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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)