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Mass-discrepancy acceleration relation : a natural outcome of galaxy formation in cold dark matter halos.

Ludlow, A. D. and Benítez-Llambay, A. and Schaller, M. and Theuns, T. and Frenk, C. S. and Bower, R. and Schaye, J. and Crain, R. A. and Navarro, J. F. and Fattahi, A. and Oman, K. A. (2017) 'Mass-discrepancy acceleration relation : a natural outcome of galaxy formation in cold dark matter halos.', Physical review letters., 118 (16). p. 161103.


We analyze the total and baryonic acceleration profiles of a set of well-resolved galaxies identified in the eagle suite of hydrodynamic simulations. Our runs start from the same initial conditions but adopt different prescriptions for unresolved stellar and active galactic nuclei feedback, resulting in diverse populations of galaxies by the present day. Some of them reproduce observed galaxy scaling relations, while others do not. However, regardless of the feedback implementation, all of our galaxies follow closely a simple relationship between the total and baryonic acceleration profiles, consistent with recent observations of rotationally supported galaxies. The relation has small scatter: Different feedback implementations—which produce different galaxy populations—mainly shift galaxies along the relation rather than perpendicular to it. Furthermore, galaxies exhibit a characteristic acceleration g † , above which baryons dominate the mass budget, as observed. These observations, consistent with simple modified Newtonian dynamics, can be accommodated within the standard cold dark matter paradigm.

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Publisher statement:Reprinted with permission from the American Physical Society: Ludlow A. D., Benítez-Llambay A., Schaller M., Theuns T., Frenk C. S., Bower R., Schaye J., Crain R. A. Navarro J. F., Fattahi A. & Oman K. A. (2017). Mass-Discrepancy Acceleration Relation: A Natural Outcome of Galaxy Formation in Cold Dark Matter Halos. Physical Review Letters 118(16): 161103 © 2017 by the American Physical Society. Readers may view, browse, and/or download material for temporary copying purposes only, provided these uses are for noncommercial personal purposes. Except as provided by law, this material may not be further reproduced, distributed, transmitted, modified, adapted, performed, displayed, published, or sold in whole or part, without prior written permission from the American Physical Society.
Date accepted:24 October 2016
Date deposited:18 July 2017
Date of first online publication:21 April 2017
Date first made open access:18 July 2017

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