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Vertical Motion and the Thickness of Hi Disks: Implications for Galactic Mass Models

Published online by Cambridge University Press:  04 August 2017

P. C. van der Kruit  and
G. S. Shostak
P. C. van der Kruit
Affiliation:
Kapteyn Astronomical Institute, University of Groningen, the Netherlands
G. S. Shostak
Affiliation:
Kapteyn Astronomical Institute, University of Groningen, the Netherlands

Extract

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Most studies of the mass distribution in spiral galaxies have been based on the observed rotation curves. A serious ambiguity in this approach has always been that the rotation curve contains in itself no information on the mass distribution in the direction perpendicular to the galactic plane. The usual assumption has been that the mass in late type galaxies is distributed as the light, namely outside the central bulge in a highly flattened disk. In recent years it has been found that the rotation curves decline little or not at all, indicating large increases in the local value of M/L with increasing galactocentric radius (e.g. Bosma and van der Kruit, 1979). On the basis of dynamical arguments involving stability it has been suspected that the material giving rise to the large values of M/L - the “dark matter” - is distributed in the halos of these galaxies, so that the assumption of a flat mass distribution would have to be wrong.

Type
I. Kinematics of Gas and the Underlying Mass Distribution
Information
Symposium - International Astronomical Union , Volume 100: Internal Kinematics and Dynamics of Galaxies , 1983 , pp. 69 - 76
Copyright
Copyright © Reidel 1983 

References

Baldwin, J.E. 1980, The Structure and Evolution of Normal Galaxies (ed. Lynden-Bell, D. and Fall, S.M.), Cambridge Univ. Press, p. 137.Google Scholar
Boroson, T. 1981, Ap. J. Suppl. 46, 177.Google Scholar
Bosma, A., Kruit, P.C. van der 1979, Astron. Astrophys. 79, 281.Google Scholar
Briggs, F.H. 1982, preprint.Google Scholar
Celnick, W., Rohlfs, K. Braunsfurth, E. 1979, Astron. Astrophys. 76, 24.Google Scholar
Jackson, P.D., Kellman, S.A. 1974, Ap. J. 190, 53.Google Scholar
Kruit, P.C. van der 1981, Astron. Astrophys. 99, 298.Google Scholar
Kruit, P.C. van der, Searle, L. 1981a, Astron. Astrophys. 95, 105 (KSI).Google Scholar
Kruit, P.C. van der, Searle, L. 1981b, Astron. Astrophys. 95, 116 (KSII).Google Scholar
Kruit, P.C. van der, Searle, L. 1982a, Astron. Astrophys. 110, 61 (KSIII).Google Scholar
Kruit, P.C. van der, Searle, L. 1982b, Astron. Astrophys. 110, 79 (KSIV).Google Scholar
Kruit, P.C. van der, Shostak, G.S. 1982 Astron. Astrophys. 105, 359.Google Scholar
Oort, J.H. 1965, Stars and Stellar Systems V: Galactic Structure (ed. Blaauw, A. and Schmidt, M.), Univ. of Chicago Press, p. 455.Google Scholar
Sancisi, R., Allen, R.J. 1979, Astron. Astrophys. 74, 73.Google Scholar