NASA/IPAC EXTRAGALACTIC DATABASE
Date and Time of the Query: 2019-03-24 T08:07:09 PDT
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For refcode 2012A&A...541A..28T:
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2012A&A...541A..28T Seyfert's Sextet: where is the gas? Tamburri, S.; Trinchieri, G.; Wolter, A.; Sulentic, J.; Durbala, A.; Rosado, M. Abstract. Aims: Seyfert's Sextet (a.k.a HCG 79) is one of the most compact and isolated galaxy groups in the local Universe. It shows a prominent diffuse light component that accounts for ~50% of the total observed light. This likely indicates that the group is in an advanced evolutionary phase, which would predict a significant hot gaseous component. Previous X-ray observations had suggested a low luminosity for this system, but with large uncertainties and poor resolution. Methods: We present the results from a deep (70 ks), high resolution Chandra observation of Seyfert's Sextet, requested with the aim of separating the X-ray emission associated with the individual galaxies from that of a more extended inter-galactic component. We discuss the spatial and spectral characteristics of this group we derive with those of a few similar systems also studied in the X-ray band. Results: The high resolution X-ray image indicates that the majority of the detected emission does not arise in the compact group but is concentrated towards the NW and corresponds to what appears to be a background galaxy cluster. The emission from the group alone has a total luminosity of ~1 x 10^40^ erg s^-1^ in the (0.5-5) keV band. Most of the luminosity can be attributed to the individual sources in the galaxies, and only ~2 x 10^39^ erg s^-1^ is due to a gaseous component. However, we find that this component is also mostly associated with the individual galaxies of the Sextet, leaving little or no residual in a truly IGM component. The extremely low luminosity of the diffuse emission in Seyfert's Sextet might be related to its small total mass. Key words: galaxies: groups: general, galaxies: groups: individual: HGC 79, intergalactic medium, X-rays: galaxies
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