Description

A cooling flow model after Mushotzky and Szymkowiak ("Cooling Flows in Clusters and Galaxies" ed. Fabian, 1988). This one uses the xsmekal model for the individual temperature components and differs from xscflow in setting the emissivity function to be the inverse of the cooling time. The switch parameter determines whether the xsmekal 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.

The model assumes H_0=50 and q_0=0. The abundance ratios are set by the xspecabundan command.

Please note that there is no support in CIAO 3.2 for setting the cflow_version and cflow_ntemps variables of the model. The version used in Sherpa corresponds to cflow_version=2, and cflow_ntemps is fixed at 10. Prior to CIAO 3.2 the model used corresponded to cflow_version=1, and so contained an error in the calculation of the emission measure distribution at the ends of the temperature range.

xsmkcflow Parameters

This information is taken from the XSpec User's Guide. Version 11.3.1 of the XSpec models is supplied with CIAO 3.2.