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Table 3.

Spectral fit results for the phenomenological model [(partcov*xstar500)*(xstar5000*pow + zgauss1 + zgauss2)].

2004 2008A 2008B 2009 2014A 2014B 2014C 2015
Power law emission: pow
Γ
N1 keV/10−4
Partially covering absorber: partcov*xstar500
NH/1022
log ξ
Cf (%)
Highly ionized absorber: xstar5000
NH/1022
log ξ
υout/c
Gaussian emission line: zgauss1
E (keV) ≡6.4
σ (eV)
I/(10−6) < 3.6 < 3.2 < 2.2
EW < 200 < 150 < 140
Gaussian emission line: zgauss2
E (keV)
σ (eV)
I/(10−5)
EW
MOS cross-calibration constant
C

Fit statistics χ2/ν = 2176/1888
Pnull = 4 × 10−6

Notes. Units: power-law normalization N1 keV [10−4 photons keV−1 cm−2 s−1]; column density NH [1022 cm−2]; ionization parameter ξ [erg cm s−1]; outflowing velocity υout [c]; Gaussian emission line centroid energy E [keV], width σ [eV], intensity I [10−5 photons cm−2 s−1], equivalent width (EW) [eV]; flux f [10−12 erg s−1 cm−2]; luminosity L [1043 erg s−1]. The parameters kept tied between different epochs are the highly ionized absorber ionization parameter and the Gaussian emission line widths and centroid energies. The unabsorbed flux is corrected for both intrinsic and Galactic absorptions, as is the luminosity.

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