/* Reads mass function in from a file and spline interpolates.
*/
double nbody_massfunction(double m)
{
static int flag=0,n;
static double *x,*y,*y2,log10_2,normhi,normlo;
float x1,x2,x3;
int i;
double a,dx;
char aa[1000];
FILE *fp;
if(!flag)
{
log10_2=log10(2.0);
flag++;
if(!(fp=fopen(Files.MassFuncFile,"r")))
endrun("ERROR opening MassFuncFile");
i=0;
n = filesize(fp);
fprintf(stderr,"Read %d lines from [%s]\n",n,Files.MassFuncFile);
x=dvector(1,n);
y=dvector(1,n);
y2=dvector(1,n);
for(i=1;i<=n;++i)
{
fscanf(fp,"%f %f",&x1,&x2);
x[i]=log(x1);
y[i]=log(x2);
fgets(aa,1000,fp);
}
spline(x,y,n,2.0E+30,2.0E+30,y2);
fclose(fp);
fprintf(stderr,"Minimum halo mass in N-body dndM= %e\n",exp(x[1]));
normhi = exp(y[n])/halo_mass_function(exp(x[n]));
normlo = exp(y[1])/halo_mass_function(exp(x[1]));
}
m=log(m);
// if(m>x[n])return(0);
/*if(m<x[1])return(0);*/
splint(x,y,y2,n,m,&a);
return(exp(a));
}
/* It may be a bit costly to run the above function every time you need
* dn/dM, so here we put the values into an array and then interpolate.
*
* The currentrange of masses calculated is 10^9 to 10^16.7. The tabulation is
* done in log(M), so the spline interpolation will perform a power-law fit
* to masses outside this range.
*/
double dndM_interp(double m)
{
static int flag=0,prev_cosmo=0, n;
static double *x,*y,*y2;
int i;
double dm,max=16.7,min=8,a,m1,m2,dm1;
if(!flag || RESET_COSMOLOGY!=prev_cosmo)
{
n = 200;
if(!ThisTask && OUTPUT)
fprintf(stdout,"RESET: resetting mass function for %f %f\n",OMEGA_M,SIGMA_8);
fflush(stdout);
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(halo_mass_function(x[i]));
if(isnan(y[i])) { n = i-1; break; }
if(isinf(y[i])) { n = i-1; break; }
/*
if(DELTA_HALO!=200)
{
//FAKE_DATA: DELTA_HALO==650
m1 = halo_mass_conversion2(x[i]*1.01,halo_c200(x[i]*1.01),200.0,650.0);
m2 = halo_mass_conversion2(x[i]*0.99,halo_c200(x[i]*0.99),200.0,650.0);
dm1 = (x[i]*1.01 - x[i]*0.99)/(m1-m2);
y[i] = y[i] + log(dm1);
x[i]=(halo_mass_conversion2(x[i],halo_c200(x[i]),200.0,650.0));
}
*/
//printf("MF%d %e %e %e\n",RESET_COSMOLOGY,x[i],exp(y[i]),halo_mass_function(x[i]));fflush(stdout);
x[i]=log(x[i]);
continue;
}
spline(x,y,n,2.0E+30,2.0E+30,y2);
prev_cosmo=RESET_COSMOLOGY;
//fprintf(stderr,"MMAX %e\n",exp(x[n]));
}
m=log(m);
if(m>x[n])return 0;
splint(x,y,y2,n,m,&a);
return(exp(a));
}
/* It may be a bit costly to run the above function every time you need
* dn/dM, so here we put the values into an array and then interpolate.
*
* The currentrange of masses calculated is 10^9 to 10^16.7. The tabulation is
* done in log(M), so the spline interpolation will perform a power-law fit
* to masses outside this range.
*/
double dndM_interp(double m)
{
static int flag=0,prev_cosmo=0, n;
static double *x,*y,*y2;
int i;
double dm,max=16.7,min=8,a,m1,m2,dm1;
if(!flag || RESET_COSMOLOGY!=prev_cosmo)
{
n = 200;
if(!ThisTask && OUTPUT)
fprintf(stdout,"RESET: resetting mass function for %f %f\n",OMEGA_M,SIGMA_8);
fflush(stdout);
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(halo_mass_function(x[i]));
//printf("MF%d %e %e\n",RESET_COSMOLOGY,x[i],exp(y[i]));fflush(stdout);
if(isnan(y[i])) { n = i-1; break; }
if(isinf(y[i])) { n = i-1; break; }
x[i]=log(x[i]);
continue;
}
spline(x,y,n,2.0E+30,2.0E+30,y2);
prev_cosmo=RESET_COSMOLOGY;
//fprintf(stderr,"MMAX %e\n",exp(x[n]));
}
m=log(m);
if(m>x[n])return 0;
splint(x,y,y2,n,m,&a);
return(exp(a));
}
