Exponentially cut off power law
spectrum reflected from neutral material (Magdziarz & Zdziarski 1995,
MNRAS, 273, 837). The output spectrum is the sum of the cut-off 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 Ec = 0 there is no cutoff in the power
law. The metal and iron abundance are variable with respect to those defined 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 PEXRAV_PRECISION eg xset PEXRAV_PRECISION 0.05. The default precision is 0.01 (ie 1%).
|
par1 |
|
|
par2 |
Ec, cutoff energy (keV) (if Ec = 0 there is no cutoff) |
|
par3 |
relrefl, reflection scaling factor (0, no reflected component < relrefl < 1 for isotropic source above disk) |
|
par4 |
redshift, z |
|
par5 |
abundance of elements heavier than He relative to the solar abundances |
|
par6 |
iron abundance relative to that defined by abund |
|
par7 |
cosine of inclination angle |
|
norm |
photon flux at 1 keV (photons keV–1cm-2 s-1) of the cutoff broken power-law only (no reflection) in the observed frame. |
, first power law
photon index, 