On the Doppler page redshift came from motion through space. In an expanding universe there is a simpler and more general way to see it: the light stretches along with the universe. This is the last piece of the kinematics of homogeneous expansion, and the first thing Guth does in Lecture 5.
Clocks and coordinates, again#
From the previous lecture, every galaxy has fixed comoving coordinates, and physical distances are . In the idealised model all matter is at rest in these coordinates (real galaxies also have small "peculiar" motions).
Time is measured by cosmic time: clocks at rest relative to the local matter, synchronised by something everyone in the universe can see. Guth's example: agree to set every clock to midnight when the cosmic microwave background has cooled to a chosen temperature. Because the universe is homogeneous, every observer sees the same history, so clocks synchronised once stay synchronised. Any quantity that changes with time and is the same everywhere would do, such as the value of the Hubble rate.
Cosmic time is an idealisation. Near a lump of matter clocks run differently — near the Sun by about one part in a million, near a giant black hole by much more — but for the universe on large scales it works.
Deriving the redshift#
Put us at the origin and a galaxy at comoving distance . Think of each crest of the light wave as a separate pulse travelling toward us. In comoving coordinates every pulse moves at
In words
dx over dt equals c over a(t)
This speed depends on time but not on position — that is homogeneity. So two successive crests always move at exactly the same coordinate speed at the same moment, and the coordinate distance between them never changes. Their physical separation, which is the wavelength, is , so it grows in step with the universe:
In words
lambda (t) is proportional to a(t)
The time between crests is , so periods stretch in the same way, and the redshift is simply
In words
1 plus z equals capital delta t sub O over capital delta t sub S equals lambda sub O over lambda sub S equals a(t sub O ) over a(t sub S )
Here is when the light left the source and when we observe it. The redshift tells you directly how much the universe has expanded while the light was on its way.
Reading the expansion from a spectrum
The hydrogen Lyman-alpha line is emitted at 121.6 nm. In a distant quasar it is observed at 364.8 nm. What is the redshift, and how much has the universe expanded since the light left?
Redshift
, so .
Expansion
. When the light set out, every distance between galaxies was one third of what it is today. Far-ultraviolet light has been stretched into the near-ultraviolet, just short of visible light (which starts around 380–400 nm); at it would arrive as blue light at 486 nm.
What this does not say
It does not say how long ago that was. Turning into a time needs , which depends on gravity and the contents of the universe — the subject of the next pages.
How this relates to the Doppler shift#
Two differences matter.
It is more general. The derivation used only two facts: the scale factor converts metres to coordinates, and light always moves at as measured locally. Gravity does not change either fact, so the formula holds with gravity included. Gravity is hidden in , whose evolution it controls. No time-dilation factor appears, because both clocks — at the galaxy and here — are at rest relative to their local matter and read cosmic time.
It uses different variables. The special-relativity formula gives as a function of a velocity measured in one inertial frame. The cosmological formula gives in terms of the scale factor at two times. In a real universe with gravity there is no single inertial frame covering both galaxies, so "the velocity" of a distant galaxy is not well defined in the special-relativity sense.
The two must agree when there is no gravity. Then nothing decelerates the expansion, velocities stay constant and grows linearly; choosing at the moment when gives . Guth announces an extra-credit problem to show that in that case reproduces the relativistic Doppler formula exactly.
Summary#
- Comoving galaxies and cosmic time give a common description for every observer.
- Light's coordinate speed is the same everywhere at a given time, so crests keep a fixed coordinate separation and wavelengths grow in proportion to .
- : redshift measures how much the universe expanded while the light travelled.
- The result includes gravity (through ) and reduces to the special-relativity Doppler shift when there is no gravity.