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

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 rota...

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Bibliographic Details
Published in:Monthly notices of the Royal Astronomical Society 2012-09, Vol.425 (3), p.2299-2308
Main Authors: Swaters, R. A., Sancisi, R., van der Hulst, J. M., van Albada, T. S.
Format: Article
Language:English
Subjects:
Astrophysics
Atoms & subatomic particles
galaxies: dwarf
galaxies: kinematics and dynamics
galaxies: spiral
Mathematical models
Star & galaxy formation
Stars & galaxies
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Summary: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).
ISSN:0035-8711
1365-2966
DOI:10.1111/j.1365-2966.2012.21599.x