A cooling flow model after Mushotzky & Szymkowiak (``Cooling Flows in Clusters
and Galaxies" ed. Fabian, 1988). This one uses the mekal model for the
individual temperature components and differs from cflow in setting the
emissivity function to be the inverse of the cooling time. The model assumes
and 
. Abundance ratios are set by the abund command.
The switch parameter determines whether the mekal code will be run to
calculate the model spectrum for each temperature or whether the model
spectrum will be interpolated from a pre-calculated table. The former
is slower but more accurate.
par1 = low temperature (keV)par2 = high temperature (keV)
par3 = abundance relative to Solar
par4 = redshift
par5 = 0
calculate, 1
K = Mass accretion rate (solar mass/yr)