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create_datavector_pessim.ini
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;***********************************
;cosmosis script for 6x2pt Roman_SO
;create datavector with gaussian covariance calculated with cosmosis
;and external cosmolike ng covariance
;***********************************
%include modules/RomanxCMB/params_pessim.ini
[runtime]
sampler = test
root = ${COSMOSIS_SRC_DIR}
[pipeline]
fast_slow = F
; first_fast_module = add_intrinsic
; first_fast_module was bin_bias
values = %(ROMANxCMB_SRC_DIR)s/values_pessim.ini
priors = %(ROMANxCMB_SRC_DIR)s/priors_pessim.ini
modules = consistency check_w0wa growth_ehu ehu camb_background sigma8_rescale mead high_z_power extrapolate calculate_nz_lens calculate_nz_source unbiased_galaxies IA_keb pk_to_cl bin_bias add_intrinsic shear_m_bias save_2pt
; consistency: Computes the full set of cosmological parameter, e.g. h->H_0, Omega_m->Omega_m h^2
; check_wwa: Apply a cutoff on the sum of w0 and wa
; -- Compute linear matter power spectra
; > camb: Computes the CMB and linear matter power spectra
; -- or
; > growth_ehu Computes the growth rate
; > ehu Computes the linear matter power spectra from the growth
; > camb_background Use CAMB to calculate thermal history to get comoving distance to cmb
; sigma8_rescale: Rescales matter power spectrum to fit the desired sigma_8_input
; mead Computes the nonlinear matter spectrum and baryonic effects
; -- or
; halofit: Computes the nonlinear matter spectrum
; - to compare linear matter power spectrum results replace with rename_matter_power
; > growth: Computes the growth rate (only when not called above)
; high_z_power: Extrapolates the matter power spectra to high z using growth function
; extrapolate: Extrapolates the matter power spectra to high k
; -to load the cosmolike n(z) per bin use: load_nz_lens load_nz_source lens_photoz_bias source_photoz_bias
; calculate_nz_source:Loads the source number density from file and calculates bins
; calculate_nz_source:Loads the lens number density from file and calculates bins
; unbiased_galaxies: Computes the galaxy power spectrum (pretending for the moment that b is 1
; IA_keb Computes the eNLA intrinsic alignment model
; > IA: OLD: Computes the NLA intrinsic alignment model
; > ia_z_field: OLD: Applies an additional redshift dependence to the NLA model
; pk_to_cl: Computes C_ell values using the Limber integral
; bin_bias: Applies per-bin bias values to the galaxy-galaxy lensing and galaxy spectra
; add_intrinsic: Adds the intrinsic alignment contribution to the galaxy lensing
; shear_m_bias: Applies a shear calibration bias
; -- calculate likelihood
; 2pt_like: Computes the 2pt function likelihood, note: add 2pt to likelihoods
; -- create and save 2pt datavector
; save_2pt: Saves the theory power spectra in a data format. Calculates or loads the covariance matrix
; calc_scale_cuts calculates the scale cuts, only needed when changing the fiducial cosmological parameters
likelihoods =
;extra_output = cosmological_parameters/sigma_8 ; Derived parameter to save
quiet=F
timing=F
debug=T
[DEFAULT]
ROMANxCMB_SRC_DIR = modules/RomanxCMB
2PT_FILE = ${COSMOSIS_SRC_DIR}/%(ROMANxCMB_SRC_DIR)s/6x2pt_Roman_SO_pessim.fits
2PT_DATA_SETS = shear_cl galaxy_shear_cl shear_cmbkappa_cl galaxy_cl galaxy_cmbkappa_cl cmbkappa_cl
; when the order of the datasets is changed the gaussian covariance calculation breaks!
RUN_NAME = 6x2pt_Roman_SO_pessim
; planck_like_path=/path/to/planck/data/plc_2.0
[save_2pt]
file = %(ROMANxCMB_SRC_DIR)s/2pt_modified/save_2pt.py
ell_min = 30
ell_max = 3000
n_ell = 20
logspaced = T
real_space = F
shear_nz_name = nz_source
position_nz_name = nz_lens
filename = %(2PT_FILE)s
overwrite = T
; Cosmolike uses exact logspaced bins, without rounding the ranges to integer ell (which is the default assumption in cosmosis)
force_ell_limits_to_be_integer = T
;load which bin combinations to use
cosmolike_metadata_file = ${COSMOSIS_SRC_DIR}/%(ROMANxCMB_SRC_DIR)s/cosmolike_data/cov_indices_apr9.txt
spectrum_sections = %(2PT_DATA_SETS)s
;load external ng covariance
add_ng_cosmolike_covariance = ${COSMOSIS_SRC_DIR}/%(ROMANxCMB_SRC_DIR)s/cosmolike_data/covariances_WFIRST_SO_gold_ng_zgauss_pessim_ng.txt
cosmolike_overall_fsky = 0.0484813681 ; 2000 sq deg
new_fsky_cmb_lensing = 0.4
;params to calculate covariance
make_covariance = T
cov_calc_multiply_range_instead_of_sum = F
fsky = 0.0484813681 ; 2000 sq deg
fsky_cmblensing = 0.4 ; 0.4;fsky for cmb alone is larger than for overlap
cmblensing_noisecurve = ${COSMOSIS_SRC_DIR}/%(ROMANxCMB_SRC_DIR)s/SO_noise_curves/lensing_v3_0_0/Apr17_mv_nlkk_deproj0_SENS1_fsky_16000_iterOn.csv
number_density_lss_arcmin2 = 6.6 6.6 6.6 6.6 6.6 6.6 6.6 6.6 6.6 6.6 ; galaxies per arcminute squared
number_density_shear_arcmin2 = 5.1 5.1 5.1 5.1 5.1 5.1 5.1 5.1 5.1 5.1 ; "
sigma_e_total = 0.37 0.37 0.37 0.37 0.37 0.37 0.37 0.37 0.37 0.37 ; note this is multiplied with sqrt 2 since it is both components!
;
[pk_to_cl]
file = %(ROMANxCMB_SRC_DIR)s/projection/project_2d.py
ell_min = 30.
ell_max = 3000.
n_ell = 200
sample_mids = F ;normal: sample in log space including min and max. middle: sample in log spce n_ell+1 times then take mids of the ranges.
;note that there will be an out of bounds error if the midpoints in the datavector are not exactly the same
position-shear = lens-source ; lens and source kind of look switched to me? -Lukas
shear-shear = source-source
position-position = lens-lens
intrinsic-intrinsic = source-source
shear-intrinsic = source-source
position-intrinsic = lens-source
shear-Cmbkappa = source-cmb ;cmb is just a placeholder, kappa kernel is hardcoded
Cmbkappa-Cmbkappa = cmb-cmb
intrinsic-Cmbkappa = source-cmb
position-Cmbkappa = lens-cmb
verbose = F
get_kernel_peaks=F
set_offdiag_for_galaxycl_to_one = F ; DO NOT USE WHEN CALCULATING COVARIANCE ;saves about 0.15s per pipeline on a single core. We are not using the off diagonal terms for galaxy_cl