Previously set parameters and called calc_power_spectra() (e.g. Params – optional CAMBparams instance with parameters to use. If xvals is explicitly given, instead calculates correlations at provided \(\cos(\theta)\) values. Get the CMB correlation functions from the power spectra.īy default evaluated at points \(\cos(\theta)\) = xvals that are roots of Legendre polynomials,įor accurate back integration with rr2cl(). N_eta x len(vars) 2D numpy array of outputs or dict of 1D arrays get_cmb_correlation_functions ( params = None, lmax = None, spectrum = 'lensed_scalar', xvals = None, sampling_factor = 1 ) ¶
Get the evolution of background variables a function of conformal time.Įta – array of requested conformal times to output N_eta x len(vars) 2D numpy array of outputs or dict of 1D arrays get_background_time_evolution ( eta, vars =, format = 'dict' ) ¶ Z – array of requested redshifts to output
Get the evolution of background variables a function of redshift.įor the moment a and H are rather perversely only available via get_time_evolution() Parameters
Rs/DV, H, DA, F_AP for each requested redshift (as 2D array) get_background_redshift_evolution ( z, vars =, format = 'dict' ) ¶ Get BAO values for redshifts set in Params.z_outputs Returns N_a x len(vars) 2D numpy array or dict of 1D arrays of \(8\pi G a^4 \rho_i\) in Mpc units. Vars – list of variables to output (default all)įormat – ‘dict’ or ‘array’, for either dict of 1D arrays indexed by name, or 2D array ParametersĪ – scale factor or array of scale factors \(\Omega_i\) can be simply obtained by taking the ratio of the components to tot. Returns \(8\pi G a^4 \rho_i\) in Mpc units. Get the individual densities as a function of scale factor. \(\Omega_i(a)\) get_background_densities ( a, vars =, format = 'dict' ) ¶ Var – one of ‘K’, ‘cdm’, ‘baryon’, ‘photon’, ‘neutrino’ (massless), ‘nu’ (massive neutrinos), ‘de’ Get density relative to critical density of variables var Parameters Params – optional CAMBparams instance to useĪrray of rs/DV, H, DA, F_AP for each redshift as 2D array get_Omega ( var, z = 0 ) ¶ Get BAO parameters at given redshifts, using parameters in params Parameters Omega_de – ( float64) Omega for dark energy todayĬurvature_radius – ( float64) \(1/\sqrt\) get_BAO ( redshifts, params ) ¶ Tau_maxvis – ( float64) time at peak visibilityĪdotrad – ( float64) da/d tau in early radiation-dominated era Taurend – ( float64) time at end of recombination Taurst – ( float64) time at start of recombinationĭtaurec – ( float64) time step in recombination Grhok – ( float64) curvature contribution to critical density Grhornomass – ( float64) grhor*number of massless neutrino species Grhov – ( float64) Dark energy contribution ThermoDerivedParams – ( float64 array) array of derived parameters, see get_derived_params() to get as a dictionary To quickly make a fully calculated CAMBdata instance for a set of parameters you can call camb.get_results(). Exactly which quantities are already calculated depends on which of these functions you use and the Results for a set of parameters (given in a CAMBparams instance)Īre returned by the camb.get_background(), camb.get_transfer_functions() or camb.get_results()įunctions. CAMBdata ( * args, ** kwargs ) ¶Īn object for storing calculational data, parameters and transfer functions. Calculation results ¶ class camb.results.