mirror of
https://bitbucket.org/cosmicvoids/vide_public.git
synced 2025-07-04 23:31:12 +00:00
first pass at cleaning HOD
This commit is contained in:
P.M. Sutter
parent
134d9b1df6
commit
57715fe0de
24 changed files with 0 additions and 5963 deletions
|
|
@ -1,204 +0,0 @@
|
|||
#include <stdlib.h>
|
||||
#include <stdio.h>
|
||||
#include <math.h>
|
||||
|
||||
#include "header.h"
|
||||
|
||||
/* This is my implementation of the Halo Model fitting function
|
||||
* described in Appendix C of Smith, Peacock, et al. 2003 MNRAS 341, 1311
|
||||
*
|
||||
* Comparison to Smith et al. program halofit.f output is successful.
|
||||
*/
|
||||
|
||||
/* Internal functions
|
||||
*/
|
||||
double func_nl(double r);
|
||||
void tabulate_pk_nl(double *kk, double *pknl, int nk);
|
||||
|
||||
/* This returns the linear power
|
||||
* Delta = 4pi*k^3 P(k)/(2pi)^3
|
||||
*/
|
||||
double linear_power_spectrum(double xk)
|
||||
{
|
||||
static double *kk,*pknl,*y2,pnorm=-1,ahi,bhi;
|
||||
static int flag=1,nk=1000,prev_cosmology=0;
|
||||
double a,psp,x1[4],y1[4];
|
||||
int i;
|
||||
|
||||
if(pnorm<0 || prev_cosmology!=RESET_COSMOLOGY)
|
||||
{
|
||||
pnorm=SIGMA_8/sigmac(8.0);
|
||||
pnorm*=pnorm;
|
||||
prev_cosmology=RESET_COSMOLOGY;
|
||||
}
|
||||
if(ITRANS>0)
|
||||
psp=pow(xk,SPECTRAL_INDX)*pow(transfnc(xk),2.);
|
||||
else
|
||||
psp=pow(xk,SPECTRAL_INDX);
|
||||
psp=psp*pnorm*xk*xk*xk/(2*PI*PI);
|
||||
return(psp);
|
||||
}
|
||||
|
||||
double nonlinear_power_spectrum(double xk)
|
||||
{
|
||||
static double *kk,*pknl,*y2,pnorm=-1,ahi,bhi;
|
||||
static int flag=1,nk=1000,prev_cosmology=0;
|
||||
double a,psp,x1[4],y1[4],xklog;
|
||||
int i;
|
||||
|
||||
if(flag || RESET_COSMOLOGY!=prev_cosmology)
|
||||
{
|
||||
prev_cosmology=RESET_COSMOLOGY;
|
||||
pnorm=SIGMA_8/sigmac(8.0);
|
||||
flag=0;
|
||||
kk=dvector(1,nk);
|
||||
pknl=dvector(1,nk);
|
||||
y2=dvector(1,nk);
|
||||
tabulate_pk_nl(kk,pknl,nk);
|
||||
spline(kk,pknl,nk,1.0E+30,1.0E+30,y2);
|
||||
|
||||
/* This takes the last four points in the power spectrum at high k
|
||||
* and fits a power law to them for extrapolation.
|
||||
*/
|
||||
for(i=0;i<4;++i)
|
||||
{
|
||||
x1[i]=(kk[nk-3+i]);
|
||||
y1[i]=(pknl[nk-3+i]);
|
||||
}
|
||||
least_squares(x1,y1,4,&ahi,&bhi);
|
||||
|
||||
}
|
||||
|
||||
xklog=log(xk);
|
||||
|
||||
/* If xk is less than the smallest k value tabulates, return linear power.
|
||||
*/
|
||||
if(xklog<kk[1])
|
||||
return(linear_power_spectrum(xk));
|
||||
|
||||
/* If xk larger than highest k, return extrapolation.
|
||||
*/
|
||||
if(xklog>kk[nk])
|
||||
return((exp((ahi+bhi*xklog))));
|
||||
|
||||
splint(kk,pknl,y2,nk,xklog,&a);
|
||||
return(exp(a));
|
||||
|
||||
}
|
||||
void tabulate_pk_nl(double *kk, double *pknl, int nk)
|
||||
{
|
||||
double r_nl,pnorm,DeltaQ,DeltaLin,DeltaH,psp,neff,s1,s2,n1,n2,ncurve,
|
||||
lnk_lo,lnk_hi,dlnk,xk1,y,xk,fy;
|
||||
double an,bn,cn,f1b,f2b,f3b,alpha,beta,gamma,nu,mu;
|
||||
int i,j,n=10000;
|
||||
|
||||
/* First normalize the linear power spectrum.
|
||||
*/
|
||||
pnorm=SIGMA_8/sigmac(8.0);
|
||||
|
||||
/* Calculate the non-linear scale.
|
||||
*/
|
||||
r_nl = exp(zbrent(func_nl,log(0.01),log(10.0),1.0E-4));
|
||||
if(OUTPUT)
|
||||
fprintf(stdout,"R_NL= %f\n",r_nl);
|
||||
|
||||
/* Calculate the effective spectral index at the non-linear scale.
|
||||
*/
|
||||
s1=pnorm*sigmac(-r_nl*0.999);
|
||||
s2=pnorm*sigmac(-r_nl*1.001);
|
||||
neff=-(3+2*(s2-s1)/0.002);
|
||||
if(OUTPUT)
|
||||
fprintf(stderr,"neff= %f\n",neff);
|
||||
|
||||
/* Spectral curvature.
|
||||
*/
|
||||
lnk_hi=10.0;
|
||||
lnk_lo=-10.0;
|
||||
dlnk=(lnk_hi-lnk_lo)/n;
|
||||
s1=0;
|
||||
for(i=1;i<=n;++i)
|
||||
{
|
||||
xk1=exp(lnk_lo+(i-0.5)*dlnk);
|
||||
y=xk1*r_nl;
|
||||
DeltaLin=linear_power_spectrum(xk1);
|
||||
s1+=DeltaLin*y*y*(1-y*y)*exp(-y*y)*dlnk;
|
||||
}
|
||||
ncurve=(3+neff)*(3+neff)+4*s1;
|
||||
if(OUTPUT)
|
||||
fprintf(stderr,"ncurve= %f\n",ncurve);
|
||||
|
||||
/* Coefficients of the model.
|
||||
*/
|
||||
an=pow(10.0,1.4861 + 1.8369*neff + 1.6762*neff*neff + 0.7940*neff*neff*neff +
|
||||
0.1670*pow(neff,4.0) - 0.6202*ncurve);
|
||||
bn=pow(10.0,0.9463 + 0.9466*neff + 0.3084*neff*neff - 0.9400*ncurve);
|
||||
|
||||
cn= pow(10.0,-0.2807 + 0.6669*neff + 0.3214*neff*neff - 0.0793*ncurve);
|
||||
|
||||
gamma = 0.8649 + 0.2989*neff + 0.1631*ncurve;
|
||||
alpha = 1.3884 + 0.3700*neff - 0.1452*neff*neff;
|
||||
beta = 0.8291 + 0.9854*neff + 0.3401*neff*neff;
|
||||
mu = pow(10.0,-3.5442 + 0.1908*neff);
|
||||
nu = pow(10.0, 0.9589 + 1.2857*neff);
|
||||
|
||||
/* Testing the parameter dependence.
|
||||
* TESTING TESTING
|
||||
*/
|
||||
/*
|
||||
alpha *= 0.3;
|
||||
beta *= 0.3;
|
||||
*/
|
||||
|
||||
/* Omega-dependent functions (FLAT LAMBDA COSMOLOGY)
|
||||
*/
|
||||
f1b = pow(OMEGA_M,-0.0307);
|
||||
f2b = pow(OMEGA_M,-0.0585);
|
||||
f3b = pow(OMEGA_M,+0.0743);
|
||||
|
||||
|
||||
/* Tabulate the power spectrum
|
||||
*/
|
||||
lnk_lo=log(0.001);
|
||||
lnk_hi=log(1000.0);
|
||||
dlnk=(lnk_hi-lnk_lo)/(nk-1);
|
||||
|
||||
for(i=1;i<=nk;++i)
|
||||
{
|
||||
xk=exp(lnk_lo+(i-1)*dlnk);
|
||||
y=xk*r_nl;
|
||||
fy=y/4.0 + y*y/8.0;
|
||||
|
||||
/* TEST */
|
||||
/* fy*=1.2; */
|
||||
|
||||
DeltaLin=linear_power_spectrum(xk);
|
||||
|
||||
DeltaQ = DeltaLin*pow(1+DeltaLin,beta)/(1+alpha*DeltaLin)*exp(-fy);
|
||||
|
||||
DeltaH = an*pow(y,3*f1b)/(1+bn*pow(y,f2b)+pow(cn*f3b*y,3-gamma));
|
||||
|
||||
DeltaH*= 1.0/(1+mu/y+nu/(y*y));
|
||||
|
||||
kk[i]=log(xk);
|
||||
pknl[i]=log(DeltaQ + DeltaH);
|
||||
}
|
||||
}
|
||||
|
||||
/* This is a function to find the non-linear scale. Similar to M_star,
|
||||
* but here we're using a Guassian smoothing window rather than top hat.
|
||||
* (And we're finding the scale at which the variance = 1, not 1.686).
|
||||
*/
|
||||
double func_nl(double r)
|
||||
{
|
||||
static int prev_cosmology=0;
|
||||
double sig;
|
||||
static double pnorm=-1;
|
||||
|
||||
if(pnorm<0 || RESET_COSMOLOGY!=prev_cosmology)
|
||||
pnorm=SIGMA_8/sigmac(8.0);
|
||||
prev_cosmology=RESET_COSMOLOGY;
|
||||
|
||||
r=exp(r);
|
||||
sig=pnorm*sigmac(-r);
|
||||
return sig-1.0;
|
||||
}
|
||||
Loading…
Add table
Add a link
Reference in a new issue