Angular diameter distance

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

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

The angular diameter distance depends on the assumed cosmology of the universe. The angular diameter distance to an object at redshift, $z$ , is expressed in terms of the comoving distance, $r$ as:
$d_{A}={\frac {S_{k}(r)}{1+z}}$
Where $S_{k}(r)$ is the FLRW coordinate defined as:
$S_{k}(r)={\begin{cases}\sin \left({\sqrt {-\Omega _{k}}}H_{0}r\right)/\left(H_{0}{\sqrt {|\Omega _{k}|}}\right)&\Omega _{k}<0\\r&\Omega _{k}=0\\\sinh \left({\sqrt {\Omega _{k}}}H_{0}r\right)/\left(H_{0}{\sqrt {|\Omega _{k}|}}\right)&\Omega _{k}>0\end{cases}}$
Where $\Omega _{k}$ is the curvature density and $H_{0}$ 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. Note that beyond a certain redshift, the angular diameter distance gets smaller with increasing redshift. In other words, an object "behind" another of the same size, beyond a certain redshift (roughly z=1.5), appears larger on the sky, and would therefore have a smaller "angular diameter distance".

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 objects redshift from Earth (which is related to its distance, $d$ , from Earth). In a Euclidean geometry the relation between size on the sky and distance from Earth would simply be given by the equation:

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

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

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

However, in the ΛCDM model (the currently favored cosmology), 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 $\theta$ and $x$ , assuming the Universe is Euclidean.

The actual relation between the angular-diameter distance, $d_{A}$ , and redshift is given below. $q_{0}$ is the present-day value of the deceleration parameter, which measures the deceleration of the expansion rate of the Universe; in the simplest models, $q_{0}<0.5$ corresponds to the case where the Universe will expand forever, $q_{0}>0.5$ to closed models which will ultimately stop expanding and contract $q_{0}=0.5$ corresponds to the critical case – Universes which will just be able to expand to infinity without re-contracting.

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

The Mattig relation yields the angular-diameter distance as a function of redshift for a universe with Ω_Λ = 0.[1]

References

Derek Raine; E.G. Thomas (2001). "Chapter 6:2". An Introduction to the Science of Cosmology. CRC Press. p. 102. ISBN 978-0-7503-0405-4.

External links

iCosmos: Cosmology Calculator (With Graph Generation )

This article is issued from Wikipedia. The text is licensed under Creative Commons - Attribution - Sharealike. Additional terms may apply for the media files.

[1] Derek Raine; E.G. Thomas (2001). "Chapter 6:2". An Introduction to the Science of Cosmology. CRC Press. p. 102. ISBN 978-0-7503-0405-4.

Angular diameter distance

Angular size redshift relation

See also

References

External links