Diffraction of light through a rectangular aperture is a rather straightforward extension of 1-dimensional diffraction from a slit, as shown in the diagrams below.

A circular aperture is qualitatively similar, but an accurate quantitative treatment of the pattern requires more complicated mathematics. The intensity pattern is called the "Airy Disk". The main features are shown in the diagram below. The first minimum occurs at an angle θ = 1.22 λ/D, where D is the diameter of the aperture. On a screen a distance L >> D from the aperture the minimum is seen at a radial distance r' = 1.22 λL/D from the center of the pattern

Producing a laser beam is an attempt to confine the light in the directions transverse to the direction of propagation. The light will spread out in the same way it does after passing through an aperture.

Assume that at z = 0 the diameter of a laser beam is restricted to a(0). The angle through which the light spreads is approximately
θ ≈ λ/a(0). (For back-of-the-envelope calculations we
often ignore the factor of 1.22.) Because the laser beam diameter is
typically much larger the wavelength of light, or a(0) >> λ, θ is quite small.
At a large distance z the diameter of the beam will have increased to a(z) ≈ z*2θ.
Consider a HeNe laser, for which λ = 633 nm with a beam waist of ~ 0.6 mm. Then
θ ~ 10^{-3} rad = 1 millirad. The beam must propagate ~ 3 m before
the diameter increases by a factor of 10.

In geometrical optics we assume that an ideal, aberration-free lens focuses
parallel rays to a single point one focal length away from the lens. But the
lens itself acts like an aperture with diameter D for the incident light. The
light passing through the lens therefore spread out. This yields a blurred spot
at the focal point. Light near the focal point exhibits an Airy Disc pattern. The size of the Airy Disc is determined by the focal length f and diameter D of
the lens. The radius r of the Airy Disc at the focal point of a lens is given by
r = 1.22 λf/D.

If all ray aberrations in an optical system can be eliminated, such that all
of the rays leaving a given object point land inside of the Airy Disc associated
with the corresponding image point, then we have a diffraction-limited optical
system. This is the absolute best we can do for an optical system that has
lenses with finite diameters.

The **resolving power** of an
optical instrument is its ability to separate the images of two objects, which
are close together. Some binary stars in the sky look like one single star when
viewed with the naked eye, but the images of the two stars are clearly resolved
when viewed with a telescope.

Why?

The merging of the images in the eye is caused by diffraction.

If you look at a far-away object, then the image of the object will form a
diffraction pattern on your retina. For two far-away objects, separated by a
small angle θ, the diffraction patterns will overlap.
You are able to resolve the two objects as long as the central maxima of the two
diffraction patterns do not overlap. The two images are just resolved when one
central maximum falls onto the first minimum of the other diffraction pattern. This is known as the
**Rayleigh criterion**. If
the two central maxima overlap the two objects look like one.

The width of the central maximum in a diffraction pattern depends on the size
of the aperture, (i.e. the size of the slit). The aperture of your eye is your
pupil. A telescope has a much larger aperture, and therefore has a greater
resolving power. The minimum angular separation of two objects which can just be
resolved is given by θ_{min}=1.22 λ/D,
where D is the diameter of the aperture. The factor of 1.22 applies to circular
apertures like the pupil of your eye or the apertures in telescopes and cameras.

The closer you are to two objects, the greater is the angular separation
between them. Up close, two objects are easily resolved. As your distance from
the objects increases, their images become less well resolved and eventually
merge into one image.

A spy satellite travels at a distance of 50 km above Earth's surface. How large must the lens be so that it can resolve objects with a size of 2 mm and thus read a newspaper? Assume the light has a wavelength of 400 nm.

Solution:

Diffraction limits the resolution according to
θ = 1.22 λ/D = y/L. Here
the height of the object to be resolved is y and the distance to the
object is L. Solving for D we find D = 12.2 m.