Shallow dark matter cusps in galaxy clusters

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dc.contributor.author Laporte, Chervin F. P. en_US
dc.contributor.author White, Simon D. M. en_US
dc.contributor.author Naab, Thorsten en_US
dc.contributor.author Ruszkowski, Mateusz en_US
dc.contributor.author Springel, Volker en_US
dc.date.accessioned 2012-07-12T17:25:22Z
dc.date.available 2013-09-03T15:38:27Z en_US
dc.date.issued 2012-07-21 en_US
dc.identifier.citation Laporte, Chervin F. P.; White, Simon D. M.; Naab, Thorsten; Ruszkowski, Mateusz; Springel, Volker (2012). "Shallow dark matter cusps in galaxy clusters." Monthly Notices of the Royal Astronomical Society 424(1). <http://hdl.handle.net/2027.42/92100> en_US
dc.identifier.issn 0035-8711 en_US
dc.identifier.issn 1365-2966 en_US
dc.identifier.uri http://hdl.handle.net/2027.42/92100
dc.description.abstract We study the evolution of the stellar and dark matter components in a galaxy cluster of 10 15  M ⊙ from z = 3 to the present epoch using the high‐resolution collisionless simulations of Ruszkowski & Springel. At z = 3 the dominant progenitor haloes were populated with spherical model galaxies with and without accounting for adiabatic contraction. We apply a weighting scheme which allows us to change the relative amount of dark and stellar material assigned to each simulation particle in order to produce luminous properties which agree better with abundance‐matching arguments and observed bulge sizes at z = 3. This permits the study of the effect of initial compactness on the evolution of the mass–size relation. We find that for more compact initial stellar distributions the size of the final brightest cluster galaxy grows with mass according to r ∝ M 2 , whereas for more extended initial distributions, r ∝ M . Our results show that collisionless mergers in a cosmological context can reduce the strength of inner dark matter cusps with changes in logarithmic slope of 0.3–0.5 at fixed radius. Shallow cusps such as those found recently in several strong lensing clusters thus do not necessarily conflict with cold dark matter, but may rather reflect on the initial structure of the progenitor galaxies, which was shaped at high redshift by their formation process. en_US
dc.publisher Wiley Periodicals, Inc. en_US
dc.publisher Blackwell Publishing Ltd en_US
dc.subject.other Galaxies: Elliptical and Lenticular, CD en_US
dc.subject.other Galaxies: Formation en_US
dc.subject.other Galaxies: Evolution en_US
dc.subject.other Galaxies: Clusters: General en_US
dc.title Shallow dark matter cusps in galaxy clusters en_US
dc.type Article en_US
dc.rights.robots IndexNoFollow en_US
dc.subject.hlbsecondlevel Astronomy en_US
dc.subject.hlbtoplevel Science en_US
dc.description.peerreviewed Peer Reviewed en_US
dc.contributor.affiliationum Department of Astronomy, University of Michigan, 500 Church Street, Ann Arbor, MI 48109, USA en_US
dc.contributor.affiliationother Zentrum für Astronomie der Universität Heidelberg, Astronomisches Recheninstitut, Mönchhofstr. 12‐14, 69120 Heidelberg, Germany en_US
dc.contributor.affiliationother Heidelberger Institut für Theoretische Studien, Schloss‐Wolfsbrunnenweg 35, 69118 Heidelberg, Germany en_US
dc.contributor.affiliationother The Michigan Center for Theoretical Physics, 3444 Randall Lab, 450 Church Street, Ann Arbor, MI 48109, USA en_US
dc.contributor.affiliationother Max Planck Institute for Astrophysics, Karl‐Schwarzschild‐Strasse 1, 85740 Garching, Germany en_US
dc.description.bitstreamurl http://deepblue.lib.umich.edu/bitstream/2027.42/92100/1/j.1365-2966.2012.21262.x.pdf
dc.identifier.doi 10.1111/j.1365-2966.2012.21262.x en_US
dc.identifier.source Monthly Notices of the Royal Astronomical Society en_US
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dc.owningcollname Interdisciplinary and Peer-Reviewed
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