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HI Rotation Curves of Galaxies

Published online by Cambridge University Press:  04 August 2017

R. Sancisi  and
T. S. van Albada
R. Sancisi
Affiliation:
Kapteyn Astronomical Institute, Groningen University, The Netherlands
T. S. van Albada
Affiliation:
Kapteyn Astronomical Institute, Groningen University, The Netherlands

Abstract

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The observational evidence on the discrepancy between the mass distribution in galaxies derived from HI rotation curves and that derived from the distribution of light is reviewed. In the outer parts the discrepancy is such that in some galaxies there is at least three times as much dark matter as luminous matter. This is a direct consequence of the nearly constant circular velocity far beyond the edge of the visible part of the galaxy, as derived from the motion of HI. The discrepancy is clearly present already near the edge of the visible disk (R25). In the inner regions, i.e. inside approximately 2.5 disk scale-lengths, no dark matter is required, but its presence can not be ruled out. There is no evidence for a dependence on galaxy luminosity or morphological type. These results suggest a strong coupling between luminous matter and dark matter within individual galaxies, and among galaxies as well. Finally attention is drawn to the large-scale asymmetries in the outer parts of galaxies and to possible implications for the vertical distribution of dark matter.

Type
Review Paper
Information
Symposium - International Astronomical Union , Volume 117: Dark Matter in the Universe , 1987 , pp. 67 - 81
Copyright
Copyright © Reidel 1987 

References

Bahcall, J.N. 1984, Astrophys. J. 287, 926.Google Scholar
Bahcall, J.N., and Casertano, C. 1985, Astrophys. J. 293, L7.Google Scholar
Baldwin, J.E., Lynden-Bell, D., and Sancisi, R. 1980, Mon. Not. R. Astr. Soc. 193, 313.Google Scholar
Begeman, K. 1985, in preparation.Google Scholar
Bosma, A. 1981, Astron. J. 86, 1791.Google Scholar
Carignan, C., and Freeman, K.C. 1985, Astrophys. J. 294, 494.Google Scholar
Carignan, C., Sancisi, R., and van Albada, T.S. 1985, in preparation.Google Scholar
Casertano, S. 1983, Mon. Not. R. Astr. Soc. 203, 735.Google Scholar
Faber, S.M., and Gallagher, J.S. 1979, Ann. Rev. Astron. Astrophys. 17, 135.Google Scholar
Jensen, E.B., and Thuan, T.X. 1982, Astrophys. J. Suppl. 50, 421.Google Scholar
Larson, R.B., and Tinsley, B.M. 1978, Astrophys. J. 219, 46.Google Scholar
Roelfsema, P.R., and Allen, R.J. 1985, Astron. Astrophys. 146, 213.Google Scholar
Rubin, V.C., Ford, W.K. Jr., and Thonnard, N. 1980, Astrophys. J. 238, 471.Google Scholar
Rubin, V.C., Burstein, D., Ford, W.K. Jr., and Thonnard, N. 1985, Astrophys. J. 289, 81.Google Scholar
Sancisi, R., and Allen, R.J. 1979, Astron. Astrophys. 74, 73.Google Scholar
van Albada, T.S., Bahcall, J.N., Begeman, K., and Sancisi, R. 1985, Astrophys. J. 295, 305.Google Scholar
van der Kruit, P.C., and Searle, L. 1981, Astron. Astrophys. 95, 105.Google Scholar
van der Kruit, P.C. 1981, Astron. Astrophys. 99, 298.Google Scholar
Wevers, B.M.H.R. 1984, , Groningen University.Google Scholar