clevar.cosmology.parent_class module¶
- class clevar.cosmology.parent_class.Cosmology(**kwargs)[source]¶
Bases:
objectCosmology object superclass for supporting multiple back-end cosmology objects
- Variables
~Cosmology.backend (str) – Name of back-end used
~Cosmology.be_cosmo (cosmology library) – Cosmology library used in the back-end
- eval_da(z)[source]¶
Computes the angular diameter distance between 0.0 and z.
\[d_a(z) = \frac{c}{H_0}\frac{1}{1+z}\int_{0}^{z}\frac{dz'}{E(z')}\]- Parameters
z (float) – Redshift.
- Returns
Angular diameter distance in units \(M\!pc\)
- Return type
float
Notes
Describe the vectorization.
- eval_da_z1z2(z1, z2)[source]¶
Computes the angular diameter distance between z1 and z2.
\[d_a(z1, z2) = \frac{c}{H_0}\frac{1}{1+z2}\int_{z1}^{z2}\frac{dz'}{E(z')}\]- Parameters
z1 (float) – Redshift.
z2 (float) – Redshift.
- Returns
Angular diameter distance in units \(M\!pc\)
- Return type
float
Notes
Describe the vectorization.
- eval_mass2radius(mass, z, delta=200, mass_type='background')[source]¶
Computes the radius from M_Delta
\[R_{\Delta} = \left(\frac{3M_{\Delta}}{4\pi\Delta\rho}\right)^{1/3}\]where \(\rho\) can be background or matter.
- Parameters
MASS (float, array) – Mass of the volume in M_sun
z (float, array) – Redshift
delta (int, float) – Delta
- Returns
Radius in Mpc
- Return type
float, array
- get_E2(z)[source]¶
Gets hubble parameter squared (normalized at 0)
\[E^{2}(z) = \frac{H(z)^{2}}{H_{0}^{2}}.\]- Parameters
z (float) – Redshift.
- Returns
E – Dimensionless normalized hubble parameter
- Return type
float
- get_Omega_m(z)[source]¶
Gets the value of the dimensionless matter density
\[\Omega_m(z) = \frac{\rho_m(z)}{\rho_\mathrm{crit}(z)}.\]- Parameters
z (float) – Redshift.
- Returns
Omega_m – dimensionless matter density, \(\Omega_m(z)\).
- Return type
float
Notes
Need to decide if non-relativist neutrinos will contribute here.
- mpc2rad(dist1, redshift)[source]¶
Convert between Mpc and radians using the small angle approximation and \(d = D_A \theta\).
- Parameters
dist1 (array_like) – Input distances in Mpc
redshift (float) – Redshift used to convert between angular and physical units
cosmo (astropy.cosmology) – Astropy cosmology object to compute angular diameter distance to convert between physical and angular units
do_inverse (bool) – If true, converts Mpc to radians
- Returns
dist2 – Distances in radians
- Return type
array_like
- rad2mpc(dist1, redshift)[source]¶
Convert between radians and Mpc using the small angle approximation and \(d = D_A \theta\).
- Parameters
dist1 (array_like) – Input distances in radians
redshift (float) – Redshift used to convert between angular and physical units
cosmo (astropy.cosmology) – Astropy cosmology object to compute angular diameter distance to convert between physical and angular units
do_inverse (bool) – If true, converts Mpc to radians
- Returns
dist2 – Distances in Mpc
- Return type
array_like