The behaviour of dark matter associated with four bright cluster galaxies in the 10 kpc core of Abell 3827

Massey, Richard and Williams, Liliya and Smit, Renske and Swinbank, Mark and Kitching, Thomas D. and Harvey, David and Jauzac, Mathilde and Israel, Holger and Clowe, Douglas and Edge, Alastair and Hilton, Matt and Jullo, Eric and Leonard, Adrienne and Liesenborgs, Jori and Merten, Julian and Mohammed, Irshad and Nagai, Daisuke and Richard, Johan and Robertson, Andrew and Saha, Prasenjit and Santana, Rebecca and Stott, John and Tittley, Eric (2015) The behaviour of dark matter associated with four bright cluster galaxies in the 10 kpc core of Abell 3827. Monthly Notices of the Royal Astronomical Society, 449 (4). pp. 3393-3406. ISSN 0035-8711

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Galaxy cluster Abell 3827 hosts the stellar remnants of four almost equally bright elliptical galaxies within a core of radius 10 kpc. Such corrugation of the stellar distribution is very rare, and suggests recent formation by several simultaneous mergers. We map the distribution of associated dark matter, using new Hubble Space Telescope imaging and Very Large Telescope/Multi-Unit Spectroscopic Explorer integral field spectroscopy of a gravitationally lensed system threaded through the cluster core. We find that each of the central galaxies retains a dark matter halo, but that (at least) one of these is spatially offset from its stars. The best-constrained offset is 1.62(-0.49)(+0.47) kpc, where the 68 per cent confidence limit includes both statistical error and systematic biases in mass modelling. Such offsets are not seen in field galaxies, but are predicted during the long infall to a cluster, if dark matter self-interactions generate an extra drag force. With such a small physical separation, it is difficult to definitively rule out astrophysical effects operating exclusively in dense cluster core environments - but if interpreted solely as evidence for self-interacting dark matter, this offset implies a cross-section sigma(DM)/(m) similar to (1.7 +/- 0.7) x 10(-4) cm(2) g(-1) x (t(infall)/10(9) yr)(-2), where t(infall) is the infall duration.

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Journal Article
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Monthly Notices of the Royal Astronomical Society
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17 Jan 2017 15:18
Last Modified:
22 Nov 2022 04:15