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Galaxies 2016, 4(4), 79; doi:10.3390/galaxies4040079

Using the Outskirts of Galaxy Clusters to Determine Their Mass Accretion Rate

Institut d’Astrophysique Spatiale, CNRS (UMR8617) Université Paris-Sud 11, Bât. 121, F-91405 Orsay, France
Academic Editors: Stefano Ettori and Dominique Eckert
Received: 27 September 2016 / Revised: 8 December 2016 / Accepted: 9 December 2016 / Published: 20 December 2016
(This article belongs to the Special Issue Exploring the Outskirts of Galaxy Clusters)
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Abstract

We explore the possibility of using the external regions of galaxy clusters to measure their mass accretion rate (MAR). The main goal is to provide a method to observationally investigate the growth of structures on the nonlinear scales of galaxy clusters. We derive the MAR by using the mass profile beyond the splashback radius, evaluating the mass of a spherical shell and the time it takes to fall in. The infall velocity of the shell is extracted from N-body simulations. The average MAR returned by our prescription in the redshift range z = [ 0 , 2 ] is within 20%–40% of the average MAR derived from the merger trees of dark matter haloes in the reference N-body simulations. Our result suggests that the external regions of galaxy clusters can be used to measure the mean MAR of a sample of clusters. View Full-Text
Keywords: galaxies clusters: general; methods: N-body simulations; cosmology: theory galaxies clusters: general; methods: N-body simulations; cosmology: theory
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This is an open access article distributed under the Creative Commons Attribution License which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. (CC BY 4.0).

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De Boni, C. Using the Outskirts of Galaxy Clusters to Determine Their Mass Accretion Rate. Galaxies 2016, 4, 79.

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