A cooling flow model after Mushotzky & Szymkowiak (Cooling Flows in Clusters and Galaxies ed. A. C. Fabian, 1988). This one uses the mekal (or vmekal) model for the individual temperature components and differs from cflow in setting the emissivity function to be the inverse of the bolometric luminosity. The model assumes H_{0} = 50 and q_{0} = 0. 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 precalculated table. The former is slower but more accurate.
For the mkcflow model the parameters are:
par1 
low temperature (keV) 
par2 
high temperature (keV) 
par3 
abundance relative to Solar 
par4 
(fixed) redshift 
par5 
0 calculate 
1 interpolate 

2 interpolate using APEC model 

norm 
Mass accretion rate (solar mass/yr) 
While for the vmcflow variant the parameters are:
par1 
low temperature (keV) 
par2 
high temperature (keV) 
par3par16 
Abundances for He, C, N, O, Ne, Na, Mg, Al, Si, S, Ar, Ca, Fe, Ni wrt Solar (given by the Anders & Grevesse mixture) 
par17 
Redshift 
par18 
0 calculate 
1 interpolate 

2 interpolate using APEC model 

norm 
Mass accretion rate (solar mass/yr) 