AstronomyLight and Telescopes

Telescopes: Light-Gathering and Resolution

A telescope's light-gathering power grows with the square of its diameter, and a bigger aperture shows finer detail.

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You know from Refraction and Lenses that a lens bends light to a focus. A telescope uses a big lens (a refractor) or a curved mirror (a reflector) to bring light from a distant object to a focus, where an eye, a camera or a spectrograph collects it. Every large research telescope today is a reflector, because a mirror can be supported from behind and has no color fringes.

Why it works

Most things in the sky are faint, so a telescope's first job is to gather light. It catches every photon that lands on its mirror, so the light gathered is proportional to the area, $\pi D^2/4$: double the diameter, four times the light. Its second job is to resolve detail. Light spreading as waves (diffraction) blurs every point into a tiny disk, of angular size about $1.22\lambda/D$ radians; in arcseconds, $\theta \approx 2.5 \times 10^{5}\,\dfrac{\lambda}{D}$. A wider aperture makes a smaller blur. Magnification, $f_{\text{objective}}/f_{\text{eyepiece}}$, comes third: it only spreads out whatever light and detail the aperture captured.

Key idea

Light-gathering power grows as $D^2$; the finest resolvable angle is about $2.5 \times 10^{5}\,\lambda/D$ arcseconds. Both depend on the aperture $D$, which is why astronomers build ever larger mirrors.
Two telescopes side by side: the collecting areas (with photons arriving) and how each one images a close pair of stars.

Worked examples

Worked example: A big mirror against your eye

How much more light does the $10$ m Keck telescope collect than a dark-adapted eye with a $7$ mm pupil?
  1. Same units: $10$ m $= 10{,}000$ mm.
  2. Ratio of areas $= \left(\frac{10{,}000}{7}\right)^2 = 1429^2 = 2.0 \times 10^{6}$.
  3. About two million times the light: it sees objects millions of times fainter.

Answer: About $2 \times 10^{6}$ times.

Worked example: Hubble's sharpness

What is the finest detail the $2.4$ m Hubble Space Telescope can resolve at $500$ nm?
  1. $\lambda = 500$ nm $= 5.00 \times 10^{-7}$ m.
  2. $\theta = 2.5 \times 10^{5} \times \frac{5.00 \times 10^{-7}}{2.4} = 0.052$ arcseconds.
  3. Ground telescopes this size are blurred by the turbulent air to about $0.5$ to $1$ arcsecond, unless they use adaptive optics; Hubble, above the air, reaches its full sharpness.

Answer: About $0.05$ arcseconds.

Common mistake

Many people think a telescope's main job is to magnify. Stars are so far away that even the biggest telescope shows them as points; what it shows is more of them, fainter ones, and finer detail in extended objects. Extra magnification without more aperture only makes a bigger, dimmer blur. Check: telescopes are named by their diameter (a "10 m telescope"), never by their magnification.
A refracting telescope: the objective forms an image that the eyepiece views. Magnification is the ratio of their focal lengths.
Try lenses and focal lengths on the Optics Bench.
Try it in the Science LabOptics Bench

Practice

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Sources and further reading

  • OpenStax, Astronomy 2e, section 6.1, Telescopes
  • OpenStax, Astronomy 2e, section 6.2, Telescopes Today
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