Free coursewareRewritten from MIT OpenCourseWareCC BY-NC-SA 4.0
Open CosmologyPhysics & cosmology: four years, plus a graduate year

Cosmological redshift

Light stretches with the universe — the redshift of a distant galaxy tells you how much the universe has expanded since the light left it.

You need this first

Full reading path (6 pages)
  1. Vectors (8.01)
  2. Position and velocity in one dimension (8.01)
  3. Acceleration in one dimension (8.01)
  4. Motion in two dimensions and projectiles (8.01)
  5. The homogeneous expanding universe (8.286)
  6. The Doppler effect and special relativity (8.286)
On this page · 4 sections
  1. Clocks and coordinates, again
  2. Deriving the redshift
  3. How this relates to the Doppler shift
  4. Summary

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 ℓp(t)=a(t) ℓc\ell_p(t) = a(t)\,\ell_c. 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 ℓc\ell_c. Think of each crest of the light wave as a separate pulse travelling toward us. In comoving coordinates every pulse moves at

Coordinate speed of light
dxdt=ca(t)\frac{dx}{dt} = \frac{c}{a(t)}
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 Δx\Delta x between them never changes. Their physical separation, which is the wavelength, is a(t) Δxa(t)\,\Delta x, so it grows in step with the universe:

Wavelength follows the scale factor
λ(t)∝a(t)\lambda(t) \propto a(t)
In words

lambda (t) is proportional to a(t)

The time between crests is Δt=λ/c\Delta t = \lambda/c, so periods stretch in the same way, and the redshift is simply

Cosmological redshift
1+z=ΔtOΔtS=λOλS=a(tO)a(tS)1 + z = \frac{\Delta t_O}{\Delta t_S} = \frac{\lambda_O}{\lambda_S} = \frac{a(t_O)}{a(t_S)}
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 tSt_S is when the light left the source and tOt_O when we observe it. The redshift tells you directly how much the universe has expanded while the light was on its way.

The same light wave at emission and when received, computed for redshift z. The universe has grown by a factor 1 + z in between, and so has every wavelength.
Worked example

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

1+z=364.8/121.6=3.01 + z = 364.8/121.6 = 3.0, so z=2.0z = 2.0.

Expansion

a(tO)/a(tS)=1+z=3a(t_O)/a(t_S) = 1 + z = 3. 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 z=3z = 3 it would arrive as blue light at 486 nm.

What this does not say

It does not say how long ago that was. Turning zz into a time needs a(t)a(t), 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 cc as measured locally. Gravity does not change either fact, so the formula holds with gravity included. Gravity is hidden in a(t)a(t), 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 zz as a function of a velocity measured in one inertial frame. The cosmological formula gives zz 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 a(t)a(t) grows linearly; choosing t=0t = 0 at the moment when a=0a = 0 gives a∝ta \propto t. Guth announces an extra-credit problem to show that in that case 1+z=a(tO)/a(tS)1 + z = a(t_O)/a(t_S) reproduces the relativistic Doppler formula exactly.

Summary#

  • Comoving galaxies and cosmic time give a common description for every observer.
  • Light's coordinate speed c/a(t)c/a(t) is the same everywhere at a given time, so crests keep a fixed coordinate separation and wavelengths grow in proportion to a(t)a(t).
  • 1+z=a(tO)/a(tS)1 + z = a(t_O)/a(t_S): redshift measures how much the universe expanded while the light travelled.
  • The result includes gravity (through a(t)a(t)) and reduces to the special-relativity Doppler shift when there is no gravity.

Symbols on this page

Show the 11 symbols used here
Δ\Delta capital delta
A change or difference in a quantity, e.g. Δx = x₂ − x₁. Say it: “capital delta”.
λ\lambda lambda
Wavelength. Say it: “lambda”.
ℓ\ell script l
A length or distance; ℓ_p is a physical distance and ℓ_c a comoving one. Say it: “ell”.
≈\approx approximately equal
Is approximately equal to. Say it: “is approximately”.
∝\propto proportional to
Is proportional to: doubling one doubles the other. Say it: “is proportional to”.
aa a
The scale factor a(t): how much the universe has expanded. Physical distance = a × comoving distance (Guth's units: metres per notch). Say it: “a”.
zz z
Redshift: 1 + z = a(observed)/a(emitted), how much the universe has stretched since the light left. Say it: “z”.
GG G
Newton's gravitational constant, G ≈ 6.674 × 10⁻¹¹ m³ kg⁻¹ s⁻². Say it: “G”.
cc c
The speed of light, c ≈ 2.998 × 10⁸ m/s. Say it: “c”.
ℓp\ell_{p} physical distance
A physical (proper) distance: what a ruler would measure at one moment, ℓ_p = a(t) ℓ_c. Say it: “ell p”.
ℓc\ell_{c} comoving distance
A comoving distance: fixed as the universe expands, measured in coordinate units (Guth's notches). Say it: “ell c”.

Tap or click a symbol in a formula to see the same explanation. All symbols: symbols and notation.

Where this leads

Pages that build on this

Check your understanding

  1. Light from a galaxy has redshift z=2z = 2. How much larger is the universe now than when the light was emitted?
  2. Why does the wavelength of light grow in proportion to a(t)a(t)?
  3. Where is gravity hidden in the cosmological redshift formula?
  4. In a universe that is contracting, light from distant galaxies would be…
0 of 4 answered

Flashcards

1 / 3