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“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: sap@sao.ru
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Abstract

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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

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