Table 1
Photon distributions of the phenomenological models used in the spectral analysis.
| XSPEC model | Photon energy distribution |
|
|
|
| PHABS | A(E) = e− NHσMM(E) |
| CUTOFFPL | C(E) = KE− Γe− E/Ecut |
| POWER | P(E) = KE− Γ |
| HIGHECUT |
|
| GAUSS |
|
| GABS |
|
| EDGE |
|
| COMPTT | See Titarchuk (1994), Hua & Titarchuk (1995) |
| COMPMAG | See Farinelli et al. (2012) |
Notes. σMM(E): 0.03−10 keV interstellar photoelectric absorptioncross-section (Morrison & McCammon 1983). NH: equivalent hydrogen column. K: normalisation in photons keV-1 cm-2 s-1 at 1 keV. Γ: power-law photon index. Ecut: cut-off energy in keV. Efold: folding energy in keV. El: iron line energy in keV. σ: iron line width in keV. K1: total photons cm-2 s-1 in the line. E0: central energy of the absorption line in keV. σ0: width of the absorption line in keV. 
, optical depth of the absorption line. Ec: threshold energy. D: absorption depth at the threshold.
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