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) |