(updated for 2013)
The term “temperature” describes several different quantities in the ISM, and in observational astronomy. Only under idealized conditions (i.e. thermodynamic equilibrium, the Rayleigh Jeans regime, etc.) are (some of) these temperatures equivalent. For example, in stellar interiors, where the plasma is very well-coupled, a single “temperature” defines each of the following: the velocity distribution, the ionization distribution, the spectrum, and the level populations. In the ISM each of these can be characterized by a different “temperature!”
the temperature of a blackbody that reproduces a given flux density at a specific frequency, such that
Note: units for are .
This is a fundamental concept in radio astronomy. Note that the above definition assumes that the index of refraction in the medium is exactly 1.
(also called , the radiation temperature) is defined by
which is the integrated intensity of a blackbody of temperature . is the Stefan-Boltzmann constant.
is defined by the slope (in log-log space) of an SED. Thus is the temperature of a blackbody that has the same ratio of fluxes at two wavelengths as a given measurement. Note that for a perfect blackbody.
is the temperature that a particle of gas would have if its Maxwell-Boltzmann velocity distribution reproduced the width of a given line profile. It characterizes the random velocity of particles. For a purely thermal gas, the line profile is given by
where in frequency units, or
in velocity units.
In the “hot” ISM is characteristic, but when (where are the Doppler full widths at half-maxima [FWHM]) then does not represent the random velocity distribution. Examples include regions dominated by turbulence.
can be different for neutrals, ions, and electrons because each can have a different Maxwellian distribution. For electrons, , the electron temperature.
is the temperature which, when plugged into the Saha equation, gives the observed ratio of ionization states.
is the temperature which, when plugged into the Boltzmann distribution, gives the observed ratio of two energy states. Thus it is defined by
Note that in stellar interiors, . In this room, , but .
is a special case of for spin-flip transitions. We’ll return to this when we discuss the important 21-cm line of neutral hydrogen.
is the temperature of a blackbody having the same mean frequency as the observed continuum spectrum. For a blackbody, . This is a useful quantity for young stellar objects (YSOs), which are often heavily obscured in the optical and have infrared excesses due to the presence of a circumstellar disk.
is a directly measured quantity (commonly used in radio astronomy) that incorporates radiative transfer and possible losses between the source emitting the radiation and the detector. In the simplest case,
where is the telescope efficiency (a numerical factor from 0 to 1) and is the optical depth.