Signatures of dark matter halo expansion in galaxy populations
Entity
UAM. Departamento de Física TeóricaPublisher
Oxford University Press on behalf of the Royal Astronomical SocietyDate
2015-08-28Citation
10.1093/mnras/stv1699
Monthly Notices of Royal Astronomical Society 453.2 (2015): 2133-2143
ISSN
0035-8711 (print); 1365-2966 (online)DOI
10.1093/mnras/stv1699Funded by
CB thanks the MICINN (Spain) for the financial support through the MINECO grant AYA2012-31101 and the Ramon y Cajal program. ADC is supported by the DARK independent fellowship program.Project
Gobierno de España. AYA2012-31101Editor's Version
http://dx.doi.org/10. 1093/mnras/stv1699Subjects
Galaxies: evolution; Galaxies: formation; Galaxies: haloes; Cosmology: theory; Dark matter; FísicaNote
This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2015 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reservedRights
© 2015 The Authors: Published by Oxford University Press on behalf of the Royal Astronomical SocietyAbstract
Dark matter cores within galaxy haloes can be formed by energy feedback from star-forming regions: an energy balance suggests that the maximum core formation efficiency arises in galaxies with Mstar ~ 108.5M⊙. We show that a model population of galaxies, in which the density profile has been modified by such baryonic feedback, is able to explain the observed galaxy velocity function and Tully-Fisher relations significantly better than a model in which a universal cuspy density profile is assumed. Alternative models, namely warm or self-interacting dark matter, also provide a better match to these observed relations than a universal profile model does, but make different predictions for how halo density profiles vary with mass compared to the baryonic feedback case. We propose that the expected signatures of the mass dependence of core formation generated by baryonic feedback
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Google Scholar:Brook, Chris B.
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Di Cintio, Arianna
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