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module.yaml
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name: hi_class
version: 1.1
purpose: "Boltzmann and background integrator for BG, CMB, matter power, and more"
url: http://hiclass-code.net
interface: hi_class_interface.py
attribution: [Miguel Zumalacarregui, Emilio Bellini, Ignacy Sawicki, Julien Lesgourgues, Thomas Tram, Benjamin Audren, Simon Prunet, Jesus Torrado, etc]
rules:
- "You can use hi_class freely, provided that in your publications, you cite at least the paper hi_class: Horndeski in the Cosmic Linear Anisotropy Solving System and the paper CLASS II: Approximation schemes. Feel free to cite more CLASS papers!"
cite:
- "JCAP 1708 (2017) 019"
- "http://arxiv.org/abs/1104.2932"
- "JCAP 07 (2011) 034"
- "http://arxiv.org/abs/1104.2934"
- "JCAP 09 (2011) 032"
assumptions:
- Dark Energy and Modified Gravity within the Horndeski framework
- Various choices for approximations and implementations of the Boltzmann and related equations
explanation:
hi_class is one of the cosmology codes for evolving perturbations
in the primordial universe into CMB and other power spectra, as
well as various other quantities. It is an extension of CLASS to consider
Dark Energy and Modified Gravity scenarios a la Horndeski.
See http://hiclass-code.net for a fuller description and the github repository
https://github.com/miguelzuma/hi_class_public for the latest public code.
You should also check out the MontePython sampler code, which uses hi_class
to do similar inference to CosmoSIS.
This version of hi_class has been modified very slightly to be able to output at
more redshifts and to use the cosmosis build system.
params:
lmax: "Integer, max angular frequency ell to use for cmb calculation (default 2000)"
kmax: "Integer, the max wavenumber k to use for P(k,z) calculation (default 50.0)"
zmax: "Max value to save P(k,z) and distances (default 4.0)"
inputs:
cosmological_parameters:
# If these parameters are not those you would like to sample over (say omega_m or
# omegaa_ch2 are preferable), please use the consistency module.
ombh2: "real, physbaryon density fraction today, Omega_b * h**2"
omch2: "real, physical cdm density fraction today, Omega_c * h**2"
h0: "real, hubble parameter H0 / 100 km/s/Mpc"
tau: "real, optical depth to last-scattering"
n_s: "real, scalar spectral index"
A_s: "real, scalar spectrum primordial amplitude"
massless_nu: "real, effective number of massless neutrinos (default 3.046)"
t_cmb: "real, the CMB temperature today in Kelvin (default=2.726)"
outputs:
cosmological_parameters:
sigma_8: "real, amplitude of linear matter power at 8/h Mpc at z=0. Only calculated if mode=all"
distances:
nz: "integer, number of z samples"
z: "1D real array, redshifts of samples"
d_a: "1D real array, angular diameter distance in Mpc"
d_m: "1D real array, co-moving distance in Mpc"
d_l: "1D real array, luminosity distance in Mpc"
age: "real, age of universe in GYr"
rs_zdrag: "real, sound horizon size at zdrag. Only if mode!=background"
matter_power_lin:
z: "1D real array, redshifts of samples. Only if mode=all"
k_h: "1D real array, k wavenumbers of samples in Mpc/h. Only if mode=all"
p_k: "2D real array, matter power spectrum at samples in (Mpc/h)^-3. Only if mode=all"
cmb_cl:
ell: "1D integer array, angular frequencies. Only if mode=cmb or all"
tt: "1D real array, ell * (ell+1) C_ell^TT / 2 pi in mu K^2. Only if mode=cmb or all"
ee: "1D real array, ell * (ell+1) C_ell^EE / 2 pi in mu K^2. Only if mode=cmb or all"
bb: "1D real array, ell * (ell+1) C_ell^BB / 2 pi in mu K^2. Only if mode=cmb or all"
te: "1D real array, ell * (ell+1) C_ell^TE / 2 pi in mu K^2. Only if mode=cmb or all"