Hostname: page-component-78c5997874-v9fdk Total loading time: 0 Render date: 2024-11-02T21:32:27.839Z Has data issue: false hasContentIssue false
  • English
  • Français

“Dark Galaxies” and Local Very Metal-Poor Gas-Rich Glaxies: Possible Interrelations

Published online by Cambridge University Press:  01 June 2007

Simon A. Pustilnik
Simon A. Pustilnik*
Affiliation:
Special Astrophysical Observatory, Russian Academy of Sciences, Nizhnij Arkhyz, Karachai-Circassia, 369167, Russia email: [email protected]
Rights & Permissions [Opens in a new window]

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.

There are only a few “dark galaxy” candidates discovered to date in the local Universe. One of the most prominent of them is the SW component of a merging system HI 1225+01. On the other hand, the number of known very metal-poor gas-rich dwarfs similar to I Zw 18 and SBS 0335–052 E, W has grown drastically during the last decade, from a dozen and a half to about five dozen. Many of them are very gas-rich, having from ~90 to 99% of all baryons in gas. For some of such objects that have the deep photometry data, no evidences for the light of old stars are found. At least a half of such galaxies with the prominent starbursts have various evidences of interactions, including advanced mergers. This suggests that a fraction of this group objects can be a kind of very stable protogalaxies (or “dark galaxies”), which have recently experienced strong disturbances from nearby massive galaxy-size bodies. Such a collision caused the gas instabilities and its collapse with the subsequent onset of starburst. We briefly discuss the morphology and gas kinematics for the subsample of the most metal-poor dwarfs that illustrate this picture. We discuss also the relation of these rare galaxies to the processes by which “dark galaxies” can occasionally transform to optically visible galaxies.

Keywords

Galaxies: formationevolutioninteractionsdwarfstarburstabundancespeculiar
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S244: Dark Galaxies and Lost Baryons , June 2007 , pp. 341 - 345
Copyright
Copyright © International Astronomical Union 2008

References

Chengalur, J. N., Giovanelli, R., & Haynes, M. P. 1991, AJ 109, 2415CrossRefGoogle Scholar
Davies, J. I., Disney, M. J., Minchin, R. F., Auld, R., & Smith, R. 2006, MNRAS 368, 1479CrossRefGoogle Scholar
Izotov, Y. I., Thuan, T. X., & Guseva, N. G. 2005, ApJ 632, 210CrossRefGoogle Scholar
Izotov, Y. I., Papaderos, P., Guseva, N. G., Thuan, T. X., & Fricke, K. J. 2006, A&A 454, 137Google Scholar
Izotov, Y. I., & Thuan, T. X. 2007, ApJ 665, 1115CrossRefGoogle Scholar
Klypin, A., Kravtsov, A. V., Valenzuela, O., & Prada, F. 1999, ApJ 552, 82CrossRefGoogle Scholar
Minchin, , et al. 2005, arXiv astro-ph/0508153Google Scholar
Mo, H., Mao, S., & White, S. 1998, MNRAS 295, 319CrossRefGoogle Scholar
Moore, B., Ghigna, S., Governato, F., et al. , 1999, ApJ 524, L19CrossRefGoogle Scholar
Putman, M. E., Bureau, M., Mould, J. R., Staveley-Smith, L., & Freeman, K. C. 1998, AJ 115, 2345CrossRefGoogle Scholar
Pustilnik, S. A., Kniazev, A. Y., Lipovetsky, V. L., & Ugryumov, A. V. 2001a, A&A 373, 24Google Scholar
Pustilnik, S. A., Brinks, E., Thuan, T. X., Lipovetsky, V. L., & Izotov, Y. I. 2001b, AJ 121, 1413CrossRefGoogle Scholar
Pustilnik, S. A., Kniazev, A. Y., Pramskij, A. G., & Ugryumov, A. V. 2003, Ap& SS, 284, 795Google Scholar
Pustilnik, S. A., Kniazev, A. Y., & Pramskij, A. G. 2005, A&A 443, 91Google Scholar
Pustilnik, S. A., Engels, D., Kniazev, A. Y., et al. , 2006, Astron. Lett. 32, 228CrossRefGoogle Scholar
Pustilnik, S. A., & Martin, J.-M. 2007, A&A 464, 859Google Scholar
Pustilnik, S. A., & Kniazev, A. Y. 2007, in: Combes, F. and Palous, J. (eds.) Galaxy Evolution Across the Hubble Time, Proc. of IAU Symp. 235, Cambridge: CUP, p. 238CrossRefGoogle Scholar
Robertson, B., Bullock, J. S., Cox, T. J., Di Mateo, T., Hernquist, L., Springel, V., & Yoshida, N. 2006, ApJ 645, 986CrossRefGoogle Scholar
Salzer, J. J., di Serego Alighieri, S., Matteucci, F., Giovanelli, R., & Haynes, M. 1991, AJ 101, 1258CrossRefGoogle Scholar
Schneider, S., Thuan, T. X., Magri, C., & Wadiak, J. E. 1991, ApJS 72, 245CrossRefGoogle Scholar
Skillman, E. D., Kennicutt, R., & Hodge, P. 1989, ApJ 347, 845Google Scholar
Springel, V., & Hernquist, L. 2005, ApJ 622, L9CrossRefGoogle Scholar
Taylor, E. & Webster, R. 2005, ApJ 634, 1067CrossRefGoogle Scholar
Trentham, N., Moeller, O., & Ramizrez-Ruiz, E. 2001, MNRAS 322, 658CrossRefGoogle Scholar
van Zee, L., Westpfahl, D., Haynes, M., & Salzer, J. J. 1998, AJ 115, 1000CrossRefGoogle Scholar
Verde, L., Peng Oh, S., & Jimenez, R. 2002, MNRAS 336, 541CrossRefGoogle Scholar
Walter, F., Skillman, E. D., & Brinks, E. 2005, ApJ 627, L105CrossRefGoogle Scholar