wcosmo.wcosmo

Functional implementation of cosmological parameters.

Note

This module is intended to be used as a functional alternative to the astropy class-based method. In general, units will be propagated when using numpy, but all of the code can also be used without units. Special care is needed with hubble_distance() and hubble_time() as these functions use constants which have units unless wcosmo.utils.disable_units() has been called.

absorption_distance(z, Om0[, w0, method])	Compute the absorption distance using an analytic integral of the Pade approximation.
comoving_distance(z, H0, Om0[, w0, method])	Compute the comoving distance using an analytic integral of the Pade approximation.
comoving_volume(z, H0, Om0[, w0, method])	Compute the comoving volume out to redshift z.
detector_to_source_frame(m1z, m2z, dL, H0, Om0)	Convert masses and luminosity distance from the detector frame to source frame masses and redshift.
differential_comoving_volume(z, H0, Om0[, ...])	Compute the differential comoving volume element.
dDLdz(z, H0, Om0[, w0, method])	The Jacobian for the conversion of redshift to luminosity distance.
efunc(z, Om0[, w0])	Compute the \(E(z)\) function for a flat wCDM cosmology.
hubble_distance(H0, *[, xp])	Compute the Hubble distance \(D_H = c H_0^{-1}\) in Mpc.
hubble_parameter(z, H0, Om0[, w0])	Compute the Hubble parameter \(H(z)\) for a flat wCDM cosmology.
hubble_time(H0, *[, xp])	Compute the Hubble time \(t_H = H_0^{-1}\) in Gyr.
inv_efunc(z, Om0[, w0])	Compute the inverse of the E(z) function for a flat wCDM cosmology.
lookback_time(z, H0, Om0[, w0, method])	Compute the lookback time using an analytic integral of the Pade approximation.
luminosity_distance(z, H0, Om0[, w0, method])	Compute the luminosity distance using an analytic integral of the Pade approximation.
source_to_detector_frame(m1, m2, z, H0, Om0)	Convert masses and redshift from the source frame to the detector frame.
z_at_value(func, fval[, zmin, zmax])	Compute the redshift at which a function equals a given value.