galapy.Cosmology
The Cosmology module defines a Cosmology class whose just a wrapper for interpolation on grid of Luminosity Distances and Ages
Classes
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Class for cosmological computations. |
- class galapy.Cosmology.CSM(cosmo)
Class for cosmological computations. It is built using pre-computed redshift-dependent quantities useful for transforming energies radiated per unit wavelength into fluxes from objects at a given distance.
- Parameters:
cosmo (string or dictionary) – If a string is passed, it should name one of the pre-computed cosmologies available in the database. Available cosmologies are
('WMAP7', 'WMAP9', 'Planck15', 'Planck18'). If a dictionary is passed, the class expects to find 3 key-value couples: (i) key = ‘redshift’, value = an array of redshift values; (ii) key = ‘luminosity_distance’, value = an array of luminosity distances corresponding to the redshift values of the first key-value couple; (iii) key = ‘age’, value = an array of ages of the Universe corresponding to the redshift values of the first key-value couple. All these arrays should have the same length.
- DL
interpolator interface to luminosity distance
- Type:
galapy.internal.interp.lin_interp
- UA
interpolator interface to age of the universe
- Type:
galapy.internal.interp.lin_interp
Examples
Interpolator attributes can be called as functions that take as input a redshift value (or an array of redshift values):
>>> from galapy.Cosmology import CSM >>> csm = CSM('Planck18') >>> csm.DL(1.0) 6791.26894
The returned value is in MegaParsecs for the luminosity distance and in years for the age.
- to_flux(redshift, restframe_wavelength, luminosity)
Converts a restframe luminosity to the flux received at a given redshift.
\[S_{\lambda_O} = \lambda_R^2 L_\text{tot}(\lambda_R) (1+z) / (4 \pi c D_L^2 )\]- Parameters:
redshift (float) – redshift of the source
restframe_wavelength (array-like) – rest-frame wavelength grid
luminosity (array-like) – rest-frame luminosity grid
- Returns:
a flux in milliJansky
- Return type:
array-like