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 E_{c} = 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 |
, first power law photon index, _{} |
par2 |
E_{c}, cutoff energy (keV) (if E_{c} = 0 there is no cutoff) |
par3 |
rel_{refl}, reflection scaling factor (0, no reflected component < rel_{refl} < 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^{–1}cm^{-2 }s^{-1}) of the cutoff broken power-law only (no reflection) in the observed frame. |