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HI and Hot Gas in the Outskirts of the M81 Group

Published online by Cambridge University Press:  26 May 2016

M. Bureau ,
F. Walter ,
J. van Gorkom  and
C. Carignan
M. Bureau
Affiliation:
Hubble Fellow, Columbia Astrophysics Laboratory, 550 West 120th Street, 1027 Pupin Hall, Mail Code 5247, New York, NY 10027, U.S.A.
F. Walter
Affiliation:
Jansky Fellow, NRAO, P.O. Box O, Socorro, NM 87801, U.S.A.
J. van Gorkom
Affiliation:
Department of Astronomy, Columbia University, 538 West 120th Street, New York, NY 10027, U.S.A.
C. Carignan
Affiliation:
Département de Physique, Université de Montréal, C.P. 6128, Succ. Centre-Ville, Montréal, QC H3C 3J7, Canada

Abstract

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Results are presented from a wide area, high resolution HI synthesis survey of the outer regions of the nearby M81 group, where internal (galactic) and external (group-related) evolution processes can be studied simultaneously in great detail. The survey encompasses the star forming dwarf galaxies M81dwA, UGC4483, and HoII, where evidence of ram pressure stripping was recently discovered. The data do not reveal any intergalactic HI, but the outer parts of HoII are reminiscent of tidal tails. We argue however that those structures are equally consistent with the latest ram pressure models including cooling. The case for a hot intergalactic medium in this poor, spiral-only group is thus still open. The survey also puts tight constraints on possible counterparts to the local high velocity cloud population in an external group, reaching a 3σ column density of 1019 atom cm−2 and a 6σ limiting mass of 1.5 × 105M⊙.

Type
Part 3. Ejection and Outflow
Information
Symposium - International Astronomical Union , Volume 217: Recycling Intergalactic and Interslettar Matter , 2004 , pp. 452 - 457
Copyright
Copyright © Astronomical Society of the Pacific 2004 

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