The flux density S as a function of frequency
and the angular
size
of a radio
source are the observables directly relevant to most cosmological
problems. They
are related to the intrinsic source luminosity L and projected linear
size d as described below.
Consider an isotropic source at redshift z with spectral luminosity
L at frequency
(measured in the source
frame). Its spectral flux density S measured at the same frequency
(in the observer's frame) will be
![]() |
(15.1) |
where A is the area of the sphere centered on the source and
containing the observer and
- ln(S /
S0) / ln(
/
0) is the two-point
spectral index between the frequencies
and
0 =
/ (1 + z) in the
observer's frame. (Note that the negative sign convention
for
is used throughout
this chapter.) The
(1 + z)1+
term expresses the special
relativistic Doppler correction; the geometry and expansion dynamics of the
universe appear only in A. An "effective distance" D
(Longair 1978)
can be defined by A
4
D2. Since
the area of the sphere centered on the observer and containing
a source at redshift z is always
A / (1 + z)2, the relation between
(projected) linear size d and measured angular size
is
![]() |
(15.2) |
The "angular size" distance is defined by
D
d /
= D /
(1 + z). The "bolometric luminosity distance"
Dbol defined by
Sbol = Lbol /
(4
Dbol2) is given by
Dbol = D(1 + z).
In Friedmann models (cosmological constant
= 0) with zero
pressure, density parameter
=
2q0, and current Hubble parameter H0
the effective distance is traditionally given
(Mattig 1958) as
![]() |
(15.3) |
However, this formula is numerically unstable for small
z, the
transformation (based on
Terrell 1977)
![]() |
(15.4) |
is better for numerical calculations. For particular values of
, D reduces
to the simpler forms:
![]() |
(15.5a)
|
To describe the distributions of sources in space and time, we also need
the comoving volume dV of the spherical shell extending from
z to z + dz. It is
dV = 4
D2 dr, where the comoving radial coordinate
element is dr = - (1 + z)c dt. In a Friedmann
universe the expansion rate is
![]() |
(15.6) |
so
![]() |
(15.7) |