Precision Fe Kalpha and Fe Kbeta Line Spectroscopy of the Seyfert 1.9 Galaxy NGC 2992 with Suzaku

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dc.creatorYaqoob, Tahir
dc.creatorMurphy, Kendrah D.
dc.creatorGriffiths, Richard E.
dc.creatorHaba, Yoshito
dc.creatorInoue, Hajime
dc.creatorItoh, Takeshi
dc.creatorKelley, Richard
dc.creatorKokubun, Motohide
dc.creatorMarkowitz, Alex
dc.creatorMushotzky, Richard
dc.creatorOkajima, Takashi
dc.creatorPtak, Andrew
dc.creatorReeves, James
dc.creatorSerlemitsos, Peter J.
dc.creatorTakahashi, Tadayuki
dc.creatorTerashima, Yuichi
dc.date2006-09-20
dc.date.accessioned2026-07-07T11:42:36Z
dc.date.available2026-07-07T11:42:36Z
dc.descriptionWe 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). We model the complex continuum in detail. There is an Fe K line emission complex that we model with broad and narrow lines and we show that the intensities of the two components are decoupled at a confidence level >3sigma. The broad Fe K line has an EW of 118 (+32,-61) eV and could originate in an accretion disk (with inclination angle greater than ~30 degrees). The narrow Fe Kalpha line has an EW of 163 (+47,-26) eV and is unresolved FWHM <4090 km/s) 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 narrow Fe Kbeta 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 Kalpha and Fe Kbeta 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 Kalpha and Fe Kbeta lines originate in a Compton-thin structure.
dc.descriptionAbstract is abridged. Accepted for publication in the Suzaku special issue of PASJ (November 2006). 18 pages, 6 figures
dc.identifierhttps://arxiv.org/abs/astro-ph/0609581
dc.identifierhttp://arxiv.org/abs/astro-ph/0609581
dc.identifierProg.Theor.Phys.Suppl.169:252-255,2007
dc.identifierdoi:10.1143/PTPS.169.252
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/200944
dc.subjectAstrophysics
dc.titlePrecision Fe Kalpha and Fe Kbeta Line Spectroscopy of the Seyfert 1.9 Galaxy NGC 2992 with Suzaku
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