A broken power-law spectrum multiplied by exponential high-energy cutoff, exp(-E/Ec), and reflected from ionized material. See Magdziarz & 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 . Then the actual reflection normalization is . Note that you need to change then the limits of excluding zero (as then the direct component appears). If , there is no cutoff in the power law. The metal and iron abundance are variable with respect to those set by the command abund.
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 eg xset BEXRIV_PRECISION 0.05. The default precision is 0.01 (ie 1%).
|par1||, first power law photon index|
|par2||, break energy (keV)|
|par3||, second power law photon index|
|par4||, the e-folding energy in keV (if there is no cutoff)|
|par5||, reflection scaling factor (1 for isotropic source above disk)|
|par7||abundance of elements heavier than He relative to the solar abundances|
|par8||iron abundance relative to the above|
|par9||cosine of inclination angle|
|par10||disk temperature (K)|
|par11||disk ionization parameter, , where is the 5eV-20keV irradiating flux and is the density of the reflector; see Done et al. 1992, ApJ 395, 275.|
|norm||photon flux at 1 keV of the cutoff broken power-law only (no reflection) in the observed frame.|