#include <stdlib.h>

#include <stdio.h>

#include <math.h>

#include "header.h"

/* This is a calculation of the differential halo mass function of

* Jenkins et al 2001 (MNRAS 321, 372).

*

*/

void initialize_mass_function2(double *a1, double *a2, double *a3, double *a4, double *a5);

void initialize_mass_function(double *a1, double *a2, double *a3, double *a4);

double every_fucking_observers_mass_function(double mass)

{

double h = HUBBLE;

return dndM_interp(mass/h)*pow(HUBBLE,3.0);

}

/* Just returns f(sigma) for the mass function

*/

double fsigma(double sig)

{

static double a1, a2, a3, a4, a5;

static double pnorm, prev_delta=-1, prev_cosmo=-1;

if(DELTA_HALO != prev_delta || prev_cosmo != RESET_COSMOLOGY)

{

initialize_mass_function2(&a1,&a2,&a3,&a4,&a5);

prev_delta = DELTA_HALO;

prev_cosmo = RESET_COSMOLOGY;

}

return a5*(pow(sig/a3,-a2)+pow(sig,-a1))*exp(-a4/sig/sig);

}

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);

}

/* 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));

}

/* 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));

}

void initialize_mass_function(double *a1, double *a2, double *a3, double *a4)

{

int n = 9, i;

double *x, *y, *z, at, ztemp;

x = dvector(1,n);

y = dvector(1,n);

z = dvector(1,n);

// initialize the overdensities

for(i=1;i<=9;i+=2)

x[i] = log(200*pow(2.0,(i-1.0)/2.0));

for(i=2;i<=9;i+=2)

x[i] = log(300*pow(2.0,(i-2.0)/2.0));

//first parameter

y[1] = 1.858659e-01 ;

y[2] = 1.995973e-01 ;

y[3] = 2.115659e-01 ;

y[4] = 2.184113e-01 ;

y[5] = 2.480968e-01 ;

y[6] = 2.546053e-01 ;

y[7] = 2.600000e-01 ;

y[8] = 2.600000e-01 ;

y[9] = 2.600000e-01 ;

spline(x,y,n,1.0E+30,1.0E+30,z);

splint(x,y,z,n,log(DELTA_HALO),a1);

if(DELTA_HALO>=1600) *a1 = 0.26;

//second parameter

y[1] = 1.466904e+00 ;

y[2] = 1.521782e+00 ;

y[3] = 1.559186e+00 ;

y[4] = 1.614585e+00 ;

y[5] = 1.869936e+00 ;

y[6] = 2.128056e+00 ;

y[7] = 2.301275e+00 ;

y[8] = 2.529241e+00 ;

y[9] = 2.661983e+00 ;

spline(x,y,n,1.0E+30,1.0E+30,z);

splint(x,y,z,n,log(DELTA_HALO),a2);

//third parameter

y[1] = 2.571104e+00 ;

y[2] = 2.254217e+00 ;

y[3] = 2.048674e+00 ;

y[4] = 1.869559e+00 ;

y[5] = 1.588649e+00 ;

y[6] = 1.507134e+00 ;

y[7] = 1.464374e+00 ;

y[8] = 1.436827e+00 ;

y[9] = 1.405210e+00 ;

spline(x,y,n,1.0E+30,1.0E+30,z);

splint(x,y,z,n,log(DELTA_HALO),a3);

//fourth parameter

y[1] = 1.193958e+00;

y[2] = 1.270316e+00;

y[3] = 1.335191e+00;

y[4] = 1.446266e+00;

y[5] = 1.581345e+00;

y[6] = 1.795050e+00;

y[7] = 1.965613e+00;

y[8] = 2.237466e+00;

y[9] = 2.439729e+00;

spline(x,y,n,1.0E+30,1.0E+30,z);

splint(x,y,z,n,log(DELTA_HALO),a4);

// now adjust for redshift

if(!(REDSHIFT>0))return;

ztemp = REDSHIFT;

if(REDSHIFT>3) ztemp = 3.0;

*a1 *= pow(1+ztemp,-0.14);

*a2 *= pow(1+ztemp,-0.14);

at = -pow(0.75/log10(DELTA_HALO/75),1.2);

at = pow(10.0,at);

*a3 *= pow(1+ztemp,-at);

}

/* This is using the normalized mass functions that

* integrate to the mean matter density of the universe

*/

void initialize_mass_function2(double *a1, double *a2, double *a3, double *a4, double *a5)

{

int n = 9, i;

double *x, *y, *z;

x = dvector(1,n);

y = dvector(1,n);

z = dvector(1,n);

// initialize the overdensities

for(i=1;i<=9;i+=2)

x[i] = log(200*pow(2.0,i-1.0));

for(i=2;i<=9;i+=2)

x[i] = log(300*pow(2.0,i-1.0));

//first parameter

y[1] = 5.143873e-01 ;

y[2] = 4.782773e-01 ;

y[3] = 4.773988e-01 ;

y[4] = 4.548802e-01 ;

y[5] = 4.431224e-01 ;

y[6] = 3.982487e-01 ;

y[7] = 3.976351e-01 ;

y[8] = 3.616926e-01 ;

y[9] = 3.282215e-01 ;

spline(x,y,n,1.0E+30,1.0E+30,z);

splint(x,y,z,n,log(DELTA_HALO),a1);

//second parameter

y[1] = 1.973173e+00 ;

y[2] = 2.056993e+00 ;

y[3] = 2.297465e+00 ;

y[4] = 2.563651e+00 ;

y[5] = 2.834270e+00 ;

y[6] = 2.916583e+00 ;

y[7] = 3.294007e+00 ;

y[8] = 3.369249e+00 ;

y[9] = 3.300715e+00 ;

spline(x,y,n,1.0E+30,1.0E+30,z);

splint(x,y,z,n,log(DELTA_HALO),a2);

//third parameter

y[1] = 9.951248e-01 ;

y[2] = 9.895878e-01 ;

y[3] = 9.343687e-01 ;

y[4] = 9.303064e-01 ;

y[5] = 9.588204e-01 ;

y[6] = 1.044357e+00 ;

y[7] = 1.065549e+00 ;

y[8] = 1.119347e+00 ;

y[9] = 1.164469e+00 ;

spline(x,y,n,1.0E+30,1.0E+30,z);

splint(x,y,z,n,log(DELTA_HALO),a3);

//fourth parameter

y[1] = 1.227880e+00 ;

y[2] = 1.310414e+00 ;

y[3] = 1.403302e+00 ;

y[4] = 1.553185e+00 ;

y[5] = 1.701724e+00 ;

y[6] = 1.906987e+00 ;

y[7] = 2.137733e+00 ;

y[8] = 2.394142e+00 ;

y[9] = 2.572204e+00 ;

spline(x,y,n,1.0E+30,1.0E+30,z);

splint(x,y,z,n,log(DELTA_HALO),a4);

//normalization parameter

y[1] = 4.816036e-01 ;

y[2] = 4.660390e-01 ;

y[3] = 4.935099e-01 ;

y[4] = 4.937660e-01 ;

y[5] = 4.960265e-01 ;

y[6] = 4.496969e-01 ;

y[7] = 4.663272e-01 ;

y[8] = 4.288530e-01 ;

y[9] = 3.879745e-01 ;

spline(x,y,n,1.0E+30,1.0E+30,z);

splint(x,y,z,n,log(DELTA_HALO),a5);

//set up mass funciton parameters as globals

/*

MFPARAM1 = *a1;

MFPARAM2 = *a2;

MFPARAM3 = *a3;

MFPARAM4 = *a4;

MFPARAM5 = *a5;

*/

}