Bases: astropy.cosmology.core.Cosmology
A class describing an isotropic and homogeneous (Friedmann-Lemaitre-Robertson-Walker) cosmology.
This is an abstract base class – you can’t instantiate examples of this class, but must work with one of its subclasses such as LambdaCDM or wCDM.
Notes
Class instances are static – you can’t change the values of the parameters. That is, all of the attributes above are read only.
The neutrino treatment assumes all neutrino species are massless.
Attributes Summary
Neff | Number of effective neutrino species |
critical_density0 | Critical density in [g cm^-3] at z=0 |
Ogamma0 | Omega gamma; the density/critical density of photons at z=0 |
hubble_distance | Hubble distance in [Mpc] |
Tcmb0 | Temperature of the CMB in Kelvin at z=0 |
hubble_time | Hubble time in [Gyr] |
Onu0 | Omega nu; the density/critical density of neutrinos at z=0 |
Ode0 | Omega dark energy; dark energy density/critical density at z=0 |
Ok0 | Omega curvature; the effective curvature density/critical density |
h | Dimensionless Hubble constant: h = H_0 / 100 [km/sec/Mpc] |
Om0 | Omega matter; matter density/critical density at z=0 |
H0 | Return the Hubble constant in [km/sec/Mpc] at z=0 |
Methods Summary
angular_diameter_distance(z) | Angular diameter distance in Mpc at a given redshift. |
Ok(z) | Return the equivalent density parameter for curvature at redshift z. |
Ogamma(z) | Return the density parameter for photons at redshift z. |
comoving_transverse_distance(z) | Comoving transverse distance in Mpc at a given redshift. |
critical_density(z) | Critical density in grams per cubic cm at redshift z. |
lookback_time(z) | Lookback time in Gyr to redshift z. |
absorption_distance(z) | Absorption distance at redshift z. |
inv_efunc(z) | Inverse of efunc. |
Tcmb(z) | Return the CMB temperature at redshift z. |
de_density_scale(z) | Evaluates the redshift dependence of the dark energy density. |
Om(z) | Return the density parameter for non-relativistic matter at redshift z. |
scale_factor(z) | Scale factor at redshift z. |
H(z) | Hubble parameter (km/s/Mpc) at redshift z. |
efunc(z) | Function used to calculate H(z), the Hubble parameter. |
distmod(z) | Distance modulus at redshift z. |
comoving_distance(z) | Comoving line-of-sight distance in Mpc at a given redshift. |
age(z) | Age of the universe in Gyr at redshift z. |
Ode(z) | Return the density parameter for dark energy at redshift z. |
luminosity_distance(z) | Luminosity distance in Mpc at redshift z. |
angular_diameter_distance_z1z2(z1, z2) | Angular diameter distance between objects at 2 redshifts. |
w(z) | The dark energy equation of state. |
comoving_volume(z) | Comoving volume in cubic Mpc at redshift z. |
Onu(z) | Return the density parameter for massless neutrinos at redshift z. |
Attributes Documentation
Methods Documentation
Angular diameter distance in Mpc at a given redshift.
This gives the proper (sometimes called ‘physical’) transverse distance corresponding to an angle of 1 radian for an object at redshift z.
Weinberg, 1972, pp 421-424; Weedman, 1986, pp 65-67; Peebles, 1993, pp 325-327.
Parameters : | z : array_like
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Returns : | d : ndarray, or float if input scalar
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Return the equivalent density parameter for curvature at redshift z.
Parameters : | z : array_like
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Returns : | Ok : ndarray, or float if input scalar
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Return the density parameter for photons at redshift z.
Parameters : | z : array_like
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Returns : | Ogamma : ndarray, or float if input scalar
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Comoving transverse distance in Mpc at a given redshift.
This value is the transverse comoving distance at redshift z corresponding to an angular separation of 1 radian. This is the same as the comoving distance if omega_k is zero (as in the current concordance lambda CDM model).
Parameters : | z : array_like
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Returns : | d : ndarray, or float if input scalar
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Notes
This quantity also called the ‘proper motion distance’ in some texts.
Critical density in grams per cubic cm at redshift z.
Parameters : | z : array_like
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Returns : | rho : ndarray, or float if input scalar
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Lookback time in Gyr to redshift z.
The lookback time is the difference between the age of the Universe now and the age at redshift z.
Parameters : | z : array_like
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Returns : | t : ndarray, or float if input scalar
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Absorption distance at redshift z.
This is used to calculate the number of objects with some cross section of absorption and number density intersecting a sightline per unit redshift path.
Parameters : | z : array_like
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Returns : | d : ndarray, or float if input scalar
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References
Hogg 1999 Section 11. (astro-ph/9905116) Bahcall, John N. and Peebles, P.J.E. 1969, ApJ, 156L, 7B
Inverse of efunc.
Parameters : | z : array_like
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Returns : | E : ndarray, or float if input scalar
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Return the CMB temperature at redshift z.
Parameters : | z : array_like
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Returns : | Tcmb : ndarray, or float if z is scalar
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Evaluates the redshift dependence of the dark energy density.
Parameters : | z : array_like
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Returns : | I : ndarray, or float if input scalar
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Notes
The scaling factor, I, is defined by , and is given by
It will generally helpful for subclasses to overload this method if the integral can be done analytically for the particular dark energy equation of state that they implement.
Return the density parameter for non-relativistic matter at redshift z.
Parameters : | z : array_like
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Returns : | Om : ndarray, or float if input scalar
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Scale factor at redshift z.
The scale factor is defined as .
Parameters : | z : array_like
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Returns : | a : ndarray, or float if input scalar
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Hubble parameter (km/s/Mpc) at redshift z.
Parameters : | z : array_like
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Returns : | H : ndarray, or float if input scalar
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Function used to calculate H(z), the Hubble parameter.
Parameters : | z : array_like
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Returns : | E : ndarray, or float if input scalar
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Notes
The return value, E, is defined such that .
It is not necessary to override this method, but if de_density_scale takes a particularly simple form, it may be advantageous to.
Distance modulus at redshift z.
The distance modulus is defined as the (apparent magnitude - absolute magnitude) for an object at redshift z.
Parameters : | z : array_like
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Returns : | distmod : ndarray, or float if input scalar
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Comoving line-of-sight distance in Mpc at a given redshift.
The comoving distance along the line-of-sight between two objects remains constant with time for objects in the Hubble flow.
Parameters : | z : array_like
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Returns : | d : ndarray, or float if input scalar
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Age of the universe in Gyr at redshift z.
Parameters : | z : array_like
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Returns : | t : ndarray, or float if input scalar
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Return the density parameter for dark energy at redshift z.
Parameters : | z : array_like
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Returns : | Ode : ndarray, or float if input scalar
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Luminosity distance in Mpc at redshift z.
This is the distance to use when converting between the bolometric flux from an object at redshift z and its bolometric luminosity.
Parameters : | z : array_like
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Returns : | d : ndarray, or float if input scalar
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References
Weinberg, 1972, pp 420-424; Weedman, 1986, pp 60-62.
Angular diameter distance between objects at 2 redshifts. Useful for gravitational lensing.
Parameters : | z1, z2 : array_like, shape (N,)
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Returns : | d : ndarray, shape (N,) or float if input scalar
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Raises : | CosmologyError :
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Notes
This method only works for flat or open curvature (omega_k >= 0).
The dark energy equation of state.
Parameters : | z : array_like
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Returns : | w : ndarray, or float if input scalar
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Notes
The dark energy equation of state is defined as , where is the pressure at redshift z and is the density at redshift z, both in units where c=1.
This must be overridden by subclasses.
Comoving volume in cubic Mpc at redshift z.
This is the volume of the universe encompassed by redshifts less than z. For the case of omega_k = 0 it is a sphere of radius comoving_distance(z) but it is less intuitive if omega_k is not 0.
Parameters : | z : array_like
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Returns : | V : ndarray, or float if input scalar
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Return the density parameter for massless neutrinos at redshift z.
Parameters : | z : array_like
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Returns : | Onu : ndarray, or float if input scalar
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