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THE DEGENERACY OF M33 MASS MODELING AND ITS PHYSICAL IMPLICATIONS

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journal contribution
posted on 18.06.2015, 13:08 by P. R. Hague, M. I. Wilkinson
The Local Group galaxy M33 exhibits a regular spiral structure and is close enough to permit high resolution analysis of its kinematics, making it an ideal candidate for rotation curve studies of its inner regions. Previous studies have claimed the galaxy has a dark matter halo with an Navarro-Frenk-White profile, based on statistical comparisons with a small number of other profiles. We apply a Bayesian method from our previous paper to place the dark matter density profile in the context of a continuous, and more general, parameter space. For a wide range of initial assumptions we find that models with inner log slope γin < 0.9 are strongly excluded by the kinematics of the galaxy unless the mass-to-light ratio of the stellar components in the 3.6 μm band satisfies Upsilon3.6 ≥ 2. Such a high Upsilon3.6 is inconsistent with current modeling of the stellar population of M33. This suggests that M33 is a galaxy whose dark matter halo has not been significantly modified by feedback. We discuss possible explanations of this result, including ram pressure stripping during earlier interactions with M31.

Funding

M.I.W. acknowledges the Royal Society for support through a University Research Fellowship. P.R.H. acknowledges STFC for financial support. This research used the Complexity HPC cluster at Leicester, which is part of the DiRAC2 national facility, jointly funded by STFC and the Large Facilities Capital Fund of BIS.

History

Citation

Astrophysical Journal, 2015, 800 (1)

Author affiliation

/Organisation/COLLEGE OF SCIENCE AND ENGINEERING/Department of Physics and Astronomy

Version

VoR (Version of Record)

Published in

Astrophysical Journal

Publisher

American Astronomical Society, IOP Publishing

issn

0004-637X

eissn

1538-4357

Copyright date

2015

Available date

18/06/2015

Publisher version

http://iopscience.iop.org/0004-637X/800/1/15/

Language

en