|AHELP for CIAO 4.5 Sherpa v1||
Neutral Compton reflection with self-consistent Fe and Ni lines. XSpec model.
This model from Nandra et al. (2007; MNRAS 382, 194) combines pexrav (see 'ahelp xspexrav') with self-consistently generated Fe K-alpha, Fe K-beta, Ni K-alpha and the Fe K-alpha Compton shoulder. Line strengths are based on Monte Carlo calculations by George and Fabian (1991; MNRAS 249, 352) which are parametrized for 1.1 < gamma < 2.5 by:
EW = 9.66 EW_0(gamma^(-2.8) - 0.56)
with inclination dependence 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 K-beta and Ni K-alpha line fluxes are 11.3% and 5% respectively of that for Fe K-alpha. The Fe K-alpha Compton shoulder is approximated as a gaussian with E = 6.315 keV and sigma = 0.035 keV. The inclination dependence is taken from Matt (2002; MNRAS 337, 147) such that :
EW_shoulder = EW_FeKalpha(0.1 + 0.1 cos i)
This is an additive model component.
|1||PhoIndex||power-law photon index, N_E prop. to E^(-PhoIndex)|
|2||foldE||cutoff energy in keV (if foldE = 0 there is no cutoff).|
|3||rel_refl||the scaling factor for reflection: < 0, no direct component; =1, isotropic source above the disk|
|5||abund||abundance of elements heavier than He relative to Solar|
|6||Fe_abund||iron abundance relative to Solar|
|7||Incl||cosine of the inclination angle|
|8||norm||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.|
This information is taken from the XSpec User's Guide. Version 12.7.1 of the XSpec models is supplied with CIAO 4.4.1.
For a list of known bugs and issues with the XSPEC models, please visit the XSPEC bugs page.
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