NASA/IPAC EXTRAGALACTIC DATABASE
Date and Time of the Query: 2019-08-17 T09:58:43 PDT
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For refcode 2012MNRAS.425.2299S:
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NED Abstract

Copyright by Royal Astronomical Society. 2012MNRAS.425.2299S The link between the baryonic mass distribution and the rotation curve shape Swaters, R. A.; Sancisi, R.; van der Hulst, J. M.; van Albada, T. S. 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 H I 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, H I scaling appears to fail in the outer parts, possibly due to observational effects or ionization of H I. 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). Key words: galaxies: dwarf, galaxies: kinematics and dynamics, galaxies: spiral
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