sp_validation.cosmology

COSMOLOGY.

Name:

cosmology.py

Description:

This file contains methods for science validation of a weak-lensing shape catalogue. Depends on a cosmological model.

Author:

Axel Guinot, Martin Kilbinger, Cail Daley

_ccl_to_camb(cosmo)[source]

Convert CCL cosmology object to CAMB parameter format.

Parameters:

cosmo (ccl.Cosmology) – CCL cosmology object

Returns:

CAMB parameters dictionary with As properly set

Return type:

dict

_camb_to_ccl(camb_params)[source]

Convert CAMB parameter format to CCL parameter dictionary.

Parameters:

camb_params (dict) – CAMB parameters dictionary with required keys: H0, ombh2, omch2, ns, and either As or sigma8

Returns:

CCL parameters dictionary

Return type:

dict

_cosmocov_to_ccl(cosmocov_params)[source]

Convert CosmoCov parameter format to CCL parameter dictionary.

Parameters:

cosmocov_params (dict) – CosmoCov parameters dictionary with required keys: Omega_m, omb, h0, sigma_8, n_spec

Returns:

CCL parameters dictionary

Return type:

dict

get_cosmo(Omega_b=None, Omega_m=None, h=None, sig8=None, ns=None, w0=None, wa=None, transfer_function='boltzmann_camb', matter_power_spectrum='halofit', cosmocov_params=None, camb_params=None)[source]

Get CCL cosmology object with user-specified parameters.

Defaults to astropy Planck18 cosmology (Table 2: TT,TE,EE+lowE+lensing+BAO). Can also use CosmoCov or CAMB parameter formats.

Parameters:

  • Omega_m (float, default=None) – Matter density parameter (defaults to Planck18: 0.30966)

  • Omega_b (float, default=None) – Baryon density parameter (defaults to Planck18: 0.04897)

  • h (float, default=None) – Reduced Hubble constant (defaults to Planck18: 0.6766)

  • sig8 (float, default=None) – RMS matter fluctuation amplitude at 8 Mpc/h (defaults to Planck18: 0.8102)

  • ns (float, default=None) – Scalar spectral index (defaults to Planck18: 0.9665)

  • w0 (float, default=None) – Dark energy equation of state parameter (defaults to -1.0)

  • wa (float, default=None) – Dark energy equation of state evolution parameter (defaults to 0.0)

  • transfer_function (str, default='boltzmann_camb') – Transfer function to use

  • matter_power_spectrum (str, default='halofit') – Matter power spectrum to use

  • cosmocov_params (dict, optional) – Parameters in CosmoCov format (Omega_m, omb, h0, sigma_8, n_spec) If provided, entries override above parameters. Mutually exclusive with camb_params.

  • camb_params (dict, optional) – Parameters in CAMB format (H0, ombh2, omch2, ns, sigma8) If provided, entries override above parameters. Mutually exclusive with cosmocov_params.

Returns:

pyccl cosmology object

Return type:

Cosmology

get_theo_c_ell(ell, z, nz, backend='ccl', cosmo=None, Omega_b=None, Omega_m=None, h=None, sig8=None, ns=None, w0=None, wa=None)[source]

Calculate theoretical angular power spectrum C_ell for weak lensing.

Parameters:

  • ell (array) – Multipole moments (e.g., np.arange(2, 2000))

  • z (array) – Redshifts for n(z) distribution

  • nz (array) – n(z) redshift distribution

  • backend (str, default="ccl") – Backend to use: “ccl” or “camb”

  • cosmo (ccl.Cosmology, optional) – CCL cosmology object. If None, will create using individual parameters.

  • Omega_b (float, optional) – Baryon density parameter (defaults to Planck 2018)

  • Omega_m (float, optional) – Matter density parameter (defaults to Planck 2018)

  • h (float, optional) – Reduced Hubble constant (defaults to Planck 2018)

  • sig8 (float, optional) – RMS matter fluctuation amplitude at 8 Mpc/h (defaults to Planck 2018)

  • ns (float, optional) – Scalar spectral index (defaults to Planck 2018)

  • w0 (float, optional) – Dark energy equation of state parameter (defaults to -1.0)

  • wa (float, optional) – Dark energy equation of state evolution parameter (defaults to 0.0)

Returns:

cl – Angular power spectrum

Return type:

array

c_ell_to_xi(cosmo, theta, ell, cl)[source]

Convert angular power spectrum to correlation functions using CCL.

Parameters:

  • cosmo (ccl.Cosmology) – CCL cosmology object (used for correlation function calculation)

  • theta (array) – Angular separations in arcminutes

  • ell (array) – Multipole moments

  • cl (array) – Angular power spectrum

Returns:

xip, xim – xi+ and xi- correlation functions

Return type:

arrays

get_theo_xi(theta, z, nz, Omega_m=None, h=None, Omega_b=None, sig8=None, ns=None, ell_min=10, ell_max=20000, n_ell=500, backend='ccl', cosmo=None, **cosmo_kwargs)[source]

Calculate theoretical xi+/xi- using individual parameters.

Parameters:

  • theta (array) – Angular separations in arcminutes

  • z (array) – Redshift array

  • nz (array) – n(z) redshift distribution

  • Omega_m (float, default=None) – Matter density parameter (defaults to Planck 2018)

  • h (float, default=None) – Reduced Hubble constant (defaults to Planck 2018)

  • Omega_b (float, default=None) – Baryon density parameter (defaults to Planck 2018)

  • sig8 (float, default=None) – RMS matter fluctuation amplitude at 8 Mpc/h (defaults to Planck 2018)

  • ns (float, default=None) – Scalar spectral index (defaults to Planck 2018)

  • ell_min (int, default=0) – Minimum ell for power spectrum calculation

  • ell_max (int, default=20000) – Maximum ell for power spectrum calculation

  • n_ell (int, default=500) – Number of ell bins

  • backend (str, default="ccl") – Backend to use: “ccl” or “camb”

  • **cosmo_kwargs – Additional arguments passed to backend

Returns:

xip, xim – Theoretical xi+ and xi- correlation functions

Return type:

arrays

stack_mm3(ra, dec, e1, e2, w, cluster_ra, cluster_dec, cluster_z, radius=100, n_match=100000, tree=None)[source]

Add docstring.

…

gamma_T_tc(ra_pos, dec_pos, ra_cat, dec_cat, e1_cat, e2_cat, w_cat=None)[source]

Gamma T tc.

Compute cross-correlation between positions (forground) and lensing (background) catalogue. Also called galaxy-galaxy lensing or population lensing.

Parameters:

  • ra_pos (array of float) – RA coordinates of foreground catalogue

  • dec_pos (array of float) – DEC coordinates of foreground catalogue

  • ra_cat (array of float) – RA coordinates of background catalogue

  • dec_cat (array of float) – DEC coordinates of background catalogue

  • e1_cat (array of float) – ellipticity component 1 of background catalogue

  • e2_cat (array of float) – ellipticity component 2 of background catalogue

  • w_cat (array of float, optional, default=None) – weight of background catalogue

Returns:

  • meanr (array of float) – spatial bin centres

  • meanlogr (array of float) – log of spatial bin centres

  • xi (array of float) – tangential shear (E-mode)

  • xi_im (array of float) – cross-component shear (B- or parity mode)

  • rms (array of float) – R.M.S of both xi and xi_im

xi_gal_gal_tc(ra_gal, dec_gal, e1_gal, e2_gal, w_gal, ra_star, dec_star, e1_star, e2_star, w_star=None, theta_min_amin=2, theta_max_amin=200, n_theta=20)[source]

Add docstring.

…

get_clusters(cluster_cat_name, vos_dir, output_dir, field_name, verbose=False)[source]

Get Clusters.

Return cluster information from file on VOspace

Parameters:

  • cluster_cat_name (string) – cluster catalogue file name

  • vos_dir (string) – directory on VOspace

  • field_name (string) – survey footprint name

  • verbose (bool, optional, default=False) – verbose output if True

Returns:

cluster information (ra, dec, z, SZ-mass)

Return type:

tuple