When a star or galaxy moves away from us, the light it emits stretches to longer wavelengths.
This shift towards the red end of the spectrum is called redshift.
The amount of shift is measured by the ratio
\$z = \dfrac{\lambda{\text{observed}} - \lambda{\text{emitted}}}{\lambda_{\text{emitted}}}\$.
Think of it like a stretching rubber band that gets longer as the source moves away.
Edwin Hubble found that the redshift of a galaxy is proportional to its distance:
\$v = H_0 \, d\$, where
\$v\$ is the recession velocity, \$H_0\$ is the Hubble constant, and \$d\$ is distance.
Using the Doppler approximation for small speeds,
\$v \approx c\,z\$, we can rewrite Hubble’s Law as
\$z \approx \dfrac{H_0}{c}\, d\$.
This means the farther a galaxy is, the more its light is redshifted—just like the sound of a siren gets lower as an ambulance drives away.
Imagine inflating a balloon with dots on it. As the balloon expands, every dot moves away from every other dot, and the distance between them grows. The dots are like galaxies; the balloon’s surface is like space.
| Galaxy | Redshift \$z\$ | Distance (Mpc) |
|---|---|---|
| NGC 1300 | 0.005 | 70 |
| M87 | 0.004 | 60 |
| NGC 4993 | 0.009 | 120 |
Keep the balloon analogy handy; it’s a favourite for explaining cosmic expansion in exams!