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 model assumes and . The abundance ratios are set by the abund 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) |