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Hi-Shells in M31

Published online by Cambridge University Press:  04 August 2017

E. Brinks  and
E. Bajaja
E. Brinks
Affiliation:
Leiden Observatory, Leiden, The Netherlands
E. Bajaja
Affiliation:
Leiden Observatory, Leiden, The Netherlands

Extract

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Close inspection of the channel maps which make up the high resolution M31 HI-data set (Brinks, this volume) resulted in finding numerous shell structures and bubble-like regions. To avoid any bias in the interpretation we shall call holes, in the course of this contribution, all those structures where we find a deficiency of neutral gas. Some of the holes can be identified directly in a total surface density map of M31, but due to blending of the various velocity components, e.g. the warp, holes tend to loose contrast. Therefore the best way to search for the holes is by inspection of the full resolution channel maps (δα x δδ x δV = 24″ x 36″ x 8.2 km s−1).

Type
II. Spiral Structure
Information
Symposium - International Astronomical Union , Volume 100: Internal Kinematics and Dynamics of Galaxies , 1983 , pp. 139 - 140
Copyright
Copyright © Reidel 1983 

References

Brinks, E.: 1981, Astron. Astrophys. 95, L1.Google Scholar
Heiles, C.: 1979, Astrophys. J. 229, 533.Google Scholar
Meaburn, J.: 1980, Monthly Notices Roy. Astron. Soc. 192, 365.Google Scholar