A broken power-law spectrum
multiplied by exponential high-energy cutoff, , 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
, 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 IREFLECT_PRECISION eg xset IREFLECT_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 |
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.} |