We present detailed time-averaged X-ray spectroscopy in the 0.5–10 keV band of the Seyfert 1.9 galaxy NGC 2992 with the Suzaku X-ray Imaging Spectrometers ( XIS ) .
The source had a factor \sim 3 higher 2–10Â keV flux ( \sim 1.2 \times 10 ^ { -11 } erg cm ^ { -2 } s ^ { -1 } ) than the historical minimum and a factor \sim 7 less than the historical maximum .
The XIS spectrum of NGCÂ 2992 can be described by several components .
There is a primary continuum , modeled as a power-law with a photon index of \Gamma = 1.57 ^ { +0.06 } _ { -0.03 } that is obscured by a Compton-thin absorber with a column density of 8.0 ^ { +0.6 } _ { -0.5 } \times 10 ^ { 21 } cm ^ { -2 } .
There is another , weaker , unabsorbed power-law component ( modeled with the same slope as the primary ) , that is likely to be due to the primary continuum being electron-scattered into our line-of-sight by a region extended on a scale of hundreds of parsecs .
We measure the Thomson depth of the scattering zone to be \tau _ { es } = ( 0.073 \pm 0.021 ) / [ \Omega / 4 \pi ] , where \Omega / 4 \pi is the fraction of the sky covered by the zone ( as seen from the X-ray source ) that is visible to the observer .
An optically-thin thermal emission component , which probably originates in the same extended region , is included in the model and yields a temperature and luminosity of kT = 0.656 ^ { +0.088 } _ { -0.061 } Â keV and \sim 1.2 \pm 0.4 \times 10 ^ { 40 } erg s ^ { -1 } respectively .
We detect an Fe K emission complex which we model with broad and narrow lines and we show that the intensities of the two components are decoupled at a confidence level > 3 \sigma .
The broad Fe K \alpha line has an equivalent width of 118 ^ { +32 } _ { -61 }  eV and could originate in an accretion disk ( with inclination angle greater than \sim 30 ^ { \circ } ) around the putative central black hole .
The narrow Fe K \alpha line has an equivalent width of 163 ^ { +47 } _ { -26 }  eV and is unresolved ( FWHM < 4090 km s ^ { -1 } ) and likely originates in distant matter .
The absolute flux in the narrow line implies that the column density out of the line-of-sight could be much higher than measured in the line-of-sight , and that the mean ( historically-averaged ) continuum luminosity responsible for forming the line could be a factor of several higher than that measured from the data .
We also detect the Fe K \beta line ( corresponding to the narrow Fe K \alpha line ) with a high signal-to-noise ratio and describe a new robust method to constrain the ionization state of Fe responsible for the Fe K \alpha and Fe K \beta lines that does not require any knowledge of possible gravitational and Doppler energy shifts affecting the line energies .
For the distant line-emitting matter ( e.g .
the putative obscuring torus ) we deduce that the predominant ionization state is lower than Fe viii ( at 99 % confidence ) , conservatively taking into account residual calibration uncertainties in the XIS energy scale and theoretical and experimental uncertainties in the Fe K fluorescent line energies .
From the limits on a possible Compton-reflection continuum it is likely that the narrow Fe K \alpha and Fe K \beta lines originate in a Compton-thin structure .