2009/09/03 by Virginia A. Kilborn, Duncan A. Forbes, David G. Barnes +4 · 4 citations
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics and Star Formation Studies #Content (measure theory) #Galaxies: Formation, Evolution, Phenomena #Galaxy #Galaxy group #Hydrogen #Luminosity #Luminosity function #Luminous infrared galaxy #Spiral galaxy #astro-ph.CO
paper · pdf · doi:10.1111/j.1365-2966.2009.15587.x
accepted for publication in MNRAS, 26 pages, 13 Figures, 2 Appendices
arxiv created 2009/09/03 · openalex publication_date 2009/11/11 · arxiv updated 2015/05/14 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We investigate the neutral hydrogen (H <scp>i</scp>) content of 16 groups for which we have multiwavelength data including X-ray observations. Wide-field imaging of the groups was obtained with the 20-cm multibeam system on the 64-m Parkes telescope. We have detected 10 previously uncatalogued H <scp>i</scp> sources, one of which has no visible optical counterpart. We examine the H <scp>i</scp> properties of the groups, compared to their X-ray characteristics, finding that those groups with a higher X-ray temperature and luminosity contain less H <scp>i</scp> per galaxy. The H <scp>i</scp> content of a group depends on its morphological make-up, with those groups dominated by early-type galaxies containing the least total H <scp>i</scp>. We determined the expected H <scp>i</scp> for the spiral galaxies in the groups, and found that a number of the galaxies were H <scp>i</scp> deficient. The H <scp>i</scp> deficient spirals were found both in groups with and without a hot intragroup medium. The H <scp>i</scp> deficient galaxies were not necessarily found at the centre of the groups, however, we did find that two-thirds of H <scp>i</scp> deficient galaxies were found within about 1 Mpc from the group centre, indicating that the group environment is affecting the gas loss from these galaxies. We determined the H <scp>i</scp> mass function for a composite sample of 15 groups, and found that it is significantly flatter than the field H <scp>i</scp> mass function. We also find a lack of high H <scp>i</scp> mass galaxies in groups. One possible cause of this effect is the tidal stripping of H <scp>i</scp> gas from spiral galaxies as they are pre-processed in groups.