mkcflow, vmcflow: cooling flow, mekal
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 H0 = 50 and q0 = 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 pre-calculated 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 |
|
1 |
|
|
2 |
|
|
norm |
Mass accretion rate (solar mass/yr) |
While for the vmcflow variant the parameters are:
|
par1 |
low temperature (keV) |
|
par2 |
high temperature (keV) |
|
par3-par16 |
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 |
|
1 |
|
|
2 |
|
|
norm |
Mass accretion rate (solar mass/yr) |
