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) |