Short Topical Videos
- Specific Intensity: What's the Flux? (by Aaron Parsons)
- Photon Buckets: How (Radio) Telescopes Receive Power (by Aaron Parsons)
 Reference Material
- Brightness and Flux Density (Condon & Ransom, NRAO)
- Specific Intensity: The Fount of All Knowledge (Heiles, UC Berkeley)
- Specific Radiative Intensity (Wikipedia)
1 Units of Radiation
In order to motivate the useful properties of specific intensity, it’s helpful to list the variety of ways we have of describing the energy transfer coming from electromagnetic waves (or photons) striking a telescope. Below are a few that are commonly used:
Voltage (with units of Volts, V) gives the most direct view of the shape of the electromagnetic waves that are striking a (usually radio) telescope. However, astronomical signals are usually noise, so the random fluctuations in voltage aren’t usually terribly illuminating, and you can’t average them directly. This makes voltage a poor unit for learning about the sky.
Power (with units of ergs/s, or watts, or dBm), which is generally proportional to voltage squared, is a much more useful quantity. For example, it can be averaged over time. However, it encodes no information about what frequency interval (bandwidth) that the measurement was made over, and the power of a measurement is generally proportional to the bandwidth of the signals you let in.
The unit dBm may not be familiar to most astronomers. It refers to decibels relative to a milliwatt:
1.3 Power Density
Power density (with units of ergs/s/Hz, or dBm/Hz), divides out by the bandwidth B that the measurement is made over. However, it contains no information about how large an area this signal was collected over.
Flux (with units of ergs/s/cm2) divides power received by the area the signal was collected over, but it does not divide by the bandwidth.
1.5 Flux Density
Flux density (with units of ergs/(s cm2 Hz), or Jy) combines power density and flux to get a measurement that divides out bandwidth and collecting area. Most astronomers can agree on the flux density of a source, but if the beam of your telescope is smaller than the source on the sky, you can get a different answer because you are not be getting all the photons from that source.
Radio astronomers use Janskies (which are units of flux density) commonly. A Jansky is defined as:
1.6 Specific Intensity
Specific intensity (with units of ergs/(s cm2 Hz sr), Jy/beam) divides flux density by the angular area of the measurement (or of the source), and is intrinsic to source. As - conserved along a ray
1.7 Brightness Temperature
Brightness temperature (with units of K) uses the Rayleigh-Jeans tail of a blackbody spectrum to define an equivalent temperature corresponding to a specific intensity. It is often used as a proxy for specific intensity.
2 Specific Intensity, Specifically
Here are some terms pertaining to telescope observations:
aperture area (ΔA), solid angle on sky (ΔΩ), exposure time (Δt), collects energy (ΔE), over waveband (Δν), but .
Iν is the specific intensity per unit frequency.
Flux density is power per unit frequency passing through a differential area whose normal is . Thus, flux density is:
Proof that Specific Intensity is conserved along a ray
The power received by the telescope is:
where Iν(α,δ) is the intensity as a function of right-ascension (α) and declination (δ). Say that Σν(α,δ) is the surface luminosity of a patch of sky (that is, the emitted intensity). Then power emitted by patch of sky is:
Recognizing that :
This derivation assumes that we are in a vacuum and that the frequencies of photons are constant. If frequencies change, then though specific intensity Iν is not conserved, is. Also, for redshift z,
so intensity decreases with redshift. Finally:
is conserved along a ray, where η is the index of refraction.
A blackbody is the simplest source: it absorbs and reemits radiation with 100% efficiency. The frequency content of blackbody radiation is given by the Planck Function:
(The Planck Function for Black Body Radiation)
The # density of photons having frequency between ν and ν + dν has to equal the # density of phase-space cells in that region, multiplied by the occupation # per cell. Thus:
so we have it. In the limit that :
Rayleigh-Jeans tail Note that this tail peaks at . Also,
Reiteration: Conservation of specific intensity
Conservation of specific intensity told us the intensity collected by your telescope is absolutely equal to the surface intensity emitted into the angle leftrightarrowonding to your pixel on the sky. Specific intensity is distance independent. 1m2 of sky emitted into one square degree specific intensity measured by a 1m2 telescope pointed at a one square degree pixel of sky.
We have flux, flux density, surface brightness, and spectral energy distribution to describe luminosity. When in doubt, look at the units. Surface brightness, like specific intensity, is distance independent. It is simply specific intensity integrated over frequency.
If you look at something through a lens, the specific intensity of a point is conserved. In the lens, the specific intensity may be greater, because is conserved (remember that η is the index of refraction of the medium), but once the light goes out again, even if the object looks bigger, the specific intensity is the same. This does not violate conservation of energy because the light is being focused to a smaller area.
Now if something is inside the lens (say, a bowl of water), then the lens bends light rays closer to each other, increasing the specific intensity. Thus, the object is emitting/scattering higher density photons, and appears more luminous, and the object also appears larger. This means that there must be some places where the object, omitting the lens, would have been visible, but now isn’t.