Documented IR_res module. More...

#include "header.h"

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Functions
double	pm_IR_LO (struct Cosmology *Cx, double k, double z, long SPLIT)
	Compute the leading-order IR-resummed matter power spectrum, ala Ivanovic et al. More...

double	pm_IR_NLO (struct Cosmology *Cx, double k, double z, long SPLIT)
	Compute the next-to-leading-order IR-resummed matter power spectrum, ala Ivanovic et al. More...

double	IR_Sigma2_integrand (double x, void *par)
	Integrand to compute the suppression factor IR_sigma2. More...

double	IR_Sigma2 (struct Cosmology *Cx, double z, double k0, long SPLIT)
	Compute the suppression factor IR_sigma2. More...

double	pm_nowiggle (struct Cosmology *Cx, double k, double z, double k0, int cleanup, long SPLIT)
	Compute the no-wiggle componenet of the matter power spectrum. More...

double	pm_nowiggle_bspline (struct Cosmology *Cx, double k, double z, int cleanup)
	Compute the no-wiggle componenet of the matter power spectrum, reading in and interpolating the output of apython code which computed the broadband by fitting families of Bsplines (see Vlah et al 2015) More...

double	pm_nowiggle_gfilter (struct Cosmology *Cx, double k, double z, int cleanup)
	Compute the no-wiggle componenet of the matter power spectrum, using Gaussian filter (see Vlah et al 2015) More...

double	pm_nowiggle_dst (struct Cosmology *Cx, double k, double z, int cleanup)
	Compute the no-wiggle componenet of the matter power spectrum, reading in and interpolating the output of apython code which computed the broadband by discrete sin-transform, See Hamann et al 2010. More...

Detailed Description

Documented IR_res module.

Azadeh Moradinezhad Dizgah, November 4th 2021

This module is computes the leading and next-to-leading IR-resummed matter power spectrum The wiggle-nowiggle seperation is performed in wnw_split.c module.

In summary, the following functions can be called from other modules:

Function Documentation

◆ IR_Sigma2()

double IR_Sigma2	(	struct Cosmology *	Cx,
		double	z,
		double	k0,
		long	SPLIT
	)

Compute the suppression factor IR_sigma2.

Parameters

Cx	Input: pointer to cosmology structure
z	Input: redshift
k0	Input: first element of the k-array, used in normalization of EH no-wiggle spectrum
SPLIT	Input: switch to set the method of wiggle-nowiggle split

Returns: value of IR resummation suppression factor

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◆ IR_Sigma2_integrand()

double IR_Sigma2_integrand	(	double	x,
		void *	par
	)

Integrand to compute the suppression factor IR_sigma2.

Parameters

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

Returns: integrand to be used in IR_sigma2() function

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◆ pm_IR_LO()

double pm_IR_LO	(	struct Cosmology *	Cx,
		double	k,
		double	z,
		long	SPLIT
	)

Compute the leading-order IR-resummed matter power spectrum, ala Ivanovic et al.

Parameters

Cx	Input: pointer to cosmology structure
k	Input: wavenumber in unit of 1/Mpc.
z	Input: redshift
SPLIT	Input: switch to set the method of wiggle-nowiggle split

Returns: value of leading IR-ressumed power spectrum

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◆ pm_IR_NLO()

double pm_IR_NLO	(	struct Cosmology *	Cx,
		double	k,
		double	z,
		long	SPLIT
	)

Compute the next-to-leading-order IR-resummed matter power spectrum, ala Ivanovic et al.

Parameters

Cx	Input: pointer to cosmology structure
k	Input: wavenumber in unit of 1/Mpc.
z	Input: redshift
SPLIT	Input: switch to set the method of wiggle-nowiggle split

Returns: value of NL IR-ressumed power spectrum

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◆ pm_nowiggle()

double pm_nowiggle	(	struct Cosmology *	Cx,
		double	k,
		double	z,
		double	k0,
		int	cleanup,
		long	SPLIT
	)

Compute the no-wiggle componenet of the matter power spectrum.

Parameters

Cx	Input: pointer to cosmology structure
k	Input: wavenumber in unit of h/Mpc.
z	Input: redshift
k0	Input: first element of the k-array, used in normalization of EH no-wiggle spectrum
cleanup	Input: switch to set whether to free the memory allocated to no-wiggle interpolators
SPLIT	Input: switch to set the method of wiggle-nowiggle split

Returns: value of no-wiggle power spectrum

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◆ pm_nowiggle_bspline()

double pm_nowiggle_bspline	(	struct Cosmology *	Cx,
		double	k,
		double	z,
		int	cleanup
	)

Compute the no-wiggle componenet of the matter power spectrum, reading in and interpolating the output of apython code which computed the broadband by fitting families of Bsplines (see Vlah et al 2015)

Parameters

Cx	Input: pointer to cosmology structure
k	Input: wavenumber in unit of h/Mpc.
z	Input: redshift
cleanup	Input: switch to set whether to free the memory allocated to no-wiggle interpolators

Returns: value of no-wiggle power spectrum

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◆ pm_nowiggle_dst()

double pm_nowiggle_dst	(	struct Cosmology *	Cx,
		double	k,
		double	z,
		int	cleanup
	)

Compute the no-wiggle componenet of the matter power spectrum, reading in and interpolating the output of apython code which computed the broadband by discrete sin-transform, See Hamann et al 2010.

Parameters

Cx	Input: pointer to cosmology structure
k	Input: wavenumber in unit of h/Mpc.
z	Input: redshift
cleanup	Input: switch to set whether to free the memory allocated to no-wiggle interpolators

Returns: value of no-wiggle power spectrum

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◆ pm_nowiggle_gfilter()

double pm_nowiggle_gfilter	(	struct Cosmology *	Cx,
		double	k,
		double	z,
		int	cleanup
	)

Compute the no-wiggle componenet of the matter power spectrum, using Gaussian filter (see Vlah et al 2015)

Parameters

Cx	Input: pointer to cosmology structure
k	Input: wavenumber in unit of h/Mpc.
z	Input: redshift
cleanup	Input: switch to set whether to free the memory allocated to no-wiggle interpolators

Returns: value of no-wiggle power spectrum

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Functions

Detailed Description

Function Documentation

◆ IR_Sigma2()

◆ IR_Sigma2_integrand()

◆ pm_IR_LO()

◆ pm_IR_NLO()

◆ pm_nowiggle()

◆ pm_nowiggle_bspline()

◆ pm_nowiggle_dst()

◆ pm_nowiggle_gfilter()