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We kindly thank Alexander Knebe, Ana Contreras, Elena Rasia, Frazer Pearce, and Roan Haggar for useful discussions. This work has received financial support from the European Union's Horizon 2020 Research and Innovation programme under the Marie Sklodowskaw-Curie grant agreement number 734374, i.e. the LACEGAL project. The simulations used in this paper have been performed in the MareNostrum Supercomputer at the Barcelona Supercomputing Center, thanks to CPU time granted by the Red Espanola de Supercomputacion. The CosmoSim data base used in this paper is a service by the Leibniz-Institute for Astrophysics Potsdam (AIP). The MultiDark data base was developed in cooperation with the Spanish MultiDark Consolider Project CSD2009-00064. WC is supported by the STFC AGP consolidated Grant ST/V000594/1 and the Atraccion de Talento Contract no. 2020T1/TIC-19882 granted by the Comunidad de Madrid in Spain. He further acknowledges the science research grants from the China Manned Space Project with no. CMS-CSST-2021-A01 and CMS-CSST-2021-B01. MDP acknowledges support from Sapienza Universit`a di Roma thanks to Progetti di Ricerca Medi 2020, RM120172B32D5BE2. For the purpose of open access, the author has applied a Creative Commons Attribution (CC BY) licence to any Author Accepted Manuscript version arising from this submission.

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The Three Hundred: cluster dynamical states and relaxation period

Publicado en:MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY. 516 (1): 26-38 - 2022-08-23 516(1), DOI: 10.1093/mnras/stac2171

Autores: Zhang, Bowei; Cui, Weiguang; Wang, Yuhuan; Dave, Romeel; De Petris, Marco;

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We introduce a new parameter lambda(DS) to quantify the dynamical state of galaxy clusters and test it using simulations from THE THREE HUNDRED cluster zoom suite. lambda(DS) is a combination of three previously used dynamical state measures, namely virial ratio, centre of mass offset, and substructure mass fraction, crafted to assume a double-Gaussian distribution, thereby yielding a natural division between relaxed and unrelaxed clusters where the Gaussians cross. Using dark matter-only simulations, we identify the optimal separator to be lambda(DS) = 3.424. We test this same criterion on two sets of fully hydrodynamical THE THREE HUNDRED runs (GADGET-X and GIZMO-SIMBA), and find only a weak dependence on the input baryonic physics. We correlate the evolution of lambda(DS) with the mass accretion history and find that halo mass changes of Delta M-200/M-200 less than or similar to 0.12 do not typically alter the dynamical state. We examine the relaxation period, defined as the time taken to return to relaxation after becoming disturbed, and find a correlation between this relaxation period and the strength of halo mass change Delta M-200/M-200. By fitting this correlation, we show that the relaxation period can be estimated from Delta M-200/M-200 (even for multiple mass accretion events) with good accuracy.

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