Hostname: page-component-8448b6f56d-c47g7 Total loading time: 0 Render date: 2024-04-23T10:21:06.622Z Has data issue: false hasContentIssue false
  • English
  • Français

An H I Census of Loose Groups of Galaxies

Published online by Cambridge University Press:  26 May 2016

D. J. Pisano ,
David G. Barnes ,
Brad K. Gibson ,
Lister Staveley-Smith  and
Ken C. Freeman
D. J. Pisano
Affiliation:
NSF Distinguished International Postdoctoral Research Fellow, ATNF, P.O. Box 76, Epping NSW 1710, Australia
David G. Barnes
Affiliation:
School of Physics, Univ. of Melbourne, Victoria 3010, Australia
Brad K. Gibson
Affiliation:
Swinburne University of Technology, Centre for Astrophysics and Supercomputing, Mail # 31, P.O. Box 218, Hawthorn, Victoria 3122, Australia
Lister Staveley-Smith
Affiliation:
ATNF, P.O. Box 76, Epping NSW 1710, Australia
Ken C. Freeman
Affiliation:
RSAA, Mount Stromlo Observatory, Cotter Road, Weston, ACT 2611, Australia

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We present results from our Parkes Multibeam H I survey of 3 loose groups of galaxies that are analogous to the Local Group. This is a survey of groups containing only spiral galaxies with mean separations of a few hundred kpc, and total areas of approximately 1 Mpc2; groups similar to our own Local Group. We present a census of the H I-rich objects in these groups down to a 1σ MHI sensitivity ~7×105M⊙, as well as the detailed properties of these detections from follow-up Compact Array observations. We found 7 new H I-rich members in the 3 groups, all of which have stellar counterparts and are, therefore, typical dwarf galaxies. The ratio of low-mass to high-mass gas-rich galaxies in these groups is less than in the Local Group meaning that the “missing satellite” problem is not unique. No high-velocity cloud analogs were found in any of the groups. If HVCs in these groups are the same as in the Local Group, this implies that HVCs must be located within ~300-400 kpc of the Milky Way.

Type
Part 1. Census
Information
Symposium - International Astronomical Union , Volume 217: Recycling Intergalactic and Interslettar Matter , 2004 , pp. 20 - 25
Copyright
Copyright © Astronomical Society of the Pacific 2004 

References

Barnes, D.G. 2001, MNRAS, 322, 486.CrossRefGoogle Scholar
Blitz, L., Spergel, D., Teuben, P.J., Hartmann, D., Burton, W.B. 1999, ApJ, 514, 818.Google Scholar
Braun, R., Burton, W.B. 1999, A&A, 351, 437.Google Scholar
de Heij, V., Braun, R., Burton, W.B. 2002a, A&A, 391, 67.Google Scholar
de Heij, V., Braun, R., Burton, W.B. 2002b, A&A, 392, 417.Google Scholar
Garcia, A.M. 1993, A&AS, 100, 47.Google Scholar
Klypin, A.A., Kravtsov, A.V., Valenzuela, O., Prada, F. 1999, ApJ, 522, 82.Google Scholar
Lockman, F.J. 2003, ApJ, 591, L33.Google Scholar
Mateo, M. 1998, ARA&A, 36, 435.Google Scholar
Moore, B., Ghigna, S., Governato, F., Lake, G., Quinn, T., Stadel, J. 1999, ApJ, 524, L19.CrossRefGoogle Scholar
Putman, M.E., et al. 2002, AJ, 123, 873.Google Scholar
Tully, R.B. 1987, ApJ, 321, 280.Google Scholar
Zabludoff, A.I., Mulchaey, J.S. 1998, ApJ, 498, L5.CrossRefGoogle Scholar