void output_halo_correlation_function(double mass)
{
int k,nr=50;
double dlogr,r,xlin,xnl,rmin = 0.15,rmax = 40.0;
FILE *fp;
char aa[100];
fprintf(stderr,"\n\nCALCULATING HALO CORRELATION FUNCTIONION (M=%.2e)\n",mass);
fprintf(stderr, "-------------------------------------------------\n\n");
sprintf(aa,"%s.halo_xi",Task.root_filename);
fp = fopen(aa,"w");
rmin = pow(3*mass/(4*DELTA_HALO*PI*RHO_CRIT*OMEGA_M),THIRD);
dlogr = (log(rmax) - log(rmin))/(nr-1);
for(k=0;k<nr;++k)
{
r = exp(k*dlogr)*rmin;
xlin = bias_interp(mass,r);
xnl = xi_interp(r);
fprintf(fp,"%e %e\n",r,xnl*xlin*xlin);
}
fclose(fp);
}
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 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);
}
