1999A&A...344..755K

We present results from an analysis of the X-ray properties of the NGC 383 galaxy group based on ROSAT PSPC and HRI data. X-ray emission can be traced out to ∼1h₅₀^–1Mpc, the estimated virial radius of the system. We determine a total mass of 610¹³h₅₀^–1M_☉ for the group inside this radius with a gas mass fraction of 21%. The intragroup gas temperature of 1.5keV is both consistent with the galaxy velocity dispersion and the X-ray luminosity - temperature relation of groups and clusters suggesting that the group is fairly relaxed. This is also indicated by the almost spherically symmetric appearance of the group's X-ray halo. The X-ray properties of the radio galaxy NGC 383 (3C 31) which is located near the center of the group are discussed. Its spectrum is best described by a two-component model, consisting of emission from a low-temperature Raymond-Smith plasma, and a hard tail. The emission from NGC 383 is not resolved by the ROSAT HRI. The possible interaction of the radio jets of 3C 31 with the IGM is studied. A spatial, spectral and temporal analysis of the Einstein source 1E 0104+3153 located within the field of view is performed, one goal being the identification of the optical counterpart (with both, a high-redshift BAL quasar and a nearby elliptical galaxy, member of a small group, located within the Einstein X-ray error circle). We find evidence that the IGM of the small group contributes significantly to the X-ray emission of 1E 0104+3153, which can be described by a Raymond-Smith model of kT≃2keV and a soft X-ray luminosity of L_x≃3x10⁴³erg/s.