The nuclear environment of 3C 33 as observed by Chandra and XMM-Newton

Details The nuclear environment of 3C 33 as observed by Chandra and XMM-Newton The nuclear environment of 3C 33 as observed by Chandra and XMM-Newton

Sep 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009hrxs.confe..43t&link_type=abstract

"High Resolution X-ray Spectroscopy: Towards IXO, Proceedings of the international workshop held at the Mullard Space Science La

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FRII Narrow Line Radio Galaxies (NLRG) optically classified as High Excitation Galaxies (HEG) share with Seyfert 2s more spectral properties than one could imagine. First of all a heavily absorbed continuum (NH~10^23-^24 cm^-2) related to the bright accretion disk obscured by an oriented thick torus. This is signalled by the presence of a prominent Fe Kalpha line and the Compton reflection. At softer energies (0.5-2 keV) a soft unabsorbed tail is often detected. While for Seyfert 2s high resolution spectroscopy led to the interpretation of this excess as produced by extended gas photoionized by the central engine, the origin of the soft X-ray emission in radio galaxies is still matter of debate. At the beginning it was suggested that the soft excess is related to the jet emerging from the edge of the dusty torus. Recently, Chandra and XMM-Newton detected emission-lines produced by photoionized gas on two radio-loud objects, 3C 445 and 3C 234, opening a new way of interptetation of the soft excess. In this poster we present another case: the radio galaxy 3C 33. Although the poor statistics did not allow an RGS analysis, what we obtained with the Chandra ACIS and XMM-Newton PN cameras is encouraging and again points toward the photoionization scenario. The combination of better quality data and high resolution spectroscopy could firmly confirm these results.

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