X-ray Emission from Megamaser Galaxy IC 2560

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Observation of the H{sub 2}O megamaser galaxy IC 2560 with the Chandra Observatory reveals a complex spectrum composed of soft X-ray emission due to multi-temperature thermal plasma, and a hard continuum with strong emission lines. The continuum is most likely a Compton reflection (reprocessing) of primary emission that is completely absorbed at least up to 7 keV. The lines can be identified with fluorescence from Si, S and Fe in the lowest ionization stages. The equivalent widths of the Si and S lines are broadly compatible with those anticipated for reprocessing by optically thick cold plasma of Solar abundances, while ... continued below

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Madejski, Greg; /SLAC /KIPAC, Menlo Park; Done, Chris; U., /Durham; Zycki, Piotr; /Warsaw, Copernicus Astron. Ctr. et al. September 12, 2005.

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Observation of the H{sub 2}O megamaser galaxy IC 2560 with the Chandra Observatory reveals a complex spectrum composed of soft X-ray emission due to multi-temperature thermal plasma, and a hard continuum with strong emission lines. The continuum is most likely a Compton reflection (reprocessing) of primary emission that is completely absorbed at least up to 7 keV. The lines can be identified with fluorescence from Si, S and Fe in the lowest ionization stages. The equivalent widths of the Si and S lines are broadly compatible with those anticipated for reprocessing by optically thick cold plasma of Solar abundances, while the large equivalent width of the Fe line requires some overabundance of iron. A contribution to the line from a transmitted component cannot be ruled out, but the limits on the strength of the Compton shoulder make it less likely. From the bolometric luminosity of the nuclear region, we infer that the source radiates at 1-10% of its Eddington luminosity, for an adopted central mass of 3 x 10{sup 6} M{sub {circle_dot}}. The overall spectrum is consistent with the hypotheses that the central engines powering the detected megamsers in accretion disks are obscured from direct view by the associated accretion disk material itself, and that there is a correlation between the occurrence of megamaser emission and Compton-thick absorption columns. For the 11 known galaxies with both column density measurements and maser emission believed to arise from accretion disks, eight AGN are Compton thick.

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  • Journal Name: Astrophysical Journal; Journal Volume: 636

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  • Report No.: SLAC-PUB-11469
  • Grant Number: AC02-76SF00515
  • Office of Scientific & Technical Information Report Number: 878419
  • Archival Resource Key: ark:/67531/metadc876734

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  • September 12, 2005

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  • Sept. 21, 2016, 2:29 a.m.

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  • Dec. 9, 2016, 9:01 p.m.

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Madejski, Greg; /SLAC /KIPAC, Menlo Park; Done, Chris; U., /Durham; Zycki, Piotr; /Warsaw, Copernicus Astron. Ctr. et al. X-ray Emission from Megamaser Galaxy IC 2560, article, September 12, 2005; [Menlo Park, California]. (digital.library.unt.edu/ark:/67531/metadc876734/: accessed October 23, 2018), University of North Texas Libraries, Digital Library, digital.library.unt.edu; crediting UNT Libraries Government Documents Department.