Exponentially cutoff power law reflected from neutral matter. XSPEC model.
Exponentially cutoff power law spectrum reflected from neutral material (Magdziarz and Zdziarski 1995, MNRAS, 273, 837). The output spectrum is the sum of an e-folded power law and the reflection component.
The reflection component alone can be obtained for relRefl < 0. Then the actual reflection normalization is |relRefl|. Note that you then need to change the limits of relRefl to exclude zero (as then the direct component appears). If foldE = 0 there is no cutoff in the power law.
The metal and iron abundance are variable with respect to those defined by the set_xsabund command. The opacities are those set by the set_xsxsect command. As expected in AGNs, H and He are assumed to be fully ionized.
The core of this model is a Greens' function integration with one numerical integral performed for each model energy. The numerical integration is done using an adaptive method which continues until a given estimated fractional precision is reached. The precision can be changed by setting PEXRAV_PRECISION, e.g.,
sherpa> set_xsxset('PEXRAV_PRECISION', '0.05')
The default precision is 0.01 (i.e., 1%).
This is an additive model component.
|1||PhoIndex||power law photon index, N_E prop. to E^(-PhoIndx)|
|2||foldE||the e-folding energy in keV (if foldE=0, there is no cutoff; change the lower limit for that)|
|3||rel_refl||reflection scaling factor; if < 0, there is no direct component; relRefl=1 for isotropic source above disk|
|5||abund||abundance of elements heavier than He relative to that defined by set_xsabund|
|6||Fe_abund||iron abundance relative to that defined by set_xsabund|
|7||cosIncl||cosine of inclination angle|
|8||norm||photon flux at 1 keV (photons/keV/cm^2/s) of the power law only in the observed frame|
This information is taken from the XSPEC User's Guide. Version 12.9.1n of the XSPEC models is supplied with CIAO 4.10.
For a list of known bugs and issues with the XSPEC models, please visit the XSPEC bugs page.
To check the X-Spec version used by Sherpa, use the get_xsversion routine from the xspec module:
sherpa> from sherpa.astro.xspec import get_xsversion sherpa> get_xsversion() '12.9.1n'
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