Journal Article

The link between the baryonic mass distribution and the rotation curve shape

R. A. Swaters, R. Sancisi, J. M. van der Hulst and T. S. van Albada

in Monthly Notices of the Royal Astronomical Society

Published on behalf of The Royal Astronomical Society

Volume 425, issue 3, pages 2299-2308
Published in print September 2012 | ISSN: 0035-8711
Published online September 2012 | e-ISSN: 1365-2966 | DOI: http://dx.doi.org/10.1111/j.1365-2966.2012.21599.x
The link between the baryonic mass distribution and the rotation curve shape

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Abstract

The observed rotation curves of disc galaxies, ranging from late-type dwarf galaxies to early-type spirals, can be fitted remarkably well simply by scaling up the contributions of the stellar and Hi discs. This ‘baryonic scaling model’ can explain the full breadth of observed rotation curves with only two free parameters. For a small fraction of galaxies, in particular early-type spiral galaxies, Hi scaling appears to fail in the outer parts, possibly due to observational effects or ionization of Hi. The overall success of the baryonic scaling model suggests that the well-known global coupling between the baryonic mass of a galaxy and its rotation velocity (known as the baryonic Tully–Fisher relation) applies at a more local level as well, and it seems to imply a link between the baryonic mass distribution and the distribution of total mass (including dark matter).

Keywords: galaxies: dwarf; galaxies: kinematics and dynamics; galaxies: spiral

Journal Article.  6656 words.  Illustrated.

Subjects: Astronomy and Astrophysics

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