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The authors would like to thank Emanuele Contini for carefully reading the manuscript and providing insightful suggestions. This work has been made possible by THE THREE HUNDRED (https://the300-project.org) collaboration. 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. 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. A.C.S., A.K., I.A.A. and C.D.V. thank the Ministerio de Ciencia e Innovacion (MICINN) for financial support under research grants PID2021-122603NB-C21 and PID2021-122603NB-C22. A.K. further thanks Drop Nineteens for "kick the tragedy". W.C. is supported by the STFC AGP Grant ST/V000594/1 and the Atraccion de Talento Contract no. 2020-T1/TIC-19882 granted by the Comunidad de Madrid in Spain. He also thanks the Ministerio de Ciencia e Innovacion (Spain) for financial support under Project grant PID2021-122603NB-C21 and ERC: HORIZON-TMA-MSCA-SE for supporting the LACEGAL-III project with grant number 101086388.

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Characterising the intra-cluster light in The Three Hundred simulations

Publicado en:ASTRONOMY & ASTROPHYSICS. 683 A59- - 2024-03-06 683(), DOI: 10.1051/0004-6361/202348474

Autores: Contreras-Santos, A; Knebe, A; Cui, W; Alonso Asensio, I; Dalla Vecchia, C; Canas, R; Haggar, R; Mostoghiu Paun, R A; Pearce, F R; Rasia, E

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We characterise the intra-cluster light (ICL) in ensembles of full-physics cluster simulations from THE THREE HUNDRED project, a suite of 324 hydrodynamical resimulations of cluster-sized halos. We identify the ICL as those stellar particles bound to the potential of the cluster itself, but not to any of its substructures, and separate the brightest cluster galaxy (BCG) by means of a fixed 50 kpc aperture. We find the total BCG+ICL mass to be in agreement with state-of-the-art observations of galaxy clusters. The ICL mass fraction of our clusters is between 30 and 50% of the total stellar mass within R-500, while the BCG represents around 10%. We further find no trend of the ICL fraction with cluster halo mass, at least not in the range [0.2, 3] 10(15) h(-1) M-circle dot considered here. For the dynamical state, characterised both by theoretical estimators and by the recent merging history of the cluster, there is a clear correlation, such that more relaxed clusters and those that have undergone fewer recent mergers have a higher ICL fraction. Finally, we investigate the possibility of using the ICL to explore the dark matter (DM) component of galaxy clusters. We compute the volumetric density profile for the DM and ICL components and show that, up to R500, the ratio between the two can be described by a power law. Working with the velocity dispersion profiles instead, we show that the ratio can be fit by a straight line. Providing the parameters of these fits, we show how the ICL can be used to infer DM properties.

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