Documented real-space, direct numerical integration computation of 1loop contributions of the halo/galaxy power spectrum See arXiv:2010.14523 for explicit expressions. More...

#include "header.h"

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Functions
double	PS_hh_G (struct Cosmology *Cx, double k, double z, double M, long mode_pt, long IR_switch, long SPLIT, long mode_mf)
	Compute the contributions up to 1loop to halo power spectrum for Gaussian initial conditions. More...

double	PS_hh_PNG (struct Cosmology *Cx, double k, double z, double M, long mode_pt, long IR_switch, long SPLIT, long mode_mf)
	Compute contributions up to 1loop to halo power spectrum arising from non-Gaussian initial conditions of local shape. More...

static int	G_loop_integrands (const int ndim, const cubareal x[], const int ncomp, cubareal ff[], void *p)
	The integrand function passed passed to Cuhre integration routine to compute Gaussian 1loop terms. More...

void	Compute_G_loops (struct Cosmology Cx, double k, double z, long IR_switch, long hm_switch, long SPLIT, double result)
	Compute the loop contributions dure to nonlinear evolution of matter fluctuations and nonlinear halo bias, present for Gaussian initial conditions. More...

static int	PNG_loop_integrands (const int ndim, const cubareal x[], const int ncomp, cubareal ff[], void *p)
	The integrand function passed passed to Cuhre integration routine to compute PNG 1loop terms. More...

void	Compute_PNG_loops (struct Cosmology Cx, double k, double z, long IR_switch, long SPLIT, double result)
	Compute the loop contributions dure to nonlinear evolution of matter fluctuations and nonlinear halo bias, rising from non-Gaussian initial conditions of local shape. More...

double	F2_s (double k1, double k2, double mu)

double	S2_s (double k1, double k2, double mu)

double	F3_s (double k, double q, double mu)

double	S2 (double mu)

double	F2 (double k1, double k2, double mu)

Detailed Description

Documented real-space, direct numerical integration computation of 1loop contributions of the halo/galaxy power spectrum See arXiv:2010.14523 for explicit expressions.

Azadeh Moradinezhad Dizgah, November 4th 2021

This module computes the 1loop halo/galaxy power sprtcurm in real-space via direct numerical integration. IR-resummation and EFT counter terms are included. In addition to loops due to gravitational loops, terms arising only in the presence of local PNG are also included. The explicit expressions of all the loops are given in 2010.14523.

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

PS_hh_G()
PS_hh_PNG()
Compute_Gloops()
Compute_PNGloops()
F2_s()
F3_s()
S2_s()
F2()
S2()

Function Documentation

◆ Compute_G_loops()

void Compute_G_loops	(	struct Cosmology *	Cx,
		double	k,
		double	z,
		long	IR_switch,
		long	hm_switch,
		long	SPLIT,
		double *	result
	)

Compute the loop contributions dure to nonlinear evolution of matter fluctuations and nonlinear halo bias, present for Gaussian initial conditions.

Parameters

Cx	Input: pointer to cosmology structure
k	Input: wavenumber
z	Input: redshift of interest
IR_switch	Input: switch to decide whether to perform IR resummation or no
hm_switch	Input: switch to decide whether to compute the 1loop terms due to matter or bias
SPLIT	Input: switch to set the method to perform the wiggle-nowiggle split of matter power spectrum
result	Output: an output array containing the results of the 1loop terms, has 2 elements for hm_switch=MATTER, and 6 elements for hm_switch=HALO

Returns: void

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◆ Compute_PNG_loops()

void Compute_PNG_loops	(	struct Cosmology *	Cx,
		double	k,
		double	z,
		long	IR_switch,
		long	SPLIT,
		double *	result
	)

Compute the loop contributions dure to nonlinear evolution of matter fluctuations and nonlinear halo bias, rising from non-Gaussian initial conditions of local shape.

Parameters

Cx	Input: pointer to cosmology structure
k	Input: wavenumber
z	Input: redshift of interest
IR_switch	Input: switch to decide whether to perform IR resummation or no
SPLIT	Input: switch to set the method to perform the wiggle-nowiggle split of matter power spectrum
result	Output: an output array containing the results of the 1loop terms, has 8 elements for hm_switch=HALO

Returns: void

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◆ F2()

double F2	(	double	k1,
		double	k2,
		double	mu
	)

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◆ F2_s()

double F2_s	(	double	k1,
		double	k2,
		double	mu
	)

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◆ F3_s()

double F3_s	(	double	k,
		double	q,
		double	mu
	)

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◆ G_loop_integrands()

static int G_loop_integrands	(	const int *	ndim,
		const cubareal	x[],
		const int *	ncomp,
		cubareal	ff[],
		void *	p
	)

static

The integrand function passed passed to Cuhre integration routine to compute Gaussian 1loop terms.

Parameters

ndim	Input: Dimensionality of the domain of integration
x	Input: An array of integration variables
ncomp	Input: Dimensionality of the integrand function
ff	Input: Array of values of the integrand of dimension fdim
p	Input: integration parmaeters return the error status

Model used in 1907.06666, the integrals are given in the appendix, Eq. A1, note that my S2_s = sigma^2(q,k-1) and F2_s = F2(q,k-q) in their notation. Factor of 2. * (logqmax - logqmin) is due to change of variable from 0 to logarithmic k, and a factor of 2*PI is due to integration over azimuthal angle. Note that to compare the theoretical predictions against Emiliano's measurement, since he is using a different notation for Fourier transform, I need to devide each 0 power spectrum by a factor of 1/pow(2.*M_PI,3.), which I do in my pk_lin() function. If using another notation for Fourier transform (the one that I usually use, which has a factor of 1/pow(2*M_PI,3) in the definition), you need to multiply these integrands by a factor of 1/pow(2*M_PI,3).

The integrands below correspond to the follwing bias combinaions:

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◆ PNG_loop_integrands()

static int PNG_loop_integrands	(	const int *	ndim,
		const cubareal	x[],
		const int *	ncomp,
		cubareal	ff[],
		void *	p
	)

static

The integrand function passed passed to Cuhre integration routine to compute PNG 1loop terms.

Parameters

ndim	Input: Dimensionality of the domain of integration
x	Input: An array of integration variables
ncomp	Input: Dimensionality of the integrand function
ff	Input: Array of values of the integrand of dimension fdim
p	Input: integration parmaeters return the error status

Factor of 2. * (logqmax - logqmin) is due to change of variable from 0 to logarithmic k, and a factor of 2*PI is due to integration over azimuthal angle. Note that to compare the theoretical predictions against Emiliano's measurement, since he is using a different notation for Fourier transform, I need to devide each 0 power spectrum by a factor of 1/pow(2.*M_PI,3.), which I do in my pk_lin() function. If using another notation for Fourier transform (the one that I usually use, which has a factor of 1/pow(2*M_PI,3) in the definition), you need to multiply these integrands by a factor of 1/pow(2*M_PI,3).

The integrands below correspond to the follwing bias combinaions:

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◆ PS_hh_G()

double PS_hh_G	(	struct Cosmology *	Cx,
		double	k,
		double	z,
		double	M,
		long	mode_pt,
		long	IR_switch,
		long	SPLIT,
		long	mode_mf
	)

Compute the contributions up to 1loop to halo power spectrum for Gaussian initial conditions.

Parameters

Cx	Input: pointer to cosmology structure
k	Input: wavenumber
z	Input: redshift of interest
M	Input: halo mass, used in computing the halo bias
mode_pt	Input: switch to decide whether to compute tree-level halo power spectrum or the 1loop
IR_switch	Input: switch to decide whether to perform IR resummation or no
SPLIT	Input: switch to set the method to perform the wiggle-nowiggle split of matter power spectrum
mode_mf	Input: switch to set the theoretical model of the mass function used to compute the halo biases

Returns: G loop contributions of P_h

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◆ PS_hh_PNG()

double PS_hh_PNG	(	struct Cosmology *	Cx,
		double	k,
		double	z,
		double	M,
		long	mode_pt,
		long	IR_switch,
		long	SPLIT,
		long	mode_mf
	)

Compute contributions up to 1loop to halo power spectrum arising from non-Gaussian initial conditions of local shape.

Parameters

Cx	Input: pointer to cosmology structure
k	Input: wavenumber
z	Input: redshift of interest
M	Input: halo mass, used in computing the halo bias
mode_pt	Input: switch to decide whether to compute tree-level halo power spectrum or the 1loop
IR_switch	Input: switch to decide whether to perform IR resummation or no
SPLIT	Input: switch to set the method to perform the wiggle-nowiggle split of matter power spectrum
mode_mf	Input: switch to set the theoretical model of the mass function used to compute the halo biases

Returns: PNG loop contributions of P_h

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◆ S2()

double S2 ( double mu )

◆ S2_s()

double S2_s	(	double	k1,
		double	k2,
		double	mu
	)

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Functions

Detailed Description

Function Documentation

◆ Compute_G_loops()

◆ Compute_PNG_loops()

◆ F2()

◆ F2_s()

◆ F3_s()

◆ G_loop_integrands()

◆ PNG_loop_integrands()

◆ PS_hh_G()

◆ PS_hh_PNG()

◆ S2()

◆ S2_s()