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 EW0(γ-2.8 - 0.56)
with inclination dependence for for i < 85 degrees :
EW = EW0 (2.20 cos i - 1.749 (cos i)2 + 0.541(cos i)3)
and abundance dependence :
log EW = log EW0 (0.0641 log AFe - 0.172 (log AFe)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 :
EWshoulder = EWFe Kα(0.1 + 0.1 cos i)
The model parameters are :
par1= γ power-law photon index, NE a E-γ.
par2 = Ec cutoff energy in keV (if Ec = 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 = Afe iron abundance relative to Solar.
par7               the inclination angle (degrees).
K normalization is the photon flux at 1 keV (photons/keV/cm2/s) of the cutoff
power law only (without reflection) and in the Earth frame.