|AHELP for CIAO 4.5 Sherpa v1||
E-folded broken power law reflected from neutral matter. XSpec model.
Broken power law spectrum multiplied by exponential high-energy cutoff Exp[-E/foldE] , and reflected from neutral material. See Magdziarz and Zdziarski 1995, MNRAS, 273, 837 for details. 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 abundance are variable with respect to those set by a command set_xsabund. The opacities are of Balucinska and McCammon (1992 and 1994, private communication). 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 BEXRAV_PRECISION, e.g., 'xset BEXRAV_PRECISION 0.05' (see 'ahelp set_xsxset'). 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)|
|6||cosincl||cosine of inclination angle|
|7||abund||abundance of elements heavier than He relative to the solar abundances|
|8||fe_abund||iron abundance relative to the above|
|10||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 12.7.1 of the XSpec models is supplied with CIAO 4.4.1.
For a list of known bugs and issues with the XSPEC models, please visit the XSPEC bugs page.
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