University of Surrey

Test tubes in the lab Research in the ATI Dance Research

Dark matter cores all the way down

Read, JI, Agertz, O and Collins, MLM (2016) Dark matter cores all the way down Monthly Notices of the Royal Astronomical Society, 459. pp. 2573-2590.

MNRAS-2016-Read-2573-90.pdf - Version of Record

Download (6MB) | Preview
Text (licence)
Available under License : See the attached licence file.

Download (33kB) | Preview
[img] Text
DMcore_all_way_down updated.pdf - Accepted version Manuscript
Restricted to Repository staff only

Download (3MB)
[img] Text
DMcore_all_way_down.pdf - Accepted version Manuscript
Restricted to Repository staff only
Available under License : See the attached licence file.

Download (3MB)


We use high resolution simulations of isolated dwarf galaxies to study the physics of dark matter cusp-core transformations at the edge of galaxy formation: M200 = 107 109M .We work at a resolution ( 4 pc minimum cell size; 250M per particle) at which the impact from individual supernovae explosions can be resolved, becoming insensitive to even large changes in our numerical `sub-grid' parameters. We nd that our dwarf galaxies give a remarkable match to the stellar light pro le; star formation history; metallicity distribution function; and star/gas kinematics of isolated dwarf irregular galaxies. Our key result is that dark matter cores of size comparable to the stellar half mass radius r1=2 always form if star formation proceeds for long enough. Cores fully form in less than 4 Gyrs for the M200 = 108M and 14 Gyrs for the 109M dwarf. We provide a convenient two parameter `coreNFW' tting function that captures this dark matter core growth as a function of star formation time and the projected stellar half mass radius. Our results have several implications: (i) we make a strong prediction that if CDM is correct, then `pristine' dark matter cusps will be found either in systems that have truncated star formation and/or at radii r > r1=2; (ii) complete core formation lowers the projected velocity dispersion at r1=2 by a factor 2, which is su cient to fully explain the `too big to fail problem'; and (iii) cored dwarfs will be much more susceptible to tides, leading to a dramatic scouring of the subhalo mass function inside galaxies and groups.

Item Type: Article
Subjects : subj_Physics
Divisions : Faculty of Engineering and Physical Sciences > Physics
Authors :
Read, JI
Agertz, O
Collins, MLM
Date : 28 March 2016
DOI : 10.1093/mnras/stw713
Copyright Disclaimer : This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2016 The authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
Uncontrolled Keywords : astro-ph.GA, astro-ph.GA, astro-ph.CO
Related URLs :
Depositing User : Symplectic Elements
Date Deposited : 03 May 2016 11:45
Last Modified : 31 Oct 2017 18:16

Actions (login required)

View Item View Item


Downloads per month over past year

Information about this web site

© The University of Surrey, Guildford, Surrey, GU2 7XH, United Kingdom.
+44 (0)1483 300800