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Internals

The following types and methods are internal, and should not be considered safe for public use.

Types

Cosmology.FlatLCDM — Type
struct FlatLCDM{T<:Real} <: Cosmology.AbstractFlatCosmology

ΛCDM model of the universe with $Ω_k = 0$.

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Cosmology.ClosedLCDM — Type
struct ClosedLCDM{T<:Real} <: Cosmology.AbstractClosedCosmology

ΛCDM model of the universe with $Ω_k < 0$.

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Cosmology.OpenLCDM — Type
struct OpenLCDM{T<:Real} <: Cosmology.AbstractOpenCosmology

ΛCDM model of the universe with $Ω_k > 0$.

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Cosmology.FlatWCDM — Type
struct FlatWCDM{T<:Real} <: Cosmology.AbstractFlatCosmology

wCDM model of the universe with $Ω_k = 0$.

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Cosmology.ClosedWCDM — Type
struct ClosedWCDM{T<:Real} <: Cosmology.AbstractClosedCosmology

wCDM model of the universe with $Ω_k < 0$.

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Cosmology.OpenWCDM — Type
struct OpenWCDM{T<:Real} <: Cosmology.AbstractOpenCosmology

wCDM model of the universe with $Ω_k > 0$.

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Methods

Cosmology.E — Function
E(c::AbstractCosmology, z)

Dimensionless Hubble function $E(z)$ at redshift z. It's defined as

\[E(z) ≡ \frac{H(z)}{H_0} = \frac{H(z)}{(100\mathrm{km/s/Mpc}) h}\]

where $H_0 = H(z=0)$ is the Hubble parameter at the present epoch (Schneider 2015, p. 183).

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Cosmology.Z — Function
Z(c::AbstractCosmology, z, nothing; kws...)
Z(c::AbstractCosmology, z₁, z₂; kws...)

The line-of-sight comoving distance contributions for comoving radial distance.

It performs the integral

\[Z = \int_{z_1}^{z_2} \frac{dz}{E(z)} = \int_{a_2}^{a_1} \frac{da}{a^2 E(a)}\]

where we can perform a change of variables with $a = 1/(1+z)$, and $dz = -da/a^2$.

If nothing is used for the second bound of integration, it defaults to z₁ = 0 (i.e., a₁ = 1).

See also

comoving_radial_dist

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Cosmology.T — Function
T(c::AbstractCosmology, a0, a1; kws...)

The line-of-sight contributions for lookback time.

It performs the integral

\[T = \int_{a_0}^{a_1} \frac{da}{a E(a)}\]

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Cosmology.a2E — Function
a2E(c::AbstractCosmology, a)

Calculates the intermediate quantity $a^2 E(a)$. This is an internal function used to simplify computation.

Mathematical definition for ΛCDM models:

\[a^2 E(a) = \sqrt{Ω_r + Ω_m a + Ω_k a^2 + Ω_Λ a^4}\]

and for wCDM models:

\[a^2 E(a) = \sqrt{Ω_r + Ω_m a + Ω_k a^2 + Ω_Λ a_{de}}\]

where $Ω_k = 0$ for a flat cosmological model, and $a_{de} = a^{1 - 3(w_0 + w_a)} \exp(3 w_a (a - 1))$ (Scherrer, 2015).

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Bibliography