E-folded broken power law reflected from ionized matter. XSPEC model.
Broken power law spectrum multiplied by exponential high-energy cutoff, Exp[-E/foldE], and reflected from ionized material. See Magdziarz and Zdziarski 1995, MNRAS, 273, 837 for details. Ionization and opacities of the reflecting medium is computed as in the xsabsori midel. The output spectrum is the sum of an e-folded broken 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 need to change then the limits of relRefl excluding zero (as then the direct component appears). If foldE = 0, there is no cutoff in the power law. The metal and iron abundances are variable with respect to those set by the command set_xsabund.
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 BEXRIV_PRECISION, e.g.,
sherpa> set_xsxset('BEXRIV_PRECISION', '0.05')
The default precision is 0.01 (i.e., 1%).
This is an additive model component.
|1||Gamma1||first power law photon index|
|2||breakE||break energy (keV)|
|3||Gamma2||second power law photon index|
|4||foldE||the e-folding energy in keV (if foldE=0, there is no cutoff)|
|5||rel_refl||reflection scaling factor (1 for isotropic source above disk)|
|7||abund||abundance of elements heavier than He relative to the solar abundances|
|8||Fe_abund||iron abundance relative to the above|
|9||cosIncl||cosine of inclination angle|
|10||T_disk||disk temperature in K|
|11||xi||disk ionization parameter, xi = 4 pi F_ion/n, where F_ion is the 5 eV - 20 keV irradiating flux, n is the density of the reflector; see Done et al., 1992, ApJ, 395, 275|
|12||norm||photon flux at 1 keV of the cutoff broken power law only (no reflection) 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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