The results thus indicate removal of both hot and cold gas from the group members via a combination of ram pressure stripping and tidal interactions. Suggestive evidence is further seen for galaxies with close neighbors in position-velocity space to show relatively low H I content, consistent with tidal removal of H I. Six of the 20 H I-detected group members show H I evidence of ongoing interactions with other galaxies or with the intragroup medium. The H I results suggest moderate H I mass loss from the group members when compared to similar field galaxies. The X-ray data are consistent with efficient ram pressure stripping of the hot gas halos of early-type galaxies near the group core, but no X-ray tails are seen and the limited statistics preclude strong conclusions. There is indirect evidence that the hot gaseous halos of spiral galaxies.
The high hot-to-cold gas ratio in the cloud indicates a significant evaporation of the H i gas, probably by thermal conduction from the hotter cluster plasma with a sub-Spitzer rate. Our observations cover nearly all group members within a projected radius of 1.15 Mpc (~1.4 R vir) of the group center, down to a limiting X-ray luminosity and H I mass of 3 × 1039 erg s-1 and 2 × 108 M &sun, respectively. This is most easily explained by ram pressure stripping as the dwarfs move. It has a temperature of 0.89 keV and a mass of 4.5 × 10 8 M, exceeding the estimated H i gas mass.
Here we present extensive Chandra and Very Large Array mosaic observations of the hot and cold interstellar medium within the members of the nearby, X-ray bright NGC 2563 group, a prime target for studies of the role of gas stripping and interactions in relatively small host halos. The role of environmentally induced gas stripping in driving galaxy evolution in groups remains poorly understood. Zabludoff, Eric Wilcots, Paul Martini, Duane Lee, Timothy P. Hot and Cold Galactic Gas in the NGC 2563 Galaxy Group Type
0 kommentar(er)
