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HI Distribution in Extreme Dwarf Irregulars and Dwarf Spheroidals

Published online by Cambridge University Press:  14 August 2015

Claude Carignan
Claude Carignan*
Affiliation:
Département de Physique and Observatoire Astronomique du Mont Mégantic, Université de Montréal, C.P. 6128, Suce “centre-ville”, Montréal, Québec, Canada H3C 3J7

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Recent studies (Puche & Westpfahl 1994, Young & Lo 1996) have shown that the distribution of HI in some extreme low luminosity dwarf irregular galaxies (e.g. M81dwA, Holmberg I, Leo A) tends to have a ring-like (or shell-like) distribution which suggests that a single burst of star formation could expell most of the remaining ISM (or at least a large fraction of it) from the system. In view of this, Puche & Westpfahl (1994) suggested that in dwarf spheroidal galaxies, the HI should be found at large radii since no young stellar population is observed in most of them.

References

Carignan, C., Demers, S. and Côté, S. (1991) ApJ, 381, L13 Google Scholar
Oosterloo, T., Da Costa, G.S. and Staveley-Smith, L. (1996) AJ, 112, 1969 Google Scholar
Puche, D. and Westpfahl, D. (1994) in ESO/OHP Workshop on Dwarf Galaxies, eds. Meylan, G. & Prugniel, P. (Garching: ESO), p. 273 Google Scholar
Young, L.M. and Lo, K.Y. (1996) ApJ, 462, 203 Google Scholar