Angular diameter distance

The angular diameter distance is a distance measure used in astronomy. It is defined in terms of an object's physical size, x {displaystyle x} , and θ {displaystyle heta } the angular size of the object as viewed from earth. d A = x θ {displaystyle d_{A}={frac {x}{ heta }}} The angular diameter distance depends on the assumed cosmology of the universe. The angular diameter distance to an object at redshift, z {displaystyle z} , is expressed in terms of the comoving distance, r {displaystyle r} as: d A = S k ( r ) 1 + z {displaystyle d_{A}={frac {S_{k}(r)}{1+z}}} Where S k ( r ) {displaystyle S_{k}(r)} is the FLRW coordinate defined as: S k ( r ) = { sin ⁡ ( − Ω k H 0 r ) / ( H 0 | Ω k | ) Ω k < 0 r Ω k = 0 sinh ⁡ ( Ω k H 0 r ) / ( H 0 | Ω k | ) Ω k > 0 {displaystyle S_{k}(r)={egin{cases}sin left({sqrt {-Omega _{k}}}H_{0}r ight)/left(H_{0}{sqrt {|Omega _{k}|}} ight)&Omega _{k}<0\r&Omega _{k}=0\sinh left({sqrt {Omega _{k}}}H_{0}r ight)/left(H_{0}{sqrt {|Omega _{k}|}} ight)&Omega _{k}>0end{cases}}} Where Ω k {displaystyle Omega _{k}} is the curvature density and H 0 {displaystyle H_{0}} is the value of the Hubble parameter today. The angular diameter distance is a distance measure used in astronomy. It is defined in terms of an object's physical size, x {displaystyle x} , and θ {displaystyle heta } the angular size of the object as viewed from earth. d A = x θ {displaystyle d_{A}={frac {x}{ heta }}} The angular diameter distance depends on the assumed cosmology of the universe. The angular diameter distance to an object at redshift, z {displaystyle z} , is expressed in terms of the comoving distance, r {displaystyle r} as: d A = S k ( r ) 1 + z {displaystyle d_{A}={frac {S_{k}(r)}{1+z}}} Where S k ( r ) {displaystyle S_{k}(r)} is the FLRW coordinate defined as: S k ( r ) = { sin ⁡ ( − Ω k H 0 r ) / ( H 0 | Ω k | ) Ω k < 0 r Ω k = 0 sinh ⁡ ( Ω k H 0 r ) / ( H 0 | Ω k | ) Ω k > 0 {displaystyle S_{k}(r)={egin{cases}sin left({sqrt {-Omega _{k}}}H_{0}r ight)/left(H_{0}{sqrt {|Omega _{k}|}} ight)&Omega _{k}<0\r&Omega _{k}=0\sinh left({sqrt {Omega _{k}}}H_{0}r ight)/left(H_{0}{sqrt {|Omega _{k}|}} ight)&Omega _{k}>0end{cases}}} Where Ω k {displaystyle Omega _{k}} is the curvature density and H 0 {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. 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'. 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 {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: where θ {displaystyle heta } is the angular size of the object on the sky, x {displaystyle x} is the size of the object and d {displaystyle d} is the distance to the object. Where θ {displaystyle heta } is small this approximates to: θ ≈ x d {displaystyle heta 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 θ {displaystyle heta } and x {displaystyle x} , assuming the Universe is Euclidean. The actual relation between the angular-diameter distance, d A {displaystyle d_{A}} , and redshift is given below. q 0 {displaystyle q_{0}} is called the deceleration parameter and measures the deceleration of the expansion rate of the Universe; in the simplest models, q 0 < 0.5 {displaystyle q_{0}<0.5} corresponds to the case where the Universe will expand for ever, q 0 > 0.5 {displaystyle q_{0}>0.5} to closed models which will ultimately stop expanding and contract q 0 = 0.5 {displaystyle q_{0}=0.5} corresponds to the critical case – Universes which will just be able to expand to infinity without re-contracting.