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This work has been made possible by the `The Three Hundred' Collaboration (https://www.the300-project.org).The project 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 authors would like to thank the anonymous referee for their constructive feedback, which improved the quality of this paper. Additionally, they would like to thank The Red Espanola de Supercomputacion for granting us computing time at the MareNostrum Supercomputer of the BSC-CNS where most of the cluster simulations have been performed. Part of the computations with GADGET-X have also been performed at the `Leibniz-Rechenzentrum' with CPU time assigned to the Project `pr83li'. RM, AK, and GY would like to thank MINECO/FEDER (Spain) for financial support under research grants AYA2015-63819-P and MICIU/FEDER for financial support under research grant PGC2018-094975-C21. RM further acknowledges support from the International Centre for Radio Astronomy (ICRAR) for funding this project. AK further acknowledges support from the Spanish Red Consolider MultiDark FPA2017-90566-REDC and thanks Joy Division for unknown pleasures. CL has received funding from the ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), through project number CE170100013. WC acknowledges the supported by the European Research Council under grant number 670193. SB acknowledges financial support from PRIN-MIUR 2015W7KAWC, the INFN INDARK grant, and the EU H2020 Research and Innovation Programme under the ExaNeSt project (Grant Agreement No. 671553). KD acknowledges support through ORIGINS, founded by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under Germany's Excellence Strategy -EXC-2094 -390783311. The authors contributed to this paper in the following ways: RM, AK, FRP and CP formed the core team. RM analysed the data, produced the plots and wrote the paper along with AK, FRP, CL, WC, SB, and KD. SB, KD, GM, and GY supplied the simulation data. All authors had the opportunity to provide comments on this work. This work was created by making use of the following software: Python, Matplotlib (Hunter 2007), Numpy (van der Walt et al. 2011), scipy (Virtanen et al. 2020), astropy (Astropy Collaboration 2013, 2018), and pynbody (Pontzen et al. 2013).

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The Three Hundred Project: The stellar angular momentum evolution of cluster galaxies

Publicado en:ASTRONOMY & ASTROPHYSICS. 652 A10- - 2021-08-02 652(), DOI: 10.1051/0004-6361/202038425

Autores: Mostoghiu, R.; Knebe, A.; Pearce, F. R.; Power, C.; Lagos, C. D. P.; Cui, W.; Borgani, S.; Dolag, K.; Murante, G.; Yepes, G.;

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Resumen

Using 324 numerically modelled galaxy clusters as provided by THE THREE HUNDRED project, we study the evolution of the kinematic properties of the stellar component of haloes on first infall. We selected objects with M-star>5x10(10) h(-1) M-circle dot within 3R(200) of the main cluster halo at z=0 and followed their progenitors. We find that although haloes are stripped of their dark matter and gas after entering the main cluster halo, there is practically no change in their stellar kinematics. For the vast majority of our 'galaxies' - defined as the central stellar component found within the haloes that form our sample - their kinematic properties, as described by the fraction of ordered rotation, and their position in the specific stellar angular momentum-stellar mass plane j(star)-M-star are mostly unchanged by the influence of the central host cluster. However, for a small number of infalling galaxies, stellar mergers and encounters with remnant stellar cores close to the centre of the main cluster, particularly during pericentre passage, are able to spin up their stellar component by z=0.

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