A broken power-law spectrum multiplied by exponential high-energy cutoff, exp(-E/Ec), and reflected from neutral 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 |relrefl|. Note
that you need to change then the limits of 
excluding zero (as then the
direct component appears). If Ec = 0, 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 opacities are those set by the command
xsect. 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 eg xset BEXRAV_PRECISION 0.05. The default precision is 0.01 (ie 1%).
|
par1 |
|
|
par2 |
Ebreak, break energy (keV) |
|
par3 |
|
|
par4 |
Ec, the e-folding energy in keV (if Ec = 0 there is no cutoff) |
|
par5 |
relrefl, reflection scaling factor (1 for isotropic source above disk) |
|
par6 |
redshift, z |
|
par7 |
abundance of elements heavier than He relative to the solar abundances |
|
par8 |
iron abundance relative to the above |
|
par9 |
cosine of inclination angle |
|
norm |
photon flux at 1 keV of the cutoff broken power-law only (no reflection) in the observed frame.} |
, first power law
photon index
, second power law
photon index