An XMM-Newton Observation of the Bright Seyfert 2 Galaxy NGC 6300

Details An XMM-Newton Observation of the Bright Seyfert 2 Galaxy NGC 6300 An XMM-Newton Observation of the Bright Seyfert 2 Galaxy NGC 6300

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aas...201.4821m&link_type=abstract

American Astronomical Society, 201st AAS Meeting, #48.21; Bulletin of the American Astronomical Society, Vol. 34, p.1183

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We present preliminary results from an XMM-Newton observation of the bright, nearby (18 Mpc) Seyfert 2 galaxy NGC 6300. We observe diffuse soft (0.1--2 keV) X-ray emission extended on a scale of ~ 2 arcmin, corresponding to the scale of the host ring galaxy. Two soft X-ray sources within 80 arcseconds of the nucleus were found; if associated with the galaxy, their 0.2--10 keV luminosity is 1--5x 1039 erg s-1. They may be ultraluminous compact X-ray sources, similar to those discovered in other nearby galaxies. The fainter of the two objects seems to correspond to a source of UV emission observed by the XMM-Newton optical monitor. The X-ray spectrum of the active nucleus is a rather typical one for a Compton-thin Seyfert 2 galaxy. It consists of a heavily absorbed, strongly-variable hard component dominating the 3--10 keV band, and a soft component dominating the 0.2--1.7 keV band. In the 3--10 keV band, the spectrum is well fitted by a power-law model (Γ 3-10keV ~= 1.9) seen through a Compton-thin (NH ~= 2.1 x 1023 cm-2) absorber. We confirm the presence of a K{≻ α } fluorescence neutral iron line with a centroid at EFe = 6.42 keV and an equivalent width EWFe ~= 150 +/- 20 eV. The iron line may be marginally resolved. The observed flux in the 2--10 keV band is F ~= 7 x 10-12 ergs cm-2 s-1, comparable to the flux observed by BeppoSAX two years earlier. The spectrum in the 0.2--1.7 keV band is well fitted by a power-law (Γ {0.2-1.7 keV} ~= 1.9), attenuated only by the gas in our Galaxy.

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