Hostname: page-component-586b7cd67f-t7fkt Total loading time: 0 Render date: 2024-11-26T04:52:32.012Z Has data issue: false hasContentIssue false
  • English
  • Français

Distribution and motions of HI in M31

Published online by Cambridge University Press:  04 August 2017

E. Brinks  and
W. B. Burton
E. Brinks
Affiliation:
Sterrewacht, Leiden, The Netherlands
W. B. Burton
Affiliation:
Sterrewacht, Leiden, The Netherlands

Extract

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.

It has become clear in the past few years that the distribution and kinematics of HI in M31 is far from simple. The new high-resolution survey made with the Westerbork SRT in the 21-cm line of atomic hydrogen by Brinks and Shane (1983) shows this dramatically. Along almost any line of sight through M31 two separate velocity systems are sampled. Based on a previous survey Shane (1978) and later Bajaja and Shane (1982) proposed that the extra component is due to warping of the plane of the galaxy into the direction of and crossing the line-of-sight. Roberts et al. (1978) and Whitehurst et al. (1978) emphasized that the observed profile structure ruled out confinement of the gas to a thin plane. Unwin (1983) reached a similar conclusion on the basis of his survey. The most complete model produced up until now which accounts for the two velocity systems is the one by Henderson (1979), based on the 100-m Effelsberg survey of M31 by Cram et al. (1980)

Type
PART II: COMPOSITION, STRUCTURE AND KINEMATICS
Information
Symposium - International Astronomical Union , Volume 106: The Milky Way Galaxy , 1985 , pp. 437 - 442
Copyright
Copyright © Reidel 1985 

References

Bajaja, E., Shane, W.W.: 1982, Astron. Astrophys. Suppl. 49, 745.Google Scholar
Brinks, E., Shane, W.W.: 1983, Astron. Astrophys. Suppl. (submitted).Google Scholar
Burton, W.B., Liszt, H.S.: 1978, Astrophys. J. 225, 815.Google Scholar
Byrd, G.G.: 1977, Astrophys. J. 218, 86.Google Scholar
Cram, T.R., Roberts, M.S., Whitehurst, R.N.: 1980, Astron. Astrophys. Suppl. 40, 215.Google Scholar
Emerson, D.T., Newton, K.: 1978, in “Structure and Properties of Nearby Galaxies” (IAU Symp. No. 77), eds. Berkhuijsen, E.M. and Wielebinski, R. (Reidel, Dordrecht), p. 183 Google Scholar
Henderson, A.P.: 1979, Astron. Astrophys. 75, 311.Google Scholar
Henderson, A.P., Jackson, P.D., Kerr, F.J.: 1982, Astrophys. J. 263, 116.Google Scholar
Kulkarni, S.R., Blitz, L., Heiles, C.: 1982, Astrophys. J. 259, L63.Google Scholar
Roberts, M.S., Whitehurst, R.N., Cram, T.R.: 1978, in “Structure and Properties of Nearby Galaxies” (IAU Symp. No. 77), eds. Berkhuijsen, E.M. and Wielebinski, R. (Reidel, Dordrecht), p. 169.Google Scholar
Sancisi, R.: 1983, in “Internal Kinematics and Dynamics of Galaxies” (IAU Symp. No. 100), ed. Athanassoula, E. (Reidel, Dordrecht), p. 55.Google Scholar
Shane, W.W.: 1978, in “Structure and Properties of Nearby Galaxies” (IAU Symp. No. 77), eds. Berkhuijsen, E.M. and Wielebinski, R. (Reidel, Dordrecht), p. 180.Google Scholar
Unwin, S.C.: 1983, Monthly Notices Roy. Astron. Soc. (preprint).Google Scholar
Whitehurst, R.N., Roberts, M.S., Cram, T.R.: 1978, in “Structure and Properties of Nearby Galaxies” (IAU Symp. No. 77), eds. Berkhuijsen, E.M. and Wielebinski, R. (Reidel, Dordrecht), p. 175.Google Scholar