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This work has been made possible by the 'The Three Hundred' collaboration.6 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 Supercomputaci ' on. As part of The Three Hundred Project, this work has received financial support from the European Union's Horizon 2020 Research and Innovation Programme under the Marie Sklodowska Curie grant agreement number 734374, the LACEGAL project.RH and AvdL acknowledge support by the US Department of Energy under award DE-SC0018053. AC acknowledges support from the National Science Foundation PHY 1852239 `Summer Undergraduate Research in Physics and Astronomy at the University of Michigan' grant. CA acknowledges support from the LSA Collegiate Fellowship at the University of Michigan, the Leinweber Foundation, and DoE Award DE-SC009193. CG and MM acknowledge the grants ASI n.I/023/12/0, ASI-INAF n. 2018-23-HH.0 and PRIN-MIUR 2017 WSCC32 'Zooming into dark matter and proto-galaxies with massive lensing clusters; they also acknowledge support from INAF (funding of main-stream projects). WC is supported by the European Research Council under grant number 670193 and by the STFC AGP Grant ST/V000594/1. He further acknowledges the science research grants from the China Manned Space Project with NO. CMS-CSST-2021-A01 and CMS-CSST-2021-B01. GY acknowledges financial support from Ministerio de Ciencia, Innovacion y Universidades/Fondo Europeo de Desarrollo Regional, under research grant PGC2018-094975-C21.

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Brightest cluster galaxies trace weak lensing mass bias and halo triaxiality in the three hundred project

Publicated to:MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY. 513 (2): 2178-2193 - 2022-06-01 513(2), DOI: 10.1093/mnras/stac997

Authors: Herbonnet, Ricardo; Crawford, Adrian; Avestruz, Camille; Rasia, Elena; Giocoli, Carlo; Meneghetti, Massimo; von Der Linden, Anja; Cui, Weiguang; Yepes, Gustavo;

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Abstract

Galaxy clusters have a triaxial matter distribution. The weak-lensing signal, an important part in cosmological studies, measures the projected mass of all matter along the line of sight, and therefore changes with the orientation of the cluster. Studies suggest that the shape of the brightest cluster galaxy (BCG) in the centre of the cluster traces the underlying halo shape, enabling a method to account for projection effects. We use 324 simulated clusters at four redshifts between 0.1 and 0.6 from 'The Three Hundred Project' to quantify correlations between the orientation and shape of the BCG and the halo. We find that haloes and their embedded BCGs are aligned, with an average similar to 20 degree angle between their major axes. The bias in weak lensing cluster mass estimates correlates with the orientation of both the halo and the BCG. Mimicking observations, we compute the projected shape of the BCG, as a measure of the BCG orientation, and find that it is most strongly correlated to the weak-lensing mass for relaxed clusters. We also test a 2D cluster relaxation proxy measured from BCG mass isocontours. The concentration of stellar mass in the projected BCG core compared to the total stellar mass provides an alternative proxy for the BCG orientation. We find that the concentration does not correlate to the weak-lensing mass bias, but does correlate with the true halo mass. These results indicate that the BCG shape and orientation for large samples of relaxed clusters can provide information to improve weak-lensing mass estimates.

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