Hostname: page-component-848d4c4894-8bljj Total loading time: 0 Render date: 2024-07-01T17:27:19.212Z Has data issue: false hasContentIssue false
  • English
  • Français

Intergalactic HI Clouds

Published online by Cambridge University Press:  26 May 2016

F. H. Briggs
F. H. Briggs*
Affiliation:
RSAA, Mount Stromlo Observatory, ANU Cotter Road, Weston Creek 2611 ACT, 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.

Neutral intergalactic clouds are so greatly out numbered by galaxies that their integral HI content is negligible in comparison to that contained in optically luminous galaxies. In fact, no HI cloud that is not associated with a galaxy or grouping of galaxies has yet been identified. This points to a causal relationship that relies on gravitational potentials that bind galaxies also being responsible for confining HI clouds to sufficient density that they can become self-shielding to the ionizing background radiation. Unconfined clouds of low density become ionized, but confined clouds find themselves vulnerable to instability and collapse, leading to star formation.

Type
Part 1. Census
Information
Symposium - International Astronomical Union , Volume 217: Recycling Intergalactic and Interslettar Matter , 2004 , pp. 26 - 33
Copyright
Copyright © Astronomical Society of the Pacific 2004 

References

Blitz, L. et al 1999, ApJ, 514, 818.CrossRefGoogle Scholar
Braun, R. and Burton, W.B. 1999, A&A, 341, 437.Google Scholar
Briggs, F.H. 1990, AJ, 100, 999.CrossRefGoogle Scholar
van Driel, W., & van Woerden, H. 1991, A&A, 243, 71.Google Scholar
Felton, J.E. 1985, Comments Astrophys., 11, 53.Google Scholar
Fisher, J.R., & Tully, R.B. 1975, A&A, 44, 151.Google Scholar
Fisher, J.R., & Tully, R.B. 1981, ApJL, 243, L21.Google Scholar
Giovanelli, R., & Haynes, M.P. 1989a, AJ, 97, 633.Google Scholar
Giovanelli, R., & Haynes, M.P. 1989b, ApJL, 346, L5.Google Scholar
Haehnelt, M., Steinmetz, M., Rauch, M. 1998, ApJ, 495, 647.CrossRefGoogle Scholar
Lo, K-Y., & Sargent, W.L.W. 1979,Google Scholar
Madgwick, D.S. et al 2002, MNRAS, 333, 133.Google Scholar
Oosterloo, T. et al. 2003, IAUS, 217, 108.Google Scholar
Prochaska, J.X., Wolfe, A.M. 1997, ApJ, 487, 73.CrossRefGoogle Scholar
Schneider, S.E., et al 1989, AJ, 97, 666.Google Scholar
Spitzer, L. 1978, Physical Processes in the Interstellar Medium, John Wiley & Sons: New York.)Google Scholar
Wolfe, A.M., et al 1986, ApJS, 61, 249.CrossRefGoogle Scholar
Zwaan, M.A., et al 1997, ApJ, 490, 173.CrossRefGoogle Scholar
Zwaan, M.A., & Briggs, F.H. 2000, ApJ, 530L, 61.Google Scholar
Zwaan, M.A. 2001, MNRAS, 325, 1142.CrossRefGoogle Scholar
Zwaan, M.A., et al, 2003, AJ, 125, 2842.CrossRefGoogle Scholar