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pexmon:  neutral Compton reflection with self-consistent Fe and Ni lines.

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 EW0-2.8 - 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.

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.


 

next up previous contents
Next: Pexrav Up: Additive Model Components Previous: Pegpwrlw