Cosmology
Hubble's Law
The farther a galaxy, the faster it recedes — the fingerprint of an expanding universe
Hubble's Law is the observed proportionality between how far a galaxy is and how fast it appears to be moving away from us: recession velocity equals the Hubble constant times distance, v = H₀d. Edwin Hubble published it in 1929 from Cepheid distances and Vesto Slipher's redshifts, two years after Georges Lemaître derived the same relation from general relativity. Because a galaxy twice as distant recedes twice as fast, the pattern has no centre — it is the unmistakable signature that space itself is expanding, stretching light toward the red. The slope, H₀, is the present expansion rate, measured today as roughly 67–73 km/s/Mpc, and its inverse — the Hubble time — is about 14 billion years. In 2018 the IAU recommended renaming it the Hubble–Lemaître law.
- Governing relationv = H₀d
- Hubble constant H₀~67–73 km/s/Mpc
- Discovered / predictedHubble 1929; Lemaître 1927
- Hubble time 1/H₀~14 billion years
- Low-z redshift linkv ≈ cz
- MeaningUniverse is expanding uniformly
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Why Hubble's Law matters
- It launched observational cosmology. Before 1929 the universe was widely thought static and possibly no bigger than the Milky Way. A linear v–d relation across dozens of galaxies made the cosmos dynamic, vast, and evolving.
- It is the empirical backbone of the Big Bang. Run the expansion backwards and everything converges — the same extrapolation that predicts the cosmic microwave background and the light-element abundances.
- H₀ sets the cosmic clock and yardstick. The Hubble time 1/H₀ frames the age of the universe, and H₀ converts any galaxy's redshift into a distance — the workhorse of galaxy surveys.
- Its slope is a battleground. The 5-sigma disagreement between early- and late-universe values of H₀ — the Hubble tension — may be the loudest hint of new physics beyond ΛCDM.
- It calibrates dark energy. Extending the velocity-distance relation to high redshift with Type Ia supernovae revealed, in 1998, that the expansion is accelerating.
The equation and its symbols
The law is deceptively simple:
v = H₀ d
- v — recession velocity, in km/s. The rate at which a galaxy moves away from us due to cosmic expansion (the peculiar velocity from local gravity must be subtracted).
- d — proper distance to the galaxy, usually in megaparsecs (1 Mpc = 3.086 × 10¹⁹ km ≈ 3.26 million light-years).
- H₀ — the Hubble constant, the present-day expansion rate, in km/s/Mpc. The subscript "0" denotes "now"; the more general time-varying quantity H(t) is the Hubble parameter.
For nearby galaxies the recession velocity connects to the measured redshift by v ≈ cz, where z = Δλ/λ is the fractional wavelength stretch and c is the speed of light. Combining the two gives the practical distance estimator d ≈ cz / H₀. Note the units: H₀ carries dimensions of inverse time, so its reciprocal is a time and its reciprocal-times-c is a length — the Hubble length, about 4,300 Mpc (14 billion light-years).
How it works, step by step
- Measure the redshift. A galaxy's spectrum shows familiar absorption lines — calcium H and K, hydrogen Balmer lines — shifted to longer wavelengths. The fractional shift z = Δλ/λ is read directly and precisely.
- Measure the distance independently. Redshift alone cannot give distance, so astronomers climb the cosmic distance ladder: parallax for nearby stars, Cepheid variables (whose period fixes their luminosity via the Leavitt law) in nearby galaxies, then Type Ia supernovae as standard candles out to hundreds of Mpc.
- Plot velocity against distance. When cz is plotted versus d, the points fall on a straight line through the origin. The slope is H₀.
- Interpret the line. A straight line through the origin means every observer, on every galaxy, sees the same law — the hallmark of homogeneous, isotropic expansion described by the Friedmann equations. There is no centre and no edge.
- Extrapolate in time. Uniform expansion implies a finite past: at t = 0 all separations vanish. The characteristic timescale is the Hubble time, 1/H₀ ≈ 14 Gyr, close to the true 13.8-Gyr age.
Key numbers and comparison
| Quantity / probe | Value | Note |
|---|---|---|
| Hubble's original 1929 slope | ~500 km/s/Mpc | Wrong by ~7× — his Cepheid calibration was off |
| Planck 2018 (CMB, early universe) | 67.4 ± 0.5 km/s/Mpc | ΛCDM fit to the microwave background |
| SH0ES (Cepheids + Type Ia SNe) | 73.0 ± 1.0 km/s/Mpc | Late-universe distance ladder |
| Hubble time 1/H₀ (H₀ = 70) | ~14 billion years | Ballpark for the age of the universe |
| Hubble length c/H₀ (H₀ = 70) | ~4,300 Mpc ≈ 14 Gly | Rough size of the observable horizon scale |
| Recession of a galaxy at 100 Mpc | ~7,000 km/s (H₀ = 70) | Corresponds to z ≈ 0.023 |
A worked example and the history
Take the Coma cluster, roughly 100 Mpc away with a mean redshift z ≈ 0.023. Its recession velocity is v ≈ cz = 300,000 km/s × 0.023 ≈ 6,900 km/s. Dividing by distance gives H₀ ≈ 6,900 / 100 = 69 km/s/Mpc — squarely inside the modern range. Reverse the arithmetic and you have the standard way distances are estimated: a quasar at z = 0.1 sits roughly at d ≈ cz/H₀ ≈ 30,000/70 ≈ 430 Mpc.
Historically, the story runs Slipher → Lemaître → Hubble. Vesto Slipher measured the first galaxy redshifts at Lowell Observatory starting in 1912, finding most "spiral nebulae" fleeing at hundreds of km/s. In 1927 Georges Lemaître, a Belgian priest and physicist, solved Einstein's equations for an expanding universe, combined them with Slipher's velocities and Hubble's early distances, and derived v = H₀d — even estimating a coefficient near 625 km/s/Mpc. His paper appeared in a little-read French journal. In 1929 Edwin Hubble, using mostly Slipher's redshifts (with a handful of new ones from his collaborator Milton Humason) and his own Cepheid distances from Mount Wilson's 100-inch telescope, published the relation with 24 galaxies and made it famous. The 1998 discovery of cosmic acceleration by the High-z Supernova Search and the Supernova Cosmology Project extended the very same velocity-distance diagram into the high-redshift regime, revealing dark energy.
Common misconceptions
- "Galaxies are flying through space away from us." No — space itself expands between galaxies. Cosmological redshift is stretched wavelength, not a Doppler shift through a static space.
- "We are at the centre of the expansion." There is no centre. Because v ∝ d, every observer sees the same recession law; the pattern is centreless, like dots on an inflating balloon.
- "Recession faster than light is impossible." Beyond the Hubble distance, galaxies recede faster than c. This is allowed — no object moves through space faster than light; it is space growing.
- "The Hubble constant is truly constant." It is constant in space (same everywhere now) but not in time. H(t) was much larger in the past; "H₀" means its value today.
- "1/H₀ is exactly the age of the universe." Only in an empty, coasting universe. Deceleration then acceleration make the true age (13.8 Gyr) differ slightly from the Hubble time.
- "The law holds at all distances." The clean linear v = H₀d applies only nearby (low z). At high z, curvature of the expansion history and the breakdown of v = cz require the full Friedmann framework.
Frequently asked questions
What is Hubble's Law in simple terms?
Hubble's Law says the farther a galaxy is, the faster it appears to move away from us, and the relationship is a straight line: recession velocity v = H₀ × distance d. A galaxy twice as far recedes twice as fast. This is not galaxies flying through space away from a center — it is space itself expanding between galaxies, stretching the light we receive to longer (redder) wavelengths.
What is the Hubble constant H₀?
H₀ is the present-day expansion rate of the universe — the slope of the velocity-distance line. It is measured in kilometres per second per megaparsec (km/s/Mpc). Current estimates cluster around 67–73 km/s/Mpc: the Planck CMB value is 67.4 ± 0.5, while the SH0ES Cepheid + Type Ia supernova value is about 73.0 ± 1.0. A galaxy 100 Mpc away therefore recedes at roughly 7,000 km/s.
Did Hubble or Lemaître discover Hubble's Law?
Both. Georges Lemaître derived the velocity-distance relation in 1927 from Einstein's general relativity and even estimated the constant, but published in an obscure French-language journal. Edwin Hubble independently published the observational relation in 1929 using Cepheid distances and Vesto Slipher's redshifts. In 2018 the International Astronomical Union recommended calling it the Hubble–Lemaître law to credit both.
How does Hubble's Law prove the universe is expanding?
If every galaxy recedes with a speed proportional to its distance, the pattern looks the same from every galaxy — there is no special centre. That is exactly the signature of uniform expansion: a grid where every gap stretches at the same fractional rate. Run it backwards and everything converges to a hot, dense start — the Big Bang. No steady, static universe reproduces a linear v = H₀d relation across billions of light-years.
What is the difference between redshift and recession velocity?
Redshift z is what we actually measure — the fractional stretch of a spectral line, z = Δλ/λ. For nearby galaxies the recession velocity is simply v ≈ cz. But at large z this breaks down: cosmological redshift is space stretching, not a Doppler shift, and distant galaxies can have apparent recession speeds greater than c without violating relativity. The clean v = H₀d law holds only in the nearby, low-redshift universe.
Why do different measurements of the Hubble constant disagree?
This is the Hubble tension. The early-universe route — fitting the cosmic microwave background with the ΛCDM model — gives H₀ ≈ 67.4 km/s/Mpc. The late-universe route — the cosmic distance ladder of Cepheids and Type Ia supernovae — gives H₀ ≈ 73 km/s/Mpc. The gap is now about 5 sigma, too large to be chance. Either there is an unknown systematic error or new physics beyond the standard model.
What is the Hubble time and is it the age of the universe?
The Hubble time is 1/H₀ ≈ 14 billion years for H₀ ≈ 70 km/s/Mpc. It is the age the universe would have if it had always expanded at today's rate. The true age is 13.8 billion years — close, but not identical, because the expansion rate has changed: gravity slowed it early on, and dark energy has accelerated it for the last ~5 billion years. The two effects nearly cancel, which is why 1/H₀ is a good ballpark.