wnw_split.c File Reference

Documented wiggle-nowiggle split based on 3d Gaussian filter in linear k, and using the Eisentein-Hu wiggle-no wiggle template arXiv:astro-ph/9709112. More...

#include "header.h"

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Functions
double	pk_Gfilter_nw (struct Cosmology *Cx, double k, double k0)
	Compute the nowiggle component of linear matter power spectrum using 3d Gaussian filter Computing the nowiggle component involves calculating an integral (Eq. More...
double	pk_nw_integrand (double x, void *par)
	Integrand to compute the nowiggle matter power spectrum. More...
double	EH_PS_w (struct Cosmology *Cx, double k, double k0, double pk0)
	Compute the Eisentein-Hu approximate wiggle component of linear matter power spectrum. More...
double	EH_PS_nw (struct Cosmology *Cx, double k, double k0, double pk0)
	Compute the Eisentein-Hu approximate nowiggle component of linear matter power spectrum. More...
double	T0 (struct Cosmology *Cx, double k)
	Compute the no-baryon transfer function given in Eq. More...
double	T (struct Cosmology *Cx, double k)
	Compute the total baryon+CDM transfer function. More...
double	Tt0 (struct Cosmology *Cx, double k, double x1, double x2)
	Compute the function defined in Eq. More...

Detailed Description

Documented wiggle-nowiggle split based on 3d Gaussian filter in linear k, and using the Eisentein-Hu wiggle-no wiggle template arXiv:astro-ph/9709112.

Azadeh Moradinezhad Dizgah, June 16th 2021

The algorithm closely follows Ref. arXiv:1509.02120 by Vlah et al. (described in Appendix A)

The following function will be called from other modules:

1. pk_Gfilter_nw()

Function Documentation

EH_PS_nw()

double EH_PS_nw	(	struct Cosmology *	Cx,
		double	k,
		double	k0,
		double	pk0
	)

Compute the Eisentein-Hu approximate nowiggle component of linear matter power spectrum.

Parameters

Cx	Input: pointer to Cosmology structure
k	Input: wavenumber in unit of 1/Mpc
k0	Input: smallest value of k, i.e. the largest scale
pk0	Input: value of the power spectrum at the largest scale

Returns

P_nw(k) in unit of (Mpc)^3

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EH_PS_w()

double EH_PS_w	(	struct Cosmology *	Cx,
		double	k,
		double	k0,
		double	pk0
	)

Compute the Eisentein-Hu approximate wiggle component of linear matter power spectrum.

Parameters

Cx	Input: pointer to Cosmology structure
k	Input: wavenumber in unit of 1/Mpc
k0	Input: smallest value of k, i.e. the largest scale
pk0	Input: value of the power spectrum at the largest scale

Returns

P_w(k) in unit of (Mpc)^3

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pk_Gfilter_nw()

double pk_Gfilter_nw	(	struct Cosmology *	Cx,
		double	k,
		double	k0
	)

Compute the nowiggle component of linear matter power spectrum using 3d Gaussian filter Computing the nowiggle component involves calculating an integral (Eq.

A3 of Vlah et al) Below, pk_nw_integrand()is the corresponding integrand and pk_Gfilter_nw() is the integrator

Parameters

Cx	Input: pointer to Cosmology structure
k	Input: wavenumber in unit of 1/Mpc
k0	Input: smallest value of k, i.e. the largest scale

Returns

broadband component in unit of (Mpc)^3

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pk_nw_integrand()

double pk_nw_integrand	(	double	x,
		void *	par
	)

Integrand to compute the nowiggle matter power spectrum.

Parameters

x	Input: integration variable, k-values
par	Input: integration parameters

Returns

integrand to be used in pk_Gfilter_nw() function
integration variable x = logq

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T()

double T	(	struct Cosmology *	Cx,
		double	k
	)

Compute the total baryon+CDM transfer function.

Parameters

Cx	Input: pointer to Cosmology structure
k	Input: wavenumber in unit of 1/Mpc

Returns

value of baryon+cdm transfer function

H0 value devided by the speed of light

approximate sound speed given in Eq. (26) of EH

Eq. 21 of EH ref.

Eq. 17 of EH ref

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T0()

double T0	(	struct Cosmology *	Cx,
		double	k
	)

Compute the no-baryon transfer function given in Eq.

29 of EH ref

Parameters

Cx	Input: pointer to Cosmology structure
k	Input: wavenumber in unit of 1/Mpc

Returns

value of nor-baryon transfer fit

approximate sound speed given in Eq. (26) of EH

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Tt0()

double Tt0	(	struct Cosmology *	Cx,
		double	k,
		double	x1,
		double	x2
	)

Compute the function defined in Eq.

19 of EH ref, which will be used to compute the fit for CDM transfer function in Eq. 17.

Parameters

Cx	Input: pointer to Cosmology structure
k	Input: wavenumber in unit of 1/Mpc.
x1	Input: betac AM:WHAT WAS THIS VARIABLE???
x2	Input: betac AM:WHAT WAS THIS VARIABLE???

Returns

value of the function x1 = alphac, x2 = betac in Eq. 19.

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