next up previous contents
Next: Compbb Up: Additive Model Components Previous: Cevmkl

            cflow: cooling flow

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 H_0 = 50 and q_0 = 0.. 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)