Cosmological theory codes and likelihoods¶
Models in Cosmology are usually split in two: \(\mathcal{M}=\mathcal{T}+\mathcal{E}\), where
 \(\mathcal{T}\), the theoretical model, is used to compute observable quantities \(\mathcal{O}\)
 \(\mathcal{E}\), the experimental model, accounts for instrumental errors, foregrounds… when comparing the theoretical observable with some data \(\mathcal{D}\).
In practice the theoretical model is encapsulated in one or more theory codes (CLASS, CAMB…) and the experimental model in a likelihood, which gives the probability of the data being a realization of the given observable in the context of the experiment:
Each iteration of a sampler reproduces the model using the following steps:
 A new set of theory+experimental parameters is proposed by the sampler.
 The theory parameters are passed to the theory codes, which compute one or more observables.
 The experimental parameters are passed to each of the likelihoods, which in turn ask the theory code for the current value of the observables they need, and use all of that to compute a logprobability of the data.
cobaya wraps the most popular cosmological codes under a single interface, documented below. The codes themselves are documented in the next sections, followed by the internal likelihoods included in cobaya.
Cosmological theory code¶

class
theories.cosmo.
BoltzmannBase
(info: Mapping[str, Any] = mappingproxy({}), name: Optional[str] = None, timing: Optional[bool] = None, packages_path: Optional[str] = None, initialize=True, standalone=True)¶ 
initialize
()¶ Initializes the class (called from __init__, before other initializations).

initialize_with_params
()¶ Additional initialization after requirements called and input_params and output_params have been assigned (but provider and assigned requirements not yet set).

get_allow_agnostic
()¶ Whether it is allowed to pass all unassigned input parameters to this component (True) or whether parameters must be explicitly specified (False).
Returns: True or False

get_param
(p)¶ Interface function for likelihoods and other theory components to get derived parameters.

must_provide
(**requirements)¶ Specifies the quantities that this Boltzmann code is requested to compute.
Typical requisites in Cosmology (as keywords, case insensitive):
Cl={...}
: CMB lensed power spectra, as a dictionary{[spectrum]: l_max}
, where the possible spectra are combinations of"t"
,"e"
,"b"
and"p"
(lensing potential). Get withget_Cl()
.unlensed_Cl={...}
: CMB unlensed power spectra, as a dictionary{[spectrum]: l_max}
, where the possible spectra are combinations of"t"
,"e"
,"b"
. Get withget_unlensed_Cl()
. [BETA: CAMB only; notation may change!]
source_Cl={...}
: \(C_\ell\) of given sources with given windows, e.g.:source_name: {"function": "spline""gaussian", [source_args]
; for now,[source_args]
follows the notation of CAMBSources. If can also take"lmax": [int]
,"limber": True
if Limber approximation desired, and"non_linear": True
if nonlinear contributions requested. Get withget_source_Cl()
. Pk_interpolator={...}
: Matter power spectrum interpolator in \((z, k)\). Takes"z": [list_of_evaluated_redshifts]
,"k_max": [k_max]
,"extrap_kmax": [max_k_max_extrapolated]
,"nonlinear": [TrueFalse]
,"vars_pairs": [["delta_tot", "delta_tot"], ["Weyl", "Weyl"], [...]]}
. Nonlinear contributions are included by default. Note that the nonlinear setting determines whether nonlinear corrections are calculated; theget_Pk_interpolator()
method also has a nonlinear argument to specify if you want the linear or nonlinear spectrum returned (to have both linear and nonlinear spectra available request a tuple(False,True)
for the nonlinear argument). All \(k\) values should be in units of \(1/\mathrm{Mpc}\).Pk_grid={...}
: similar toPk_interpolator
except that rather than returning a bicubic spline object it returns the raw power spectrum grid as a(k, z, P(z,k))
set of arrays. Get withget_Pk_grid()
.sigma_R={...}
: RMS linear fluctuation in spheres of radius \(R\) at redshifts \(z\). Takes"z": [list_of_evaluated_redshifts]
,"k_max": [k_max]
,"vars_pairs": [["delta_tot", "delta_tot"], [...]]}
,"R": [list_of_evaluated_R]
. Note that \(R\) is in \(\mathrm{Mpc}\), not \(h^{1}\,\mathrm{Mpc}\). Get withget_sigma_R()
.Hubble={'z': [z_1, ...]}
: Hubble rate at the requested redshifts. Get it withget_Hubble()
.angular_diameter_distance={'z': [z_1, ...]}
: Physical angular diameter distance to the redshifts requested. Get it withget_angular_diameter_distance()
.comoving_radial_distance={'z': [z_1, ...]}
: Comoving radial distance from us to the redshifts requested. Get it withget_comoving_radial_distance()
.sigma8_z={'z': [z_1, ...]}
: Amplitude of rms fluctuations \(\sigma_8\) at the redshifts requested. Get it withget_sigma8()
.fsigma8={'z': [z_1, ...]}
: Structure growth rate \(f\sigma_8\) at the redshifts requested. Get it withget_fsigma8()
.k_max=[...]
: Fixes the maximum comoving wavenumber considered. Other derived parameters that are not included in the input but whose value the likelihood may need.

requested
()¶ Returns the full set of requested cosmological products and parameters.

check_no_repeated_input_extra
()¶ Checks that there are no repeated parameters between input and extra.
Should be called at initialisation, and at the end of every call to must_provide()

get_Cl
(ell_factor=False, units='FIRASmuK2')¶ Returns a dictionary of lensed CMB power spectra and the lensing potential
pp
power spectrum.Set the units with the keyword
units=number'muK2''K2''FIRASmuK2''FIRASK2'
. The default isFIRASmuK2
, which returns CMB \(C_\ell\)’s in FIRAScalibrated \(\mu K^2\), i.e. scaled by a fixed factor of \((2.7255\cdot 10^6)^2\) (except for the lensing potential power spectrum, which is always unitless). ThemuK2
andK2
options use the model’s CMB temperature.If
ell_factor=True
(default:False
), multiplies the spectra by \(\ell(\ell+1)/(2\pi)\) (or by \(\ell^2(\ell+1)^2/(2\pi)\) in the case of the lensing potentialpp
spectrum).

get_unlensed_Cl
(ell_factor=False, units='FIRASmuK2')¶ Returns a dictionary of unlensed CMB power spectra.
For
units
options, seeget_Cl()
.If
ell_factor=True
(default:False
), multiplies the spectra by \(\ell(\ell+1)/(2\pi)\).

get_Hubble
(z, units='km/s/Mpc')¶ Returns the Hubble rate at the given redshift(s)
z
.The redshifts must be a subset of those requested when
must_provide()
was called. The available units are"km/s/Mpc"
(i.e. \(cH(\mathrm(Mpc)^{1})\)) and1/Mpc
.

get_angular_diameter_distance
(z)¶ Returns the physical angular diameter distance in \(\mathrm{Mpc}\) to the given redshift(s)
z
.The redshifts must be a subset of those requested when
must_provide()
was called.

get_comoving_radial_distance
(z)¶ Returns the comoving radial distance in \(\mathrm{Mpc}\) to the given redshift(s)
z
.The redshifts must be a subset of those requested when
must_provide()
was called.

get_Pk_interpolator
(var_pair=('delta_tot', 'delta_tot'), nonlinear=True, extrap_kmax=None)¶ Get a \(P(z,k)\) bicubic interpolation object (
PowerSpectrumInterpolator
).In the interpolator returned, both the input \(k\) and resulting \(P(z,k)\) values are in units of \(1/\mathrm{Mpc}\) (not \(h^{1}\) units).
Parameters:  var_pair – variable pair for power spectrum
 nonlinear – nonlinear spectrum (default True)
 extrap_kmax – use log linear extrapolation beyond max \(k\) computed up
to
extrap_kmax
.
Returns: PowerSpectrumInterpolator
instance.

get_Pk_grid
(var_pair=('delta_tot', 'delta_tot'), nonlinear=True)¶ Get matter power spectrum, e.g. suitable for splining. Returned arrays may be bigger or more densely sampled than requested, but will include required values.
In the grid returned, both \(k\) and \(P(z,k)\) values are in units of \(1/\mathrm{Mpc}\) (not \(h^{1}\) units), and \(z\) and \(k\) are in ascending order.
Parameters:  nonlinear – whether the linear or nonlinear spectrum
 var_pair – which power spectrum
Returns: k
,z
,Pk
, wherek
andz
are 1d arrays, and the 2d arrayPk[i,j]
is the value of \(P(z,k)\) atz[i]
,k[j]
.

get_sigma_R
(var_pair=('delta_tot', 'delta_tot'))¶ Get \(\sigma_R(z)\), the RMS power in an sphere of radius \(R\) at redshift \(z\).
Note that \(R\) is in \(\mathrm{Mpc}\), not \(h^{1}\,\mathrm{Mpc}\), and \(z\) and \(R\) are returned in ascending order.
You may get back more values than originally requested, but the requested \(R\) and \(z\) should be in the returned arrays.
Parameters: var_pair – which two fields to use for the RMS power Returns: R
,z
,sigma_R
, whereR
andz
are arrays of computed values, andsigma_R[i,j]
is the value \(\sigma_R(z)\) forz[i]
,R[j]
.

get_source_Cl
()¶ Returns a dict of power spectra of for the computed sources, with keys a tuple of sources
([source1], [source2])
, and an additional keyell
containing the multipoles.

get_sigma8_z
(z)¶ Present day linear theory rootmeansquare amplitude of the matter fluctuation spectrum averaged in spheres of radius 8 h^{−1} Mpc.
The redshifts must be a subset of those requested when
must_provide()
was called.

get_fsigma8
(z)¶ Structure growth rate \(f\sigma_8\), as defined in eq. 33 of Planck 2015 results. XIII. Cosmological parameters, at the given redshift(s)
z
.The redshifts must be a subset of those requested when
must_provide()
was called.

get_auto_covmat
(params_info, likes_info, random_state=None)¶ Tries to get match to a database of existing covariance matrix files for the current model and data.
params_info
should contain preferably the slow parameters only.


class
theories.cosmo.
PowerSpectrumInterpolator
(z, k, P_or_logP, extrap_kmax=None, logP=False, logsign=1)¶ 2D spline interpolation object (scipy.interpolate.RectBivariateSpline) to evaluate matter power spectrum as function of z and k.
This class is adapted from CAMB’s own P(k) interpolator, by Antony Lewis; it’s mostly interfacecompatible with the original.
Parameters:  z – values of z for which the power spectrum was evaluated.
 k – values of k for which the power spectrum was evaluated.
 P_or_logP – Values of the power spectrum (or logvalues, if logP=True).
 logP – if True (default: False), log of power spectrum are given and used for the underlying interpolator.
 logsign – if logP is True, P_or_logP is log(logsign*Pk)
 extrap_kmax – if set, use power law extrapolation beyond kmax up to extrap_kmax; useful for tails of integrals.

P
(z, k, grid=None)¶ Get the power spectrum at (z,k).

logP
(z, k, grid=None)¶ Get the log power spectrum at (z,k). (or minus log power spectrum if islog and logsign=1)