Extragalactic Redshifts
# Extragalactic Redshifts

John Huchra, Harvard-Smithsonian Center for Astrophysics

Last update 8 May 2009

The redshift (or blueshift) of a galaxy is the shifting of its
spectral features to longer (or shorter) wavelengths primarily due to the
combination of Doppler motions and the general expansion
of the Universe. More properly, the term **radial velocity**
is used primarily for the Doppler motions, which are usually the result of
gravitational interactions, while **redshift** is reserved for
the cosmological effects, although it is not generally possible to separate
out cosmological expansion and Doppler velocities except for nearby galaxies
and those known to be members of galaxy clusters.

Redshift, z, is defined in wavelength as
$\begin{array}{cc}\phantom{\rule{6.0em}{0ex}}& z=\genfrac{}{}{0.1ex}{}{{\lambda}_{o}-{\lambda}_{e}}{{\lambda}_{e}}=\genfrac{}{}{0.1ex}{}{{\lambda}_{o}}{{\lambda}_{e}}-1\hfill \end{array}$

where the subscripts *o* and *e* refer to observed and emitted.
In the frequency domain, redshift is defined as

$\begin{array}{cc}\phantom{\rule{6.0em}{0ex}}& z=\genfrac{}{}{0.1ex}{}{{\nu}_{e}-{\nu}_{0}}{{\nu}_{0}}=\genfrac{}{}{0.1ex}{}{{\nu}_{e}}{{\nu}_{0}}-1\hfill \end{array}$

The dichotomy between these formulae is due to the fact that redshift causes
wavelengths to increase and frequencies to decrease.

The redshift of any given galaxy can be decomposed as

$\begin{array}{cc}\phantom{\rule{6.0em}{0ex}}& {z}_{total}={z}_{grav}+{z}_{physical}+{z}_{H}\hfill \end{array}$

where z_{H} is the cosmological redshift due to Hubble expansion,
and z_{physical} is the redshift due to the physical motion of the
object with respect to the observer. In an expanding universe, the
cosmological redshift is always positive (objects are always redshifted).
The gravitational redshift z_{grav} for galaxies and quasars is usually
neglected since it is a very small part of the observed redshift in almost every
case. The physical motions of galaxies with respect to their neighbors or the
general expansion of the Universe can produce both redshifts and
blueshifts, depending on whether the induced motion is away from or
towards the observer, respectively.

Physical motions are most often gravitational in nature, such as the orbital
motion of the Earth around the Sun. The Earth is in a nearly circular orbit
around the Sun at a velocity of ~29.7 km/s. An observer at the outskirts
of the Solar system and in the plane of Earth's orbit would see the velocity
of the Earth relative to the Sun vary sinusoidally between +29.7 and
-29.7 km/s.
On cosmological scales, physical velocities are also generally caused by the
orbital motions of galaxies around each other or around a common center of mass
such as the deep potential well of a cluster of galaxies. The largest
extragalactic physical velocities seen in the nearby universe are found for
galaxies orbiting in clusters of galaxies (~1500 km/s or z = 0.005),
kinematics in the central regions of quasars and active galactic nuclei
(~10,000 km/s or = 0.035, and our Galaxy's motion with respect to the
Cosmic Microwave Background reference frame (~630 km/s, z = 0.002)

Outside the nearby Universe, redshifts or apparent radial velocities
are dominated
by the cosmological expansion. This expansion is properly described
as the stretching of the metric or yardstick. In the standard
mathematical description of cosmology, the Friedmann-Lemaitre model,
distances are defined in terms of the Robertson-Walker metric, which is
the most general mathematical description for a uniform, homogeneous
space that is expanding or contracting:

$\begin{array}{cc}\phantom{\rule{6.0em}{0ex}}& d{s}^{2}={c}^{2}d{t}^{2}+{R}^{2}\left(t\right)[\genfrac{}{}{0.1ex}{}{d{r}^{2}}{(1-k{r}^{2})}+{r}^{2}si{n}^{2}\theta d{\varphi}^{2}]\hfill \end{array}$

for spherical coordinates r, θ, φ, and time coordinate ct.
R(t) is the scale factor, a function of time that is specified by
the laws of gravity, and k is the curvature constant, being
-1, 1, or 0 for an open, closed, or flat space geometry.

In an expanding universe, the cosmological redshift of an object
is directly related to its distance.
The Proper Distance to an object is the integral of the
scale factor over the metric:

$\begin{array}{cc}\phantom{\rule{6.0em}{0ex}}& {D}_{P}=R\left(t\right){\displaystyle \underset{0}{\overset{{r}_{1}}{\int}}}\genfrac{}{}{0.1ex}{}{d{r}_{1}}{\sqrt{1-k{r}_{1}^{2}}}=\genfrac{}{}{0.1ex}{}{R\left(t\right)}{\dot{R}\left(t\right)}cz\hfill \end{array}$

which reduces to the standard redshift-distance relation

$\begin{array}{cc}\phantom{\rule{6.0em}{0ex}}& {D}_{P}=\genfrac{}{}{0.1ex}{}{cz}{{H}_{0}}\hfill \end{array}$
where

$\begin{array}{cc}\phantom{\rule{6.0em}{0ex}}& {H}_{0}=\genfrac{}{}{0.1ex}{}{\dot{R}\left(t\right)}{R\left(t\right)}\hfill \end{array}$

is the Hubble Constant, named for the discoverer of the
expansion of the Universe. The form of this equation is the reason
that redshift is often quoted as apparent radial velocity, cz.
Note that there is no special relativistic 1/(1+ v^{2}/c^{2})
correction applied – apparent radial velocity is just cz.

There are also several other definitions of distance based on
physical properties of objects, including luminosity distance
and angular diameter distance. These are also described in any specific
cosmological model in terms of the redshift and the scale factor R(t),
and can be found in most textbooks on mathematical cosmology.

The first significant extragalactic redshift was that of the Andromeda galaxy
(M31) measured by Vesto Slipher in 1912. Edwin Hubble discovered the empirical
linear correlation between redshift and distance for nearby galaxies in the
late 1920s,
although we now know that Hubble's original redshift-distance relation, 600
kilometers per second per Megaparsec, was nearly a factor of ten too steep
– today's value lies near ~70 km/s/Mpc.

Redshifts are determined spectroscopically by measuring the shift of spectral
features of known wavelength and frequency. This is usually done by
measuring individual lines such as the 21-cm emission line of
neutral hydrogen in the radio, or the strong absorption features found in
the atmospheres of cool giant stars
that dominate the optical spectrum of most galaxies, or by cross-correlating
the galaxy spectrum with a template spectrum of a similar star or galaxy at
known redshift. It is also possible to "estimate" the redshift of a galaxy
from its overall spectral energy distribution if its morphological type
is known. These "photometric" redshifts are substantially less accurate
than spectroscopic redshifts, but may be sufficient for the scientific problem
at hand.