6.2.3 The Universe

Syllabus
0625–2026–2027
Topic
6.2.3
Level

Learning objectives

6.2.3.1Milky Way is one of many billions of• Know: the Milky Way is one of many billions of galaxies making up the Universe and that the diameter of the Milky Way is approximately 100 000 light-years6.2.3.2Redshift as an increase in the• Describe redshift as an increase in the observed wavelength of electromagnetic radiation emitted from receding stars and galaxies6.2.3.3Light emitted from distant galaxies• Know: the light emitted from distant galaxies appears redshifted in comparison with light emitted on the Earth6.2.3.4Redshift in the light from distant• Know: redshift in the light from distant galaxies is evidence that the Universe is expanding and supports the Big Bang Theory6.2.3.5Microwave radiation of a specific• Know: microwave radiation of a specific frequency is observed at all points in space around us and is known as cosmic microwave background radiation (CMBR)6.2.3.6The CMBR was produced shortly after• Explain that the CMBR was produced shortly after the Universe was formed and that this radiation has been expanded into the microwave region of the electromagnetic spectrum as the Universe expanded6.2.3.7Speed v at which a galaxy is moving• Know: the speed v at which a galaxy is moving away from the Earth can be found from the change in wavelength of the galaxy’s starlight due to redshift6.2.3.8Distance d of a far galaxy can be• Know: the distance d of a far galaxy can be determined using the brightness of a supernova in that galaxy6.2.3.9Hubble constant H0 as recession speed• Define Hubble constant H0 as recession speed divided by distance from Earth; recall/use: H0 = v/d6.2.3.10Current estimate for H0 is 2.2 × 10–18• Know: the current estimate for H0 is 2.2 × 10–18 per second6.2.3.11D/v = 1/H0 estimates the age of the• Know d/v = 1/H0 estimates the age of the Universe and supports the idea that all matter was once at a single point

Place the Milky Way within the Universe

The Universe contains many billions of galaxies. The Milky Way is one of those galaxies.

The Milky Way itself contains many billions of stars and has an approximate diameter of 100 000 light-years.

Light therefore takes about 100 000 years to travel a distance equal to the Milky Way's diameter. This is a galactic scale, far larger than the Solar System.

Scale Contains
Solar System the Sun and objects orbiting it
Milky Way galaxy many billions of stars, including the Sun
Universe many billions of galaxies

The Milky Way is not the whole Universe, and 100 000 light-years is its approximate diameter, not its distance from Earth.

Describe redshift from a receding source

Redshift is an increase in the observed wavelength of electromagnetic radiation from a star or galaxy that is moving away from the observer.

Astronomers compare identifiable spectral lines in received starlight with the wavelengths of the same lines measured in a laboratory. A shift to longer wavelengths is a redshift.

For a receding source, successive wavefronts arrive more spread out, so the observed wavelength is longer than the emitted or laboratory wavelength.

Redshift does not mean that all received light is visibly red. The whole pattern of spectral wavelengths is shifted towards longer wavelengths.

Recognise redshift in light from distant galaxies

Light from distant galaxies generally appears redshifted when compared with light produced by the same elements on Earth.

If a hydrogen line has wavelength 656 nm in a laboratory but is observed at 667 nm from a galaxy, the observed wavelength has increased: 667 − 656 = 11 nm. The galaxy's light is redshifted.

The known laboratory spectrum acts as the reference. Matching the pattern of lines identifies the element; their displacement to longer wavelength identifies redshift.

A longer measured wavelength must be compared with the correct laboratory line. A single wavelength without a reference does not by itself establish redshift.

Use redshift as evidence for an expanding Universe

Redshift in the light from distant galaxies shows that those galaxies are receding from us.

When light from galaxies in all directions is generally redshifted, the large-scale separations between galaxies are increasing. This is evidence that the Universe is expanding.

Running the expansion model backwards implies that matter was closer together in the past. Redshift therefore supports the Big Bang Theory.

More distant galaxies generally show greater redshift and recession speed, strengthening the expansion interpretation.

Redshift is supporting evidence, not a claim that Earth is at a special central point. Expansion is observed on the large scale between galaxies.

Identify cosmic microwave background radiation

Cosmic microwave background radiation, abbreviated CMBR, is microwave electromagnetic radiation of a specific frequency range observed at all points in space around us.

Detectors receive this faint microwave background from every direction rather than from one local star, planet or galaxy.

Its all-sky presence is why it is described as a cosmic background: it is a property observed throughout the surrounding Universe.

CMBR is not ordinary microwave transmission from communication equipment and is not concentrated in one direction or one visible object.

Explain the origin of the CMBR

The radiation that became the CMBR was produced shortly after the Universe formed.

As the Universe expanded, the wavelength of this radiation was stretched to longer wavelengths.

That expansion shifted the radiation into the microwave region of the electromagnetic spectrum, where it is observed today from all directions.

The CMBR's ancient origin, stretched wavelength and all-sky distribution support the model of a hot early Universe that has expanded.

The CMBR was not newly produced by modern galaxies. Its wavelength changed because the Universe expanded after the radiation was released.

Determine galaxy recession speed from redshift

The recession speed v of a galaxy can be found from the redshift of its starlight: the measured change in wavelength relative to laboratory wavelengths.

Step Observation or inference
1 identify a known spectral line in the galaxy's light
2 compare its observed wavelength with the laboratory wavelength
3 find the increase in wavelength, or redshift
4 use the redshift relation supplied for the question to determine recession speed

A larger wavelength increase means a larger redshift and, under the syllabus model, a greater speed away from Earth.

Redshift determines recession speed, not distance directly. Galaxy distance is obtained using a separate observation such as supernova brightness.

Determine galaxy distance from a supernova

The distance d to a far galaxy can be determined using the observed brightness of a suitable supernova in that galaxy.

A supernova of known intrinsic brightness appears dimmer when it is farther away. Comparing its observed brightness with the expected intrinsic brightness provides the distance.

Astronomers can therefore obtain the two quantities needed for Hubble analysis in different ways: supernova brightness gives distance, while redshift gives recession speed.

The overall brightness of an unknown galaxy is not the same standard measurement. The syllabus relation uses the brightness of a supernova in that galaxy.

Define and use the Hubble constant

The Hubble constant H₀ is the ratio of a galaxy's recession speed v to its distance d from Earth: H₀ = v/d.

If H₀ is treated as constant, v = H₀d, so recession speed is directly proportional to distance. A graph of v against d has gradient H₀ when units are consistent.

Required quantity Relation
Hubble constant H₀ = v/d
recession speed v = H₀d
galaxy distance d = v/H₀

If v is in m/s and d is in m, the metres cancel and H₀ has unit s⁻¹. Convert kilometres and light-years before substitution when required.

H₀ is not the speed of light and it is not itself the age of the Universe. It is a speed-per-distance ratio.

Recall the current estimate of the Hubble constant

The current syllabus estimate of the Hubble constant is H₀ = 2.2 × 10⁻¹⁸ s⁻¹, read as 2.2 × 10⁻¹⁸ per second.

The s⁻¹ unit follows from H₀ = v/d: (m/s)/m = 1/s.

The very small value is expected because cosmic expansion is measured over extremely large distances and timescales.

Do not confuse 2.2 × 10⁻¹⁸ s⁻¹ with the speed of light, 3.0 × 10⁸ m/s. Their quantities, units and powers of ten are different.

Estimate the age of the Universe from H₀

From H₀ = v/d, rearranging gives d/v = 1/H₀. The ratio distance/speed has units of time and provides an estimate of the age of the Universe.

Using H₀ = 2.2 × 10⁻¹⁸ s⁻¹ gives age ≈ 1/H₀ ≈ 4.5 × 10¹⁷ s. Dividing by about 3.2 × 10⁷ s/year gives approximately 1.4 × 10¹⁰ years.

Galaxies are now receding, and more distant galaxies generally recede faster. Extrapolating their separations backwards implies that matter was closer together and supports the idea that all matter was once concentrated at a single point.

This is an estimate based on using the current expansion relation over cosmic history; it is not a direct stopwatch measurement.

Use the reciprocal 1/H₀, not H₀ itself. The reciprocal has units of seconds because H₀ has units s⁻¹.