This model from Nandra et al. (2007; MNRAS 382, 194) combines pexrav with self-consistently generated Fe Kα, Fe Kβ, Ni Kα and the Fe Kα Compton shoulder. Line strengths are based on Monte Carlo calculations by George and Fabian (1991; MNRAS 249, 352) which are parametrized for 1.1 < γ < 2.5 by :

EW =
9.66 EW_{0}(γ^{-2.8} - 0.56)

with inclination dependence for for i < 85 degrees :

EW =
EW_{0} (2.20 cos i - 1.749 (cos i)^{2} + 0.541(cos i)^{3})

and abundance dependence :

log
EW = log EW_{0} (0.0641 log A_{Fe} - 0.172 (log A_{Fe})^{2})

The Fe Kβ and Ni Kα line fluxes are 11.3% and 5% respectively of that for Fe Kα. The Fe Kα Compton shoulder is approximated as a gaussian with E = 6.315 keV and σ = 0.035 keV. The inclination dependence is taken from Matt (2002; MNRAS 337, 147) such that :

EW_{shoulder}
= EW_{Fe Kα}(0.1 + 0.1 cos i)

The model parameters are :

par1= γ power-law photon index, N_{E}
a E^{-γ}.

par2 = E_{c }cutoff
energy in keV (if E_{c }= 0 there is no cutoff).

par3 = scale the scaling factor for reflection;

< 0 => no direct component,

=1 => isotropic source above the disk

par4 = z redshift

par5 = A_{ } abundance
of elements heavier than He relative to Solar.

par6 = A_{fe}
iron abundance relative to Solar.

par7 = cos i cosine of the inclination angle.

K
normalization is the photon flux at 1 keV (photons/keV/cm^{2}/s) of the
cutoff

power law only (without reflection) and in the Earth frame.