This model describes X-ray transmission of an isotropic source of photons located at the center of a uniform, spherical distribution of matter, correctly taking into account Compton scattering. The model can be used for radial column densities up to cm. The valid energy range for which data can be modeled is between 10 and 18.5 keV, depending on the column density. Details of the physics of the model, the approximations used and further details on the regimes of validity can be found in Yaqoob (1997; ApJ, 479, 184). In this particular incarnation, the initial spectrum is a power law modified by a high-energy exponential cut-off above a certain threshold energy.
Also, to improve the speed, a FAST option is available in which a full
integration over the input spectrum is replaced by a simple mean
energy shift for each bin. This option is obtained by setting
par9 to a value of 1 or greater and cannot be made
variable. Further, for single-scattering albedos less than the
critical albedo (i.e. par8) energy shifts are neglected
altogether. The recommended value for par8 is 0.1 which
corresponds to about 4 keV for cosmic abundances and is more than
adequate for ASCA data.
Note that for column densities in the range - cm, the maximum number of scatterings which need be considered for convergence of the spectrum of better than 1% is between 1 and 5. For column densities as high as cm, the maximum number of scatterings which need be considered for the same level of convergence is 12. This parameter cannot be made variable.
|par1||Column density in units cm|
|par2||Maximum number of scatterings to consider.|
|par4||Iron K edge energy.|
|par5||Power-law photon index.|
|par6||High-energy cut-off threshold energy.|
|par7||High-energy cut-off e-folding energy.|
|par8||Critical albedo for switching to elastic scattering.|
|par9||If par9 >1, function uses mean energy shift, not integration.|
|par10||Source redshift, z|