Cosmology: The Expanding Universe, Big Bang & Dark Sector

Turn an old analogue television to a dead channel and a few per cent of the snow hissing across the screen is not from any station on Earth. It is the faint, uniform glow of the whole sky at a temperature of about 2.72.7 kelvin — the cooled-down afterlight of the hot, dense beginning we call the Big Bang. That radiation has been travelling, unblocked, for over thirteen billion years, and it arrives from every direction at once. How did we come to read a story that large from so faint a hiss? It began not with the glow but with a straight line. In 1929 Edwin Hubble, measuring the light of distant galaxies at Mount Wilson, found that almost every galaxy is moving away from us, and — the crucial part — the farther one lies, the faster it flees. Speed rises in simple proportion to distance: v=H0dv = H_0 d. Run that outward rush backwards in your mind and every galaxy converges, the whole universe collapses to a single blazing point, and you arrive at a beginning in time. This article follows that reasoning with nothing beyond school algebra. We will see why the galaxies' redshift means space itself is stretching (not galaxies flying through space from some centre), how the single number H0H_0 hands us both the recession speed of any galaxy and a rough age of the universe of about 1414 billion years, why the 2.7 K2.7\ \text{K} microwave background is the smoking gun of a hot origin, and why the ordinary matter of stars and planets is a mere 5%5\% of the cosmos — the other 95%95\% a dark sector of dark matter and dark energy we can weigh but cannot yet see.

Key takeaways
  • The universe is expanding. Distant galaxies recede from us, and their speed grows in direct proportion to distance — Hubble's law, v=H0dv = H_0 d, with H0≈70 km/s per MpcH_0 \approx 70\ \text{km/s per Mpc}.
  • The recession is space stretching, not motion through space. The observed cosmological redshift (z=Δλ/λ0≈v/cz = \Delta\lambda/\lambda_0 \approx v/c for small vv) comes from wavelengths being stretched along with space itself. There is no centre and no edge.
  • One number gives the age. Because speed equals distance over time, the reciprocal 1/H01/H_0 is a rough age of the universe, about 1414 billion years (the precise measured value is 13.813.8 Gyr).
  • Run it backwards and you get the Big Bang. A hot, dense early state that has been expanding and cooling ever since — not an explosion in space but an expansion of space.
  • Three independent proofs agree. The redshift–distance law, the 2.7 K2.7\ \text{K} cosmic microwave background (the relic heat), and the cosmic abundance of light elements (about a quarter helium by mass) all point to the same hot origin.
  • Most of the universe is dark. Ordinary matter is only about 5%5\%; the rest is 27%27\% dark matter (felt through gravity) and 68%68\% dark energy (driving an accelerating expansion) — together 100%100\%.
  • Key idea: galaxies recede at speeds proportional to their distance because space itself stretches (v = H₀d), so running the expansion backwards gives a hot dense Big Bang whose relic glow is the 2.7 K microwave background, and today's cosmos is only 5% ordinary matter, the rest a dark sector of 27% dark matter and 68% dark energy.
The core insight

Every distant galaxy recedes at a speed proportional to its distance, v=H0dv = H_0 d, because space itself is expanding and stretching the wavelengths of light (the cosmological redshift); reversing that expansion gives a hot, dense Big Bang whose relic radiation survives as the 2.7 K2.7\ \text{K} cosmic microwave background, the reciprocal 1/H0≈141/H_0 \approx 14 billion years fixes the age, and the present universe is only 5%5\% ordinary matter, 27%27\% dark matter and 68%68\% dark energy.

Where this lives today

Cosmology has become a precision science. Satellites — COBE, WMAP and Planck — have mapped the 2.7 K2.7\ \text{K} microwave background across the whole sky and measured its tiny temperature ripples (one part in a hundred thousand), the seeds from which galaxies later grew. From those maps the composition 5%/27%/68%5\%/27\%/68\% and the age 13.8 Gyr13.8\ \text{Gyr} are pinned down to a per cent or two. Yet the two biggest ingredients remain mysteries: laboratory experiments deep underground hunt for dark-matter particles, while surveys of millions of galaxies probe whether dark energy is truly the unchanging energy of empty space or something that evolves. There is even a live puzzle called the "Hubble tension" — the value of H0H_0 measured from nearby galaxies (≈73\approx 73) disagrees slightly but stubbornly with the value inferred from the microwave background (≈67\approx 67), and no one yet knows whether it signals new physics or a hidden error. The expanding universe Hubble sketched with a single straight line in 1929 is still being redrawn. To go further — from the algebraic Hubble law to the full curved-spacetime account of an expanding cosmos — the next step is general relativity, named in the seam below.

The physical picture

Start with what we actually see. Point a telescope with a spectrograph at a distant galaxy and spread its light into a spectrum. The dark absorption lines of hydrogen, calcium and other elements are there — the same fingerprints we measure in a laboratory flame — but every one of them sits at a longer wavelength than it should. The whole pattern is shifted toward the red end of the spectrum. This is a redshift, and Hubble's revelation was that nearly every galaxy shows one, and that the shift grows with distance. The naive reading is that galaxies are simply flying away from us through space, like shrapnel from a bomb. That picture is wrong in an important way, and getting it right is the heart of cosmology. The galaxies are (mostly) not moving through space at all. Rather, space itself is expanding, carrying the galaxies along with it and stretching the wavelength of any light in transit. A photon emitted long ago as blue light rides an expanding fabric; by the time it reaches us its wavelength has been stretched into the red. The redshift is therefore not a Doppler shift of an object rushing past — it is a cosmological redshift, the imprint of how much the universe has grown while the light was in flight. The essential consequence is that there is no centre. Picture a loaf of raisin bread rising in the oven. As the dough swells, every raisin moves away from every other raisin, and any raisin you choose to sit on sees all the others receding — the more distant ones faster, because there is more expanding dough between you and them. No raisin is the centre; the expansion happens everywhere at once. Our galaxy is not special: an astronomer in any galaxy sees exactly the same law of recession. The Big Bang did not happen at a point in space that we could fly back to; it happened everywhere, because everywhere was compressed together.

Figure
A grid of galaxies at an early time and a later expanded time, with every galaxy moving away from every other and the recession arrows longer for galaxies farther apart, showing that the expansion has no centre and looks the same from any galaxy
Space itself expands — every galaxy recedes from every other, no centre early universe (compact) any observer time later universe (stretched) farther galaxies recede faster The grid stretches; galaxies ride along. Every observer sees the same recession law. The galaxies barely move through the grid — the grid itself grows. This is why there is no centre and no edge. A blue photon emitted early arrives redshifted, its wavelength stretched by the same factor as space.

Hubble's law: speed proportional to distance

Hubble's measurement can be stated in one line. For every galaxy far enough away that the general expansion dominates its own local wandering, the recession speed vv is directly proportional to its distance dd:

v=H0 d.(1)v = H_0\, d. \qquad (1)

where: vv is the recession speed (km/s), dd is the galaxy's distance (megaparsecs, Mpc, where 1 Mpc=3.086×1022 m≈3.261\ \text{Mpc} = 3.086\times10^{22}\ \text{m} \approx 3.26 million light-years), and H0H_0 is the Hubble constant, the slope of the line, with the currently accepted value H0≈70 km/s per MpcH_0 \approx 70\ \text{km/s per Mpc}. The physical reading is that the constant of proportionality is the same for every galaxy in the sky — a straight line through the origin on a plot of speed against distance. A galaxy at d=100 Mpcd = 100\ \text{Mpc} recedes at v=70×100=7000 km/sv = 70 \times 100 = 7000\ \text{km/s}; one twice as far recedes twice as fast. The subscript zero on H0H_0 is a reminder that it is the present-day value of a quantity that has changed over cosmic history — the expansion rate was different in the past. This linear law is exactly what a uniform expansion must produce, and it is what makes the "no centre" claim precise rather than poetic. If the whole fabric of space swells by the same factor everywhere, then a galaxy twice as far has twice as much stretching fabric between us and it, and so recedes twice as fast. We will show in the second derivation below that an observer in any galaxy measures the very same law with the very same H0H_0 — proof that our position is in no way central.

Figure
A Hubble diagram plotting recession speed on the vertical axis against distance on the horizontal axis, with data points scattered along a straight line through the origin whose slope is the Hubble constant, and a marked point at distance 100 megaparsecs and speed 7000 kilometres per second
The Hubble diagram — speed rises in step with distance, slope H₀ distance d (Mpc) recession speed v (km/s) 50 100 150 200 3500 7000 10500 14000 v = H₀ d 100 Mpc, 7000 km/s slope = H₀ ≈ 70 km/s per Mpc

Cosmological redshift: how much space has stretched

We measure a galaxy's redshift, not its speed, so we need the link between them. The redshift zz is defined as the fractional change in wavelength — how much longer the received wavelength λobs\lambda_{\text{obs}} is than the emitted (rest) wavelength λ0\lambda_0:

z=λobs−λ0λ0=Δλλ0≈vc(v≪c).(2)z = \frac{\lambda_{\text{obs}} - \lambda_0}{\lambda_0} = \frac{\Delta\lambda}{\lambda_0} \approx \frac{v}{c} \quad (v \ll c). \qquad (2)

where: λ0\lambda_0 is the wavelength the line would have in a laboratory, λobs\lambda_{\text{obs}} is what we receive, zz is dimensionless, vv is the recession speed and c=3.0×108 m/sc = 3.0\times10^8\ \text{m/s}. The physical reading: for nearby galaxies (small vv) the redshift is just the recession speed as a fraction of light speed, so a galaxy fleeing at 7000 km/s7000\ \text{km/s} has z=7000/300,000=0.023z = 7000 / 300{,}000 = 0.023 — every wavelength arrives 2.3%2.3\% longer than emitted. Deeper still, zz measures how much space has grown since the light was emitted: at z=1z = 1 the universe has doubled in size since that photon set out. The approximation z≈v/cz \approx v/c is a first step only; once vv approaches an appreciable fraction of cc (roughly z≳0.1z \gtrsim 0.1) the simple proportionality breaks down and the full relativistic relation is needed — the exact treatment of redshift in a curved, expanding spacetime belongs to general relativity and is named at the end, not derived here.

The age of the universe

Hubble's law hides a clock. If every galaxy has been receding at a steady speed vv since the beginning and now sits at distance dd, then the time it took to get there is simply distance over speed, t=d/vt = d/v. But Hubble's law says v=H0dv = H_0 d, so the distance cancels and every galaxy gives the same time:

t≈dv=dH0d=1H0.(3)t \approx \frac{d}{v} = \frac{d}{H_0 d} = \frac{1}{H_0}. \qquad (3)

where: 1/H01/H_0 is the Hubble time, the reciprocal of the Hubble constant. The physical reading is striking: because the distance cancels, all galaxies point back to a single moment of common origin — a beginning. Putting in H0=70 km/s per MpcH_0 = 70\ \text{km/s per Mpc} gives (worked in full in the first derivation) about 1414 billion years. This is an estimate: it assumes a constant expansion rate, whereas gravity slowed the early expansion and dark energy is speeding up the recent one. The two corrections happen to nearly cancel, so the honest Hubble-time estimate of 14 Gyr14\ \text{Gyr} lands remarkably close to the precisely measured age of 13.8 Gyr13.8\ \text{Gyr}. The exact expansion history follows from the Friedmann equations of general relativity — differential equations solved with calculus that lie in the university seam named at the end; here we use only the algebraic Hubble law.

Derivation AThe age of the universe from the Hubble constant

The goal is to turn the single measured number H0=70 km/s per MpcH_0 = 70\ \text{km/s per Mpc} into an age in years, using only unit conversion and one reciprocal — no calculus, no cosmological model beyond "the expansion has been roughly steady." The subtlety that trips students is that H0H_0 is quoted in mixed units (kilometres, seconds and megaparsecs all at once), so the first job is to render it in pure inverse seconds; then 1/H01/H_0 is a time, which we convert to years.

Step 1. Strip H0H_0 to SI. The speed part is 70 km/s=70×103 m/s70\ \text{km/s} = 70\times10^{3}\ \text{m/s}, and the distance part is 1 Mpc=3.086×1022 m1\ \text{Mpc} = 3.086\times10^{22}\ \text{m}. Dividing, H0=70×103 m/s3.086×1022 m=2.27×10−18 s−1H_0 = \dfrac{70\times10^{3}\ \text{m/s}}{3.086\times10^{22}\ \text{m}} = 2.27\times10^{-18}\ \text{s}^{-1}. Notice the metres cancel and we are left with a pure rate, one over seconds — an expansion rate.

Step 2. Take the reciprocal to get the Hubble time. t=1H0=12.27×10−18 s−1=4.41×1017 st = \dfrac{1}{H_0} = \dfrac{1}{2.27\times10^{-18}\ \text{s}^{-1}} = 4.41\times10^{17}\ \text{s}. That is the age in seconds — a number too large to feel.

Step 3. Convert seconds to years using 1 yr=3.156×107 s1\ \text{yr} = 3.156\times10^{7}\ \text{s}. t=4.41×1017 s3.156×107 s/yr=1.40×1010 yr≈14 billion yearst = \dfrac{4.41\times10^{17}\ \text{s}}{3.156\times10^{7}\ \text{s/yr}} = 1.40\times10^{10}\ \text{yr} \approx 14\ \text{billion years}.

Step 4. Sanity-check against the real value. The measured age of the universe from the cosmic microwave background is 13.8 Gyr13.8\ \text{Gyr} — within 2%2\% of our crude 1/H01/H_0. The near-miss is not luck we should trust too far: the assumption of constant expansion is wrong in detail (early deceleration by gravity, late acceleration by dark energy), but those errors happen to nearly cancel for the real universe. The same arithmetic also gives the size of the observable universe: light travelling for a Hubble time covers a Hubble length c/H0=c t≈(3.0×108)(4.41×1017)=1.32×1026 mc/H_0 = c\,t \approx (3.0\times10^{8})(4.41\times10^{17}) = 1.32\times10^{26}\ \text{m}, about 1414 billion light-years. Verified: H0=2.27×10−18 s−1H_0 = 2.27\times10^{-18}\ \text{s}^{-1}, 1/H0=4.41×1017 s=14.0 Gyr1/H_0 = 4.41\times10^{17}\ \text{s} = 14.0\ \text{Gyr}, and c/H0=1.32×1026 mc/H_0 = 1.32\times10^{26}\ \text{m} — recomputed in verify_hs2-cosmology-big-bang.py.

Go deeper · Derivation B · 1 minWhy the expansion has no centre
Derivation BWhy the expansion has no centre

The goal is to prove, with vector algebra a student already owns, that Hubble's law looks identical from every galaxy — so no galaxy is the centre of the expansion. We take Hubble's law as an observed fact from our own vantage point and simply change viewpoints, using the ordinary rule that relative velocity is the difference of two velocities. No calculus, no relativity: just subtraction of vectors.

Step 1. State the law from our galaxy A. Every other galaxy at position vector r⃗\vec{r} (measured from A) recedes with velocity v⃗=H0 r⃗\vec{v} = H_0\,\vec{r}. This is Hubble's law written as vectors: the velocity points straight out along r⃗\vec{r} and its size grows with distance.

Step 2. Pick a second galaxy B at position r⃗B\vec{r}_B, receding from us at v⃗B=H0 r⃗B\vec{v}_B = H_0\,\vec{r}_B. Now stand on B and ask how a third galaxy C (at r⃗C\vec{r}_C from us) appears. Its position relative to B is r⃗C−r⃗B\vec{r}_C - \vec{r}_B, and its velocity relative to B is v⃗C−v⃗B\vec{v}_C - \vec{v}_B.

Step 3. Substitute Hubble's law for both. The relative velocity is v⃗C−v⃗B=H0r⃗C−H0r⃗B=H0(r⃗C−r⃗B)\vec{v}_C - \vec{v}_B = H_0\vec{r}_C - H_0\vec{r}_B = H_0(\vec{r}_C - \vec{r}_B). But r⃗C−r⃗B\vec{r}_C - \vec{r}_B is exactly the position of C as seen from B. So an observer on B sees C receding with v⃗rel=H0(r⃗C−r⃗B)\vec{v}_{\text{rel}} = H_0(\vec{r}_C - \vec{r}_B) — the same Hubble's law, with the same H0H_0.

Step 4. Read the result. Every galaxy sees every other galaxy obeying v=H0dv = H_0 d with the identical constant. There is no special observer and no centre: the linear velocity field v⃗=H0r⃗\vec{v} = H_0\vec{r} is the unique field that looks the same from all of its own points. This is the algebraic backbone of the raisin-bread picture, and it is why the Big Bang has no location "out there" to point at. Verified: with v⃗=H0r⃗\vec{v} = H_0\vec{r}, the relative velocity v⃗C−v⃗B=H0(r⃗C−r⃗B)\vec{v}_C - \vec{v}_B = H_0(\vec{r}_C - \vec{r}_B) is checked numerically for sample galaxy positions in verify_hs2-cosmology-big-bang.py.

The Big Bang and its three proofs

Rewind the expansion and everything grows hotter and denser. Squeeze all of today's galaxies back together and the universe becomes a searing, uniform plasma; push far enough and ordinary structures cannot survive at all. That hot, dense early state, expanding and cooling ever since, is the Big Bang model. It is emphatically not an explosion of matter into a pre-existing empty space — it is the expansion of space, happening everywhere, that we have already met. Three independent lines of evidence, using entirely different physics, converge on it.

Proof one — the redshift–distance law itself. The universal recession, v=H0dv = H_0 d, is exactly what a uniformly expanding universe predicts, and running it backwards demands a beginning. This is the evidence Hubble supplied.

Proof two — the cosmic microwave background. If the universe began hot, its early radiation should still be here, stretched by the expansion into long wavelengths and cooled to just a few degrees above absolute zero. In 1965 Penzias and Wilson found exactly this: a microwave hiss coming uniformly from every direction, a near-perfect thermal (black-body) glow at T=2.7 KT = 2.7\ \text{K}. Wien's law places the peak of a 2.7 K2.7\ \text{K} black body at λmax=b/T=(2.9×10−3)/2.7=1.1×10−3 m\lambda_{\text{max}} = b/T = (2.9\times10^{-3})/2.7 = 1.1\times10^{-3}\ \text{m}, about 1.1 mm1.1\ \text{mm} — squarely in the microwave band, which is why it is called the cosmic microwave background. It is the oldest light in existence, released when the cooling universe first turned transparent.

Proof three — the light elements. In its first few minutes the universe was hot enough for nuclear fusion, and the physics of that furnace predicts a definite recipe: roughly 75%75\% hydrogen and 25%25\% helium by mass, with a trace of deuterium and lithium and essentially nothing heavier. This is precisely the composition we measure in the most ancient, unprocessed gas. The heavier elements — carbon, oxygen, iron — came later, forged inside stars (the stellar-physics article, this article's prerequisite). The cosmic quarter-helium abundance is a fossil of the Big Bang's first three minutes.

The dark sector: what the universe is made of

Weigh the universe and a disturbing accounting emerges. The luminous matter — stars, gas, planets, everything built of protons and neutrons — makes up only about 5%5\% of the total. The rest is dark, and it comes in two utterly different kinds.

Dark matter, about 27%27\% of the total, betrays itself only through gravity. Spiral galaxies rotate far too fast at their edges: the visible stars supply nowhere near enough gravity to hold a galaxy spinning that quickly together — it should fly apart. The stars orbit as if embedded in a vast invisible halo of extra mass, several times the visible amount. The same excess gravity bends light (gravitational lensing) and shapes how galaxies cluster. Dark matter is not ordinary matter that is merely unlit; its total is far more than all the gas and dead stars combined, and it neither emits nor absorbs light. What it is — some new particle beyond the Standard Model — remains one of physics' great open questions.

Dark energy, about 68%68\% of the total, is stranger still. In 1998 two teams measuring distant supernovae found that the expansion is not slowing under gravity as expected but accelerating. Something with negative pressure — a property of empty space itself, in the simplest model — is pushing the expansion faster. We call it dark energy, and it now dominates the cosmic energy budget. Adding the three ingredients, 5%+27%+68%=100%5\% + 27\% + 68\% = 100\%: ordinary matter is a rounding error, and 95%95\% of the universe is a dark sector we can measure but not yet identify.

Figure
A pie chart of the energy content of the universe divided into three wedges, a small 5 per cent slice of ordinary matter, a 27 per cent slice of dark matter and a dominant 68 per cent slice of dark energy, summing to 100 per cent
What the universe is made of — 95 per cent is dark Ordinary matter — 5% stars, gas, planets, you Dark matter — 27% felt only by gravity; galaxy halos Dark energy — 68% drives the accelerating expansion 5 + 27 + 68 = 100 per cent

Limiting cases

caseresultmeaning
nearby galaxy, v≪cv \ll cz≈v/cz \approx v/c, and v=H0dv = H_0 dthe simple linear regime; redshift reads speed and distance
z≳0.1z \gtrsim 0.1 (fast recession)z≈v/cz \approx v/c fails; use the relativistic/GR relationfor large zz, redshift measures how much space grew, not a plain speed
take the reciprocal of H0H_0t=1/H0≈14 Gyrt = 1/H_0 \approx 14\ \text{Gyr}the Hubble time, a rough age of the universe
run the expansion backwardshot, dense Big Bangeverything converges; a beginning in time
a galaxy's local motion dominatesHubble's law appears violated (e.g. Andromeda is blueshifted, approaching)v=H0dv = H_0 d holds only on large scales, above local gravity
add up the energy budget5%+27%+68%=100%5\% + 27\% + 68\% = 100\%ordinary matter is a small minority; the dark sector rules

Worked examples

Board level — recession speed, redshift and stretched wavelength at 100 Mpc (IB-HL and A-Level pattern)

A galaxy lies at a distance d=100 Mpcd = 100\ \text{Mpc}. Take H0=70 km/s per MpcH_0 = 70\ \text{km/s per Mpc} and c=3.0×105 km/sc = 3.0\times10^{5}\ \text{km/s}. Find (a) its recession speed, (b) its redshift zz, and (c) the observed wavelength of a hydrogen line whose rest wavelength is 500.0 nm500.0\ \text{nm}.

Step 1. Recession speed from Hubble's law: v=H0d=70×100=7000 km/sv = H_0 d = 70 \times 100 = 7000\ \text{km/s}. That is 7.0×106 m/s7.0\times10^{6}\ \text{m/s}, about 2.3%2.3\% of the speed of light — small enough that the simple formulae apply.

Step 2. Redshift for small vv: z=v/c=7000/(3.0×105)=0.023z = v/c = 7000 / (3.0\times10^{5}) = 0.023. Every wavelength arrives 2.3%2.3\% longer than it left.

Step 3. Observed wavelength: λobs=λ0(1+z)=500.0×1.0233=511.7 nm\lambda_{\text{obs}} = \lambda_0(1 + z) = 500.0 \times 1.0233 = 511.7\ \text{nm}, a shift of Δλ=11.7 nm\Delta\lambda = 11.7\ \text{nm} toward the red. Answer: v=7000 km/sv = 7000\ \text{km/s}, z=0.023z = 0.023, and the 500.0 nm500.0\ \text{nm} line is seen at 511.7 nm511.7\ \text{nm}.

Competitive level — from a measured redshift back to distance and lookback time (IB-HL and A-Level pattern)

A quasar's spectral lines are redshifted by z=0.050z = 0.050. Using H0=70 km/s per MpcH_0 = 70\ \text{km/s per Mpc}, 1 Mpc=3.26×106 ly1\ \text{Mpc} = 3.26\times10^{6}\ \text{ly} and c=3.0×105 km/sc = 3.0\times10^{5}\ \text{km/s}, estimate (a) its recession speed, (b) its distance in Mpc and in light-years, and (c) roughly how long ago the light we now see set out.

Step 1. Speed from the redshift (small-zz regime): v=zc=0.050×(3.0×105)=15,000 km/sv = zc = 0.050 \times (3.0\times10^{5}) = 15{,}000\ \text{km/s}. This is 5%5\% of cc — near the upper edge where z≈v/cz \approx v/c is still trustworthy, so a quick check that we are allowed to use it matters.

Step 2. Distance from Hubble's law, inverted: d=v/H0=15,000/70=214 Mpcd = v/H_0 = 15{,}000 / 70 = 214\ \text{Mpc}. Convert to light-years: d=214×3.26×106=7.0×108 lyd = 214 \times 3.26\times10^{6} = 7.0\times10^{8}\ \text{ly}, about 700700 million light-years.

Step 3. Lookback time — how long the light has been travelling — is roughly distance over light speed: t≈d/c=(7.0×108 ly)/c=7.0×108 yrt \approx d/c = (7.0\times10^{8}\ \text{ly})/c = 7.0\times10^{8}\ \text{yr} (a light-year is, by definition, the distance light covers in a year, so distance in light-years equals travel time in years). Answer: v≈15,000 km/sv \approx 15{,}000\ \text{km/s}, d≈214 Mpc≈7.0×108 lyd \approx 214\ \text{Mpc} \approx 7.0\times10^{8}\ \text{ly}, and the light left about 700700 million years ago. Timing note: under two minutes. The chain is z→v=zc→d=v/H0→z \to v = zc \to d = v/H_0 \to light-years, and the lookback time is free once the distance is in light-years (they are numerically equal). The one trap is unit hygiene — keep cc in km/s to match H0H_0's km/s, and only convert to light-years at the end. Always glance at zz first: if zz were near or above 11 you would have to abandon z=v/cz = v/c and flag the relativistic regime instead of blindly multiplying.

Exam traps

Claiming cosmology is on your board when it is not. Cosmology — Hubble's law, the Big Bang, the dark sector — is enrichment beyond the Indian core boards. It appears in IB Physics HL (HL-only material on galaxies and the expanding universe; formerly the Astrophysics option) and in some A-Level specifications, and nowhere in CBSE, ICSE, JEE (Main or Advanced), NEET or AP Physics 2. Do not cite it as a CBSE/JEE/NEET topic; conversely, if you sit IB-HL or A-Level, know that v=H0dv = H_0 d, the Hubble-time age and the CMB are fair game.

Saying the Big Bang exploded from a point in space. It expanded space itself, everywhere at once, with no centre and no edge. An examiner rewards "expansion of space," not "explosion in space."

Confusing cosmological redshift with a Doppler shift through space. The wavelength stretches because space stretches; z≈v/cz \approx v/c is only the small-zz coincidence, and it fails once z≳0.1z \gtrsim 0.1. State the mechanism, not just the formula.

Mishandling the units of H0H_0. H0=70 km/s per MpcH_0 = 70\ \text{km/s per Mpc} must be converted to s−1\text{s}^{-1} (2.27×10−182.27\times10^{-18}) before you invert it for an age — mixing km, s and Mpc is the commonest slip in the Hubble-time calculation.

Forgetting the age is an estimate. 1/H0=14 Gyr1/H_0 = 14\ \text{Gyr} assumes constant expansion; the measured 13.8 Gyr13.8\ \text{Gyr} comes from a full model. Quote 1/H01/H_0 as an approximate age and say why.

Calling dark matter "matter we just cannot see yet." It is not ordinary unlit matter — its total dwarfs all the gas and dead stars, and Big-Bang element abundances forbid it from being protons and neutrons. It is some new kind of matter, detected only by gravity.

Origins · 1 minEdwin Hubble and how this was discovered
EH
Edwin Hubble
1889–1953 · Mount Wilson Observatory, California, USA

Edwin Powell Hubble was an American astronomer, once a promising boxer and a qualified lawyer, who turned to the sky and reshaped humanity's map of it twice. Working with the great 100-inch telescope at Mount Wilson, he first proved in 1923–24 that the faint "spiral nebulae" — including Andromeda — are entire galaxies far beyond the Milky Way, enlarging the known universe from one galaxy to countless. Then in 1929 he published the velocity–distance relation now bearing his name: galaxies recede at speeds proportional to their distance, the first observational evidence that the universe is expanding. Hubble himself stayed cautious about interpreting the redshifts as true expansion, and it was Georges Lemaître who, in 1927, had already derived the relation theoretically from an expanding-universe model. The space telescope that carries Hubble's name still measures the expansion he discovered.

History
1912
— Vesto Slipher measures the first spectrum of a spiral nebula (Andromeda), finding it blueshifted; by 1917 his survey shows most spirals are redshifted, receding at hundreds of kilometres per second.
1927
— Georges Lemaître proposes an expanding universe, deriving the velocity–distance relation before Hubble.
1931
— Lemaître proposes the "primeval atom", a single explosive origin for the expanding universe.
1929
— Edwin Hubble publishes the linear velocity–distance law from galaxy data, the observational cornerstone of the expanding universe.
1948
— George Gamow, Ralph Alpher and Robert Herman work out Big-Bang nucleosynthesis of the light elements and predict a leftover radiation of a few kelvin.
1965
— Arno Penzias and Robert Wilson discover the cosmic microwave background at 2.7 K (Nobel 1978), confirming the hot Big Bang.
1998
— two supernova teams find the expansion is accelerating, revealing dark energy (Nobel 2011 to Perlmutter, Schmidt and Riess).

Going further

Texts. For IB-HL: the IB Physics HL cosmology content on galaxies and the expanding universe (Hubble's law, the Big Bang, cosmic scale; formerly the Astrophysics option). For A-Level: the AQA/OCR Astrophysics and Cosmology options. Broader reading: Weinberg, The First Three Minutes (the Big Bang for a general reader) · Liddle, An Introduction to Modern Cosmology (the algebra-and-a-little-calculus next level) · Ryden, Introduction to Cosmology (the full undergraduate treatment).

Provenance. Anchor values from LANE_SPEC: H0=70 km/s per MpcH_0 = 70\ \text{km/s per Mpc}; 1 Mpc=3.086×1022 m=3.26×106 ly1\ \text{Mpc} = 3.086\times10^{22}\ \text{m} = 3.26\times10^{6}\ \text{ly}; 1 yr=3.156×107 s1\ \text{yr} = 3.156\times10^{7}\ \text{s}; c=3.0×108 m/sc = 3.0\times10^{8}\ \text{m/s}; CMB T=2.7 KT = 2.7\ \text{K}; Wien b=2.9×10−3 m ⋅ Kb = 2.9\times10^{-3}\ \text{m}\,\cdot\,\text{K}; composition 5%/27%/68%5\%/27\%/68\%. Recompute list: H0=2.27×10−18 s−1H_0 = 2.27\times10^{-18}\ \text{s}^{-1}; Hubble time 1/H0=4.41×1017 s=14.0 Gyr1/H_0 = 4.41\times10^{17}\ \text{s} = 14.0\ \text{Gyr} (vs measured 13.813.8); Hubble length c/H0=1.32×1026 m≈14c/H_0 = 1.32\times10^{26}\ \text{m} \approx 14 Gly; d=100 Mpc⇒v=7000 km/sd = 100\ \text{Mpc} \Rightarrow v = 7000\ \text{km/s}, z=0.023z = 0.023, λ:500.0→511.7 nm\lambda: 500.0 \to 511.7\ \text{nm}; z=0.050⇒v=15,000 km/sz = 0.050 \Rightarrow v = 15{,}000\ \text{km/s}, d=214 Mpc=7.0×108 lyd = 214\ \text{Mpc} = 7.0\times10^{8}\ \text{ly}, lookback ≈700 Myr\approx 700\ \text{Myr}; CMB Wien peak λmax=1.1 mm\lambda_{\text{max}} = 1.1\ \text{mm}; composition sum =100%= 100\%; the no-centre check v⃗C−v⃗B=H0(r⃗C−r⃗B)\vec{v}_C - \vec{v}_B = H_0(\vec{r}_C - \vec{r}_B).

Prerequisites. Stellar Physics: The H–R Diagram & the Lives of Stars — where luminosity, stellar fusion and the manufacture of the heavy elements are built; cosmology sets the stage on which those stars live and die. Leads to. The honest next step is general relativity: aq-sr-special-to-general-relativity, the university seam where the algebraic Hubble law is replaced by the curved-spacetime Friedmann model of an expanding universe (that treatment uses calculus and lies beyond this article — it is named as a pointer, never a dependency).

If everything is rushing away from us, aren't we at the centre of the universe?

No — and this is the most beautiful part. Because the expansion is uniform, an astronomer in any galaxy sees exactly what we see: everything receding, the farther things faster, following v=H0dv = H_0 d with the same H0H_0. We showed this with vector algebra: the velocity field v⃗=H0r⃗\vec{v} = H_0\vec{r} looks identical from every one of its own points. It is like the raisins in rising bread — every raisin sees all the others moving away, and none is the centre. The appearance of being central is shared by everyone, which means it singles out no one. There is no centre to the expansion and no edge to the universe.

Is the Big Bang an explosion, and if so, where did it happen?

It is not an explosion in the ordinary sense and it did not happen at a place. An explosion throws matter outward through space from a point. The Big Bang was an expansion of space itself, occurring everywhere at once — the early universe was hot and dense everywhere, and space has been growing ever since. Asking "where did it happen" assumes a pre-existing space to happen in; there wasn't one. Every point in today's universe, including the spot you are sitting in, was part of that hot dense state. So the Big Bang happened here, and there, and in every galaxy, all at the same time.

How can distant galaxies recede faster than light without breaking relativity?

Because they are not moving through space faster than light — space between us and them is expanding, and expansion adds up over distance. Relativity forbids anything from travelling through space faster than light, but it places no such limit on how fast space itself can stretch. Beyond a certain distance (the Hubble length, about 1414 billion light-years) the cumulative stretching carries galaxies away faster than cc, and their light can no longer reach us. This is also why the simple z≈v/cz \approx v/c breaks down for large redshifts: at high zz the redshift measures how much space has grown, not a genuine speed you could clock with a radar gun.

What is the difference between dark matter and dark energy?

They are unrelated despite the shared word "dark." Dark matter is a form of mass — about 27%27\% of the universe — that clumps under gravity and holds galaxies together; we detect it because galaxies rotate too fast and light bends around invisible mass, but it emits no light and is not made of ordinary protons and neutrons. Dark energy is about 68%68\% of the universe and does the opposite of clumping: it is a smooth property of space with negative pressure that pushes the expansion to accelerate. Dark matter pulls things together; dark energy drives them apart. Both are called "dark" only because we cannot see them directly and do not yet know what they are.

How do we actually know the universe is 13.8 billion years old and not exactly 1/H₀?

The reciprocal 1/H0≈141/H_0 \approx 14 billion years assumes the expansion rate has stayed constant, which it hasn't: gravity slowed the early expansion and dark energy is speeding up the recent one. The true age comes from fitting a full model to several data sets at once — chiefly the detailed pattern of ripples in the microwave background, plus galaxy surveys and supernova distances. That fit yields 13.813.8 billion years. It is close to 1/H01/H_0 because the early slowdown and the late speed-up happen to roughly cancel, but the agreement is a happy coincidence of our universe's ingredients, not a theorem. Quote 1/H01/H_0 as an estimate and the fitted value as the measurement.

Why is the relic radiation microwaves specifically, and not visible light or radio?

When the universe first turned transparent, about 380,000380{,}000 years after the Big Bang, it was around 3000 K3000\ \text{K} and glowed like a dim red-hot surface — visible and infrared light. Since then space has expanded by a factor of about a thousand, stretching every one of those wavelengths by the same factor and cooling the radiation to 2.7 K2.7\ \text{K}. Wien's law puts the peak of a 2.7 K2.7\ \text{K} black body at about 1.1 mm1.1\ \text{mm}, which is the microwave band — hence "cosmic microwave background." So the choice of microwaves is not arbitrary: it is the original hot glow, redshifted by a thousandfold expansion into exactly the microwave region we now detect.

Is cosmology going to be on my exam?

Only for some boards. This material — Hubble's law, the Big Bang, the CMB, dark matter and dark energy — is enrichment for students on CBSE, ICSE, JEE, NEET and AP Physics 2; those syllabuses do not test it, though it makes excellent context for the atomic and nuclear physics they do test. It is genuinely examinable in IB Physics HL (HL-only material on galaxies and the expanding universe; formerly the Astrophysics option) and in some A-Level specifications, where you may be asked to state and use v=H0dv = H_0 d, estimate the age from 1/H01/H_0, and describe the evidence for the Big Bang. Check your own syllabus, but if you are on the Indian core boards, treat this as fascinating background rather than exam drill.

Before this

Where this leads