cflow: cooling flow

A cooling flow model after Mushotzky & Szymkowiak (Cooling Flows in Clusters and Galaxies, ed. Fabian, 1988). An index of zero for the power-law emissivity function corresponds to emission measure weighted by the inverse of the bolometric luminosity at that temperature. The abundance ratios are set by the abund command. Redshift is converted to distance using the cosmology set by the cosmo command.

par1	index for power-law emissivity function
par2	low temperature (keV)
par3	high temperature (keV)
par4	abundance relative Solar
par5	redshift, z
norm	Mass accretion rate (solar mass/yr)

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Last modified: Friday, 23-Aug-2024 13:20:40 EDT