ncen1=N_cen(m);
nsat2=N_sat2(m);
ncen2=N_cen2(m);
rvir=2*pow(3.0*m/(4*DELTA_HALO*PI*OMEGA_M*RHO_CRIT),1.0/3.0);
/* Break up the contribution of pairs into
* central-satellite (cs) and satellite-satellite (ss) pairs.
* But for x-corr, we have c1-s2, c2-s1, s1-s2.
*/
f_ss=dFdx_ss(r_g2/rvir,cvir)*nsat1*nsat2;
f_cs=dFdx_cs(r_g2/rvir,cvir)*(nsat1*ncen2 + nsat2*ncen1);
x=n*(f_ss+f_cs)/rvir*m;
return(x);
}
double func1cs(double m)
{
double N,n,fac2,rvir,f_ss,f_cs,cvir,x,rfof,ncen,nsat;
m=exp(m);
cvir=halo_concentration(m)*CVIR_FAC;
n=dndM_interp(m);
nsat=N_sat(m);
ncen=N_cen(m);
rvir=2*pow(3.0*m/(4*DELTA_HALO*PI*OMEGA_M*RHO_CRIT),1.0/3.0);
/* Break up the contribution of pairs into
* central-satellite (cs) and satellite-satellite (ss) pairs.
*/
f_cs=dFdx_cs(r_g2/rvir,cvir)*nsat*ncen;
x=n*(f_cs)/rvir*m;
// if(OUTPUT==3)
// printf("%e %e %e %e %e\n",m,n,f_ss,f_cs,rvir);
return(x);
}
double func_central_bias(double m)
{
double n1,n2,m0;
m=exp(m);
n1=dndM_interp(m);
n2=N_cen(m);
return(n1*n2*m*bias_interp(m,-1));
}
/* This is a copy of the above function that can be called from any routine.
* (But this one integrates over dlogm).
*/
double func_halo_density(double m)
{
double n1;
m=exp(m);
n1=dndM_interp(m);
return(n1*m);
}
double func_mean_halo_mass(double m)
{
double n1,n2,m0;
m=exp(m);
n1=dndM_interp(m);
n2=N_avg(m);
return(n1*n2*m*m);
}
void analytic_sham()
{
int i,j,k,nlogm=400,imag,nmag,jmin;
double dlogm,halocnt[401],magcnt[200],subcnt[401],m,msub,n1,mlow,dmag,magmin,nsub;
double *hmass, *mag, *yy;
dmag = 0.2;
magmin = -18.0;
nmag = 5/dmag;
for(i=0;i<200;++i)
magcnt[i] = 0;
hmass = dvector(1,nlogm);
mag = dvector(1,nlogm);
yy = dvector(1,nlogm);
mlow = HOD.M_low;
for(i=1;i<=nlogm;++i)
halocnt[i] = subcnt[i] = 0;
// go through the mass function to find TOTAL number of halos
dlogm = log(HOD.M_max/mlow)/nlogm;
// get all HOD
HOD.mass_shift = 0;
HOD.fredc = 0.44;
HOD.mass_shift = 0.6616;
HOD.fredc = 1.00;
HOD.mass_shift = 0.2;
HOD.fredc = 0.66;
for(i=1;i<=nlogm;++i)
{
m = exp(dlogm*(i-0.5))*mlow;
halocnt[i] += dndM_interp(m)*m*dlogm;
n1 = 0;
for(j=1;j<=nlogm;++j)
{
msub = exp(dlogm*(j-0.5))*mlow;
if(msub>m/3)continue; // no subhalo greater than half total mass
//n1 = pow(m,0.5)/2.6*pow(msub,-1.5)*exp(-pow(msub/m/0.7,6))*dlogm*m/2; //original +2
//n1 = pow(m,0.7)/2.6*pow(msub,-1.7)*exp(-pow(msub/m/0.7,6))*dlogm*m/3.16;
n1 = pow(msub,-2)*m*m*dlogm*15.7*HOD.M1;
halocnt[0] += n1;
subcnt[0] += N_cen(msub)*n1;
}
//printf("%e %e %e\n",m,N_sat(m),n1);
}
printf("%f\n",subcnt[0]/halocnt[0]);
exit(0);
}
/* This is a copy of the above function that can be called from any routine.
* (But this one integrates over dlogm
*/
double func_galaxy_density(double m)
{
double n1,n2,m0;
m=exp(m);
n1=dndM_interp(m);
n2=N_avg(m);
//fprintf(stdout,"%e %e %e\n",m,n1,n2);
return(n1*n2*m);
}
double func2_m2n(double m)
{
double ncen,nsat,x;
m = exp(m);
ncen = N_cen(m);
nsat = N_sat(m);
x = poisson_prob(g31_number-1,nsat);
if(isnan(x))x = 0;
return ncen*x*m*dndM_interp(m);
}
double m2n_func1a(double m)
{
int i;
double x, logm, mu, sig, c, rvir, rs, rhos, mtrue, logj;
logm = m;
m = exp(m);
i = M2N.current_bin;
logj = log(M2N.current_Ngals);
sig = sig_rozo;
mu = B_rozo - sig*sig/2 + alpha_rozo*(logm-log(1.0e14*HUBBLE)) + log(40.0);
x = exp(-(mu - logj)*(mu - logj)/(2*sig*sig))/(RT2PI*sig)/m;
return m*m*dndM_interp(m)*x;
}
/* THis is the integrand of the number of systems
* dM dn/dM P(N_gals|M)
*
*/
double m2n_func3(double m)
{
int i;
double x, logm, mu, sig, logj;
logm = m;
m = exp(m);
logj = log(M2N.current_Ngals);
//mu = exp(-0.12)*pow(M2N.current_Ngals/40.0,1.15);
sig = sig_rozo;
mu = B_rozo - sig*sig/2 + alpha_rozo*(logm-log(1.0e14*HUBBLE)) + log(40.0);
x = exp(-(mu - logj)*(mu - logj)/(2*sig*sig))/(RT2PI*sig)/m;
//printf("%e %e %e %f %f\n",m,dndM_interp(m),x,mu,logm);
return m*dndM_interp(m)*x;
}
/* This is the function passed to qromo in the above routine.
* It is the number density of
* galaxy pairs in halos of mass m at separation r_g2.
* See Equation (11) from Berlind & Weinberg.
*/
double func1(double m)
{
double N,n,fac2,rvir,f_ss,f_cs,cvir,x,rfof,ncen,nsat,ss;
m=exp(m);
cvir=halo_concentration(m)*CVIR_FAC;
n=dndM_interp(m);
nsat=N_sat(m);
ncen=N_cen(m);
rvir=2*pow(3.0*m/(4*DELTA_HALO*PI*OMEGA_M*RHO_CRIT),1.0/3.0);
/* Break up the contribution of pairs into
* central-satellite (cs) and satellite-satellite (ss) pairs.
*/
f_ss=dFdx_ss(r_g2/rvir,cvir)*moment_ss(m)*0.5;
f_cs=dFdx_cs(r_g2/rvir,cvir)*nsat*ncen;
x=n*(f_ss+f_cs)/rvir*m;
// only send the cs term
//x = n*f_cs/rvir*m;
// only send the ss term
//x = n*f_ss/rvir*m;
// HAMANA
/*
ss = moment_ss(m);
if(ss>1)
return x;
else
return n*dFdx_cs(r_g2/rvir,cvir)*moment_ss(m)*0.5/rvir*m;
*/
// if(OUTPUT==3)
// printf("%e %e %e %e %e\n",m,n,f_ss,f_cs,rvir);
return(x);
}
void output_halo_mass_function()
{
int k,nr=100;
double x,dlogm,m,mvir,cdelta,mmin=1e8,mmax=1e16,delta_vir;
FILE *fp;
char aa[100];
fprintf(stderr,"\n\nCALCULATING HALO MASS FUNCTION.\n");
fprintf(stderr, "-------------------------------\n\n");
sprintf(aa,"%s.massfunc",Task.root_filename);
fp = fopen(aa,"w");
dlogm = (log(mmax) - log(mmin))/(nr-1);
for(k=0;k<nr;++k)
{
m = exp(k*dlogm)*mmin;
x = dndM_interp(m);
fprintf(fp,"%e %e\n",m,x);
}
fclose(fp);
}
/* This function is to be passed to qromo to integrate the number density
* of satellite galaxies.
*/
double func_satfrac(double m)
{
m=exp(m);
return(N_sat(m)*dndM_interp(m)*m);
}
/* This is a function to set the HOD parameters until
* I get some input code or batch file set up.
*
*/
void set_HOD_params()
{
int i,j=1;
double m,error=1.0,tol=1.0E-4,prev,s1,mlo;
/* If the mass function at M_max is undefined, reset M_max
*/
//LOCAL_DENSITY = -0.2;
if(LOCAL_DENSITY!=0)
{
HOD.M_max = 1.0E16;
while(dndM_interp(HOD.M_max)<=0)
{
HOD.M_max*=0.9;
}
fprintf(stderr,"NEW M_max= %e\n",HOD.M_max);
}
if(HOD.pdfc == 2 || HOD.pdfc == 3 || HOD.pdfc == 6 || HOD.pdfc == 8 || HOD.pdfc == 9 || HOD.pdfc == 12 || HOD.pdfc == 13)
SOFT_CENTRAL_CUTOFF=1;
/* Error trap both the galaxy density and M_min both left unspecified.
*/
if(HOD.M_min<=0 && GALAXY_DENSITY<=0 && HOD.free[0]==0)
endrun("ERROR: Must specify either M_min or GALAXY_DENSITY");
/* If the user has specified M_min and M1, calculate the galaxy density.
*/
if(HOD.M_min>0 && HOD.M1>0)
{
HOD.M_low = -1;
if (wp.ngal==0) wp.ngal = GALAXY_DENSITY;
if(SOFT_CENTRAL_CUTOFF)
HOD.M_low0 = HOD.M_low = exp(zbrent(func_mlow,log(HOD.M_min*1.0E-6),log(HOD.M_min*1.1),1.0E-5));
else
HOD.M_low0 = HOD.M_low = HOD.M_min;
if(HOD.M_low > HOD.M1 ) {
while(N_cen(HOD.M_low) > 0.01) HOD.M_low /= 2.;
}
//if(HOD.M_low < HOD.M_min/100.) HOD.M_low = HOD.M_min/100.;
GALAXY_DENSITY=qromo(func_galaxy_density,log(HOD.M_low),log(HOD.M_max),midpnt);
if(OUTPUT) {
fprintf(stdout,"M_low= %e\n",HOD.M_low);
fprintf(stdout,"ng= %e\n",GALAXY_DENSITY); }
}
/* If M_min<=0 then use the specified galaxy density to calculate M_min
*/
if(HOD.M_min<=0)
{
if(HOD.pdfc==7 && HOD.pdfc==8)
HOD.M_min=pow(10.0,zbrent(fixfunc1,8.0,log10(HOD.M_cen_max*0.99),1.0E-5));
else
HOD.M_min=pow(10.0,zbrent(fixfunc1,7.0,14.8,1.0E-5));
if(OUTPUT) fprintf(stderr,"SOFT_CENTRAL_CUTOFF Delta-n %d %e\n",SOFT_CENTRAL_CUTOFF,
fixfunc1(log10(HOD.M_min)));
HOD.M_low = -1;
if(SOFT_CENTRAL_CUTOFF) {
//HOD.M_low = exp(zbrent(func_mlow,log(HOD.M_min)-5*HOD.sigma_logM*2.3,
// log(HOD.M_min),1.0E-5));
HOD.M_low = HOD.M_min/2.;
while(N_cen(HOD.M_low) > 0.01)
HOD.M_low /= 2.;
} else
HOD.M_low = HOD.M_min;
if(HOD.M_low<1.0E7)HOD.M_low=1.0E+7;
if(OUTPUT) {
fprintf(stdout,"M_min %e [ng= %e]\n",HOD.M_min,GALAXY_DENSITY);
fprintf(stdout,"M_low= %e\n",HOD.M_low); }
}
/* If M1<=0 then use the specified galaxy density to calculate M1
*/
if(HOD.M1<=0)
{
HOD.M_low = -1;
if(SOFT_CENTRAL_CUTOFF)
HOD.M_low = exp(zbrent(func_mlow,log(HOD.M_min)-5*HOD.sigma_logM*2.3,
log(HOD.M_min*1.1),1.0E-5));
else
HOD.M_low = HOD.M_min;
if(HOD.M_low<1.0E7)HOD.M_low=1.0E+7;
HOD.M1=pow(10.0,zbrent(fixfunc2,log10(HOD.M_low),15.8,1.0E-5));
if(OUTPUT) {
fprintf(stdout,"M1 %e [ng= %e]\n",HOD.M1,GALAXY_DENSITY);
fprintf(stdout,"M_min = %e M_low= %e\n",HOD.M_min,HOD.M_low); }
}
/* Set the number of halo mass bins we've got.
*/
NUM_POW2MASS_BINS=log(HOD.M_max/HOD.M_low)/LN_2+1;
if(HOD.pdfc==6)
HOD.M_hi = set_high_central_mass();
HOD.M_low0 = set_low_mass();
return;
}
void output_drg_lf(int iout)
{
FILE *fp;
char fname[100];
int i,j,k,nlogm=400,imag,nmag,jmin;
double dlogm,halocnt[401],magcnt[200],m,msub,n1,mlow,dmag,magmin,nsub;
double *hmass, *mag, *yy;
dmag = 0.2;
magmin = -18.0;
nmag = 5/dmag;
for(i=0;i<200;++i)
magcnt[i] = 0;
hmass = dvector(1,nlogm);
mag = dvector(1,nlogm);
yy = dvector(1,nlogm);
mlow = HOD.M_low/5.0;
for(i=1;i<=nlogm;++i)
halocnt[i] = 0;
// go through the mass function to find TOTAL number of halos
dlogm = log(HOD.M_max/mlow)/nlogm;
for(i=1;i<=nlogm;++i)
{
m = exp(dlogm*(i-0.5))*mlow;
halocnt[i] += dndM_interp(m)*m*dlogm;
for(j=1;j<=nlogm;++j)
{
msub = exp(dlogm*(j-0.5))*mlow;
if(msub>m/2)continue; // no subhalo greater than half total mass
// charlie's fit (with extra factor of log(10)?)
halocnt[j] += 0.02*log(10)*pow(msub/m,-0.9)*exp(-msub/(2*m))*dlogm*dndM_interp(m)*m*dlogm;
// gao et al 2004-- gives ~4% at M=1e12 z=0.
//halocnt[i] += 6.3e-4*pow(msub,-1.9)*m*msub*dlogm*dndM_interp(m)*m*dlogm;
}
}
// make it cumulative
// and associate a magnitude at every mass.
mag[nlogm] = mag_at_fixed_ngal(halocnt[nlogm]);
hmass[nlogm] = exp(dlogm*(nlogm-0.5)*mlow);
for(i=nlogm-1;i>=1;--i)
{
halocnt[i] += halocnt[i+1];
mag[i] = mag_at_fixed_ngal(halocnt[i]);
hmass[i] = exp(dlogm*(i-0.5))*mlow;
//printf("CNT %e %e %e\n",hmass[i],halocnt[i],lf_number_density(-27.9,-2.0));
}
// prepare for spline interpolation
spline(hmass,mag,nlogm,1.0E+30,1.0E+30,yy);
// now go through HOD and create the DRG luminosity function
for(i=1;i<=nlogm-1;++i)
{
m = hmass[i];
if(m<HOD.M_low)continue;
imag = (magmin-mag[i])/dmag+1;
//printf("%e\n",magcnt[i]);
magcnt[imag] += N_cen(m)*dndM_interp(m)*dlogm*m;
//printf("%e %f %d %e %e %e %e %e\n",m,mag[i],imag,magcnt[imag],N_cen(m),m,dlogm,dndM_interp(m));
//continue;
// find the minimum subhalo mass
nsub = 0;
for(j=nlogm;j>=1;--j)
{
msub = hmass[j];
if(msub>m/2)continue;
nsub += 0.02*log(10)*pow(msub/m,-0.9)*exp(msub/(2*m))*dlogm;
if(nsub>N_sat(m)/HOD.freds) break;
}
if(j==nlogm)continue;
jmin = j;
if(jmin>=0)
{
printf("ERR %d %e %e %e %e %f\n",j,m,msub,nsub,N_sat(m)/HOD.freds,mag[jmin]);
}
// go through the satellites
for(j=jmin;j<=nlogm;++j)
{
msub = hmass[j];
if(msub>m/2)break;
imag = (magmin-mag[j])/dmag+1;
magcnt[imag] += HOD.freds*0.02*log(10)*pow(msub/m,-0.9)*exp(msub/(2*m))*dlogm*dndM_interp(m)*m*dlogm;
}
}
// print out the results
sprintf(fname,"drg_lf.%d",iout);
fp = fopen(fname,"w");
n1 = 0;
for(i=0;i<200;++i)
{
if(-(i-0.5)*dmag+magmin >-21.6)continue;
magcnt[i]/=dmag;
if(magcnt[i]>0)
fprintf(fp,"%f %e\n",-(i-0.5)*dmag + magmin,magcnt[i]);
n1 += magcnt[i]*dmag;
}
printf("TOTAL ngal = %e\n",n1);
fclose(fp);
}
double every_fucking_observers_mass_function(double mass)
{
double h = HUBBLE;
return dndM_interp(mass/h)*pow(HUBBLE,3.0);
}
double funcxx1(double m)
{
m=exp(m);
return(m*N_avg(m)*dndM_interp(m)*m);
}
double funcxx2(double m)
{
m=exp(m);
return(m*N_cen(m)*dndM_interp(m)*m);
}
// this is to calculate the numer-weighted mass of DRG galaxies
double func_drg1(double m)
{
m = exp(m);
return N_cen(m)*m*dndM_interp(m)*m;
}
/* This function is to be passed to qromo to integrate the number density
* of satellite galaxies.
*/
double func_satellite_density(double m)
{
m=exp(m);
return(N_sat(m)*dndM_interp(m)*m);
}
/* This is the integrand which qromo or qtrap would call
* to calculate the large-scale galaxy bias.
* The integral is a number-weighted average of the halo
* bias function, integrated over the halo mass function.
*/
double func_galaxy_bias(double m)
{
m=exp(m);
return(dndM_interp(m)*N_avg(m)*bias_interp(m,-1.)*m);
}
/* This function is to be passed to qromo to integrate the number density
* of satellite galaxies.
*/
double func_central_density(double m)
{
m=exp(m);
return(N_cen(m)*dndM_interp(m)*m);
}