Deriving the total atomic hydrogen (HI) mass of a galaxy
ALFALFA detects the HI spectral profile of a galaxy, that is, its
HI line flux over the frequency range which corresponds to the radial velocities
of all the HI atoms in the galaxy. The total HI line flux, ∫F dV, in Jy-km/s,
can be used to derive the total HI mass, in solar masses,
using the distance, estimated
from the systemic velocity via Hubble's law or by some other means.
where D is the distance in Mpc.
This equation derives from the quantum mechanics of the hyperfine transition and
the assumption that the HI gas is optically thin. If you want to know more
about how the line arises and where that equation comes from, check out a
couple of "classic" references:
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Last updated Wed Apr 23 08:30:53 EDT 2008 by martha