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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 Sklodowskaw-Curie grant agreement number 734374, the LACEGAL project. AC, AK, and GY were supported by the MICIU/FEDER through grant number PGC2018-094975-C21 as well as by the Ministerio de Ciencia e Innovaci ' on under research grant PID2021-122603NB-C21. AK further thanks Urge Overkill for sister havanna. WC was supported by the STFC AGP Grant ST/V000594/1 and by the Atracci ' on de Talento Contract no. 2020-T1/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. RH acknowledges support from STFC through a studentship.

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Galaxy pairs in the three hundred simulations: a study on the performance of observational pair-finding techniques

Publicado en:MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY. 515 (4): 5375-5388 - 2022-08-18 515(4), DOI: 10.1093/mnras/stac2127

Autores: Contreras-Santos, Ana; Knebe, Alexander; Cui, Weiguang; Haggar, Roan; Pearce, Frazer; Gray, Meghan; De Petris, Marco; Yepes, Gustavo

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Close pairs of galaxies have been broadly studied in the literature as a way to understand galaxy interactions and mergers. In observations, they are usually defined by setting a maximum separation in the sky and in velocity along the line of sight, and finding galaxies within these ranges. However, when observing the sky, projection effects can affect the results, by creating spurious pairs that are not close in physical distance. In this work, we mimic these observational techniques to find pairs in the three hundred simulations of clusters of galaxies. The galaxies' 3D coordinates are projected into 2D, with Hubble flow included for their line-of-sight velocities. The pairs found are classified into 'good' or 'bad' depending on whether their 3D separations are within the 2D spatial limit or not. We find that the fraction of good pairs can be between 30 and 60 per cent depending on the thresholds used in observations. Studying the ratios of observable properties between the pair member galaxies, we find that the likelihood of a pair being 'good' can be increased by around 40, 20, and 30 per cent if the given pair has, respectively, a mass ratio below 0.2, metallicity ratio above 0.8, or colour ratio below 0.8. Moreover, shape and stellar-to-halo mass ratios, respectively, below 0.4 and 0.2 can increase the likelihood by 50 to 100 per cent. These results suggest that these properties can be used to increase the chance of finding good pairs in observations of galaxy clusters and their environment.

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