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Latest revision as of 18:13, 14 February 2010
Here are some terms pertaining to telescope observations:
aperture area (), solid angle on sky (), exposure time (), collects energy (), over waveband (), but .
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 is the intensity as a function of right-ascension () and declination (). Say that 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 is not conserved, is. Also, for redshift ,
so intensity decreases with redshift. Finally:
is conserved along a ray, where 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 and 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,