In astronomy, angular diameter distance is a distance defined in terms of an object's physical size, ${\displaystyle x}$, and its angular size, ${\displaystyle \theta }$, as viewed from Earth:

$${\displaystyle d_{A}={\frac {x}{\theta }}}$$

Cosmology dependence

The angular diameter distance depends on the assumed cosmology of the universe. The angular diameter distance to an object at redshift, ${\displaystyle z}$, is expressed in terms of the comoving distance, ${\displaystyle r}$ as:

$${\displaystyle d_{A}={\frac {S_{k}(r)}{1+z}}}$$

where ${\displaystyle S_{k}(r)}$ is the FLRW coordinate defined as:

$${\displaystyle S_{k}(r)={\begin{cases}\sin \left(H_{0}{\sqrt {|\Omega _{k}|}}r\right)/\left(H_{0}{\sqrt {|\Omega _{k}|}}\right)&\Omega _{k}<0\\r&\Omega _{k}=0\\\sinh \left(H_{0}{\sqrt {|\Omega _{k}|}}r\right)/\left(H_{0}{\sqrt {|\Omega _{k}|}}\right)&\Omega _{k}>0\end{cases}}}$$

where ${\displaystyle \Omega _{k}}$ is the curvature density and ${\displaystyle H_{0}}$ is the value of the Hubble parameter today.

In the currently favoured geometric model of our Universe, the "angular diameter distance" of an object is a good approximation to the "real distance", i.e. the proper distance when the light left the object.

Angular size redshift relation

The angular size redshift relation for a Lambda cosmology, with on the vertical scale kiloparsecs per arcsecond.

The angular size redshift relation for a Lambda cosmology, with on the vertical scale megaparsecs.

The angular size redshift relation describes the relation between the angular size observed on the sky of an object of given physical size, and the object's redshift from Earth (which is related to its distance, ${\displaystyle d}$, from Earth). In a Euclidean geometry the relation between size on the sky and distance from Earth would simply be given by the equation:

$${\displaystyle \tan \left(\theta \right)={\frac {x}{d}}.}$$

where ${\displaystyle \theta }$ is the angular size of the object on the sky, ${\displaystyle x}$ is the size of the object and ${\displaystyle d}$ is the distance to the object. Where ${\displaystyle \theta }$ is small this approximates to:

$${\displaystyle \theta \approx {\frac {x}{d}}.}$$

However, in the ΛCDM model, the relation is more complicated. In this model, objects at redshifts greater than about 1.5 appear larger on the sky with increasing redshift.

This is related to the angular diameter distance, which is the distance an object is calculated to be at from ${\displaystyle \theta }$ and ${\displaystyle x}$, assuming the Universe is Euclidean.

The Mattig relation yields the angular-diameter distance, ${\displaystyle d_{A}}$, as a function of redshift z for a universe with Ω_Λ = 0.^[1] ${\displaystyle q_{0}}$ is the present-day value of the deceleration parameter, which measures the deceleration of the expansion rate of the Universe; in the simplest models, ${\displaystyle q_{0}<0.5}$ corresponds to the case where the Universe will expand forever, ${\displaystyle q_{0}>0.5}$ to closed models which will ultimately stop expanding and contract, ${\displaystyle q_{0}=0.5}$ corresponds to the critical case – Universes which will just be able to expand to infinity without re-contracting.

$${\displaystyle d_{A}={\cfrac {c}{H_{0}q_{0}^{2}}}{\cfrac {(zq_{0}+(q_{0}-1)({\sqrt {2q_{0}z+1}}-1))}{(1+z)^{2}}}}$$

See also

• Distance measure
• Standard ruler

References

External links

• iCosmos: Cosmology Calculator (With Graph Generation )