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Clone wikicosmosis / default_modules / wl_spectra_1.0
wl_spectra module
Compute various weak lensing C_ell from P(k,z) with the Limber integral
Name: wl_spectra
File: cosmosis-standard-library/shear/spectra/interface.so
Version: 1.0
Author(s):
- CosmoSIS team
- Matt Becker
URL:
Cite:
Rules:
Assumptions:
- The Limber integral is valid on the scales in question
Explanation
DEPRECATED: You should use the module cosmosis-standard-library/structure/projection/project_2d.py instead.
The Limber approximation integrates a 3D power spectrum over the radial
direction to get a 2D angular power spectrum. It is an approximation
which is only valid on smaller scales.
C_\ell = A \int_0^{\chi_1} W_1(\chi) W_2(\chi) P(k=l/\chi, z(\chi)) / chi^2 d\chi
The full integral must integrate over k(\ell) also.
For weak lensing, the power spectrum is the matter power spectrum and the two
kernel functions W depend on the redshift bins being used and the geometry.
Parts of this code and the underlying implementation of limber are based on cosmocalc:
https://bitbucket.org/beckermr/cosmocalc-public
##Parameters
These parameters can be set in the module's section in the ini parameter file.
If no default is specified then the parameter is required.
| Parameter | Description |
|---|---|
| n_ell | Integer; number of log-spaced ell values to compute |
| ell_min | Real; minimum ell value to compute |
| ell_max | Real; maximum ell value to compute |
| shear_shear | Logical; compute shear auto-spectra? (Default: True) |
| intrinsic_alignments | Logical; compute intrinsic alignments spectra? (Default: False) |
| matter_spectra | Logical; compute matter power spectra? (Default: False) |
| ggl_spectra | Logical; compute galaxy-galaxy lensing spectra? (Default: False) |
| gal_IA_cross_spectra | Logical; compute cross-power between galaxy positions and alignments? (Default: False) - Not implemented |
| mag_gal_cross_spectra | Logical; compute lensing magnification cross-spectra? (Default: False) |
| mag_mag | Logical; compute lensing magnification auto-spectra? (Default: False) |
##Inputs
These parameters and data are inputs to the module, either supplied as parameters by the sampler or computed by some previous module. They are loaded from the data block.
| Section | Parameter | Description |
|---|---|---|
| cosmological_parameters | omega_m | Real; density fraction of all matter; used in the prefactor |
| h0 | Real; hubble factor H0 / 100 km/s/Mpc. | |
| distances | z | real vector; redshift values of distance samples |
| d_m | real vector; comoving distnace to redshift values in units of Mpc (no factor h) | |
| matter_power_nl | z | real vector; redshift values of P(k,z) samples |
| k_h | real vector; k values of P(k,z) samples in units of Mpc/h | |
| P_k | real 2d array; non-linear matter power spectrum at samples in (Mpc/h)^{-3} | |
| wl_number_density | nbin | integer; number of redshift bins |
| z | real vector; redshift values of n(z) samples | |
| bin_ | real_vector; bin n(z) values. Need not be normalized. bin_1, bin_2, bin_3, .... | |
| matter_power_gal | z | real vector; redshift values of P(k,z) samples |
| k_h | real vector; k values of P(k,z) samples in units of Mpc/h | |
| P_k | real 2d array; non-linear galaxy power spectrum at samples in (Mpc/h)^{-3} | |
| matter_power_gal_mass | z | real vector; redshift values of P(k,z) samples |
| k_h | real vector; k values of P_{gm}(k,z) samples in units of Mpc/h | |
| P_k | real 2d array; non-linear galaxy-mass cross-power spectrum at samples in (Mpc/h)^{-3} |
##Outputs
These parameters and data are computed as outputs from the module
| Section | Parameter | Description |
|---|---|---|
| shear_cl | ell | Sample ell values for output C_ell |
| nbin | Number of redshift bins used | |
| bin_i_j | C_ell (no l(l+1) factor) for (auto-correlation) bin i and j. Only stores j<=i. | |
| shear_cl_ii | ell | Sample ell values for output C_ell |
| nbin | Number of redshift bins used | |
| bin_i_j | C_ell (no l(l+1) factor) for (auto-correlation) bin i and j. Only stores j<=i. | |
| shear_cl_gi | ell | Sample ell values for output C_ell |
| nbin | Number of redshift bins used | |
| bin_i_j | C_ell (no l(l+1) factor) for (auto-correlation) bin i and j. Only stores j<=i. | |
| matter_cl | ell | Sample ell values for output C_ell |
| nbin | Number of redshift bins used | |
| bin_i_j | C_ell (no l(l+1) factor) for (auto-correlation) bin i and j. Only stores j<=i. | |
| ggl_cl | ell | Sample ell values for output C_ell |
| nbin | Number of redshift bins used | |
| bin_i_j | C_ell (no l(l+1) factor) for (auto-correlation) bin i and j. Only stores j<=i. | |
| gal_IA_cross_cl | ell | Sample ell values for output C_ell |
| nbin | Number of redshift bins used | |
| bin_i_j | C_ell (no l(l+1) factor) for (auto-correlation) bin i and j. Only stores j<=i. | |
| magnification_galaxy_cl | ell | Sample ell values for output C_ell |
| nbin | Number of redshift bins used | |
| bin_i_j | C_ell (no l(l+1) factor) for (auto-correlation) bin i and j. Only stores j<=i. | |
| magnification_magnification_cl | ell | Sample ell values for output C_ell |
| nbin | Number of redshift bins used | |
| bin_i_j | C_ell (no l(l+1) factor) for (auto-correlation) bin i and j. Only stores j<=i. | |
| magnification_intrinsic_cl | ell | Sample ell values for output C_ell |
| nbin | Number of redshift bins used | |
| bin_i_j | C_ell (no l(l+1) factor) for (auto-correlation) bin i and j. Only stores j<=i. | |
| magnification_shear_cl | ell | Sample ell values for output C_ell |
| nbin | Number of redshift bins used | |
| bin_i_j | C_ell (no l(l+1) factor) for (auto-correlation) bin i and j. Only stores j<=i. |
Updated