Connecting galaxy evolution in clusters with their radial profiles and phase space distribution: results from the IllustrisTNG hydrodynamical simulations
We study the population of galaxies around galaxy clusters in the hydrodynamic simulation suite IllustrisTNG 300-1 to study the signatures of their evolutionary history on observable properties. We measure the radial number density profile, phase space distribution, and splashback radius for galaxie...
Published in: | Monthly Notices of the Royal Astronomical Society |
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ftpubman:oai:pure.mpg.de:item_3456357 2023-08-27T04:12:05+02:00 Connecting galaxy evolution in clusters with their radial profiles and phase space distribution: results from the IllustrisTNG hydrodynamical simulations Dacunha, T. Belyakov, M. Adhikari, S. Shin, T. Goldstein, S. Jain, B. 2022-02-12 application/pdf http://hdl.handle.net/21.11116/0000-000B-52F5-4 http://hdl.handle.net/21.11116/0000-000B-52F7-2 unknown info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stac392 http://hdl.handle.net/21.11116/0000-000B-52F5-4 http://hdl.handle.net/21.11116/0000-000B-52F7-2 info:eu-repo/semantics/closedAccess Monthly Notices of the Royal Astronomical Society info:eu-repo/semantics/article 2022 ftpubman https://doi.org/10.1093/mnras/stac392 2023-08-02T01:20:11Z We study the population of galaxies around galaxy clusters in the hydrodynamic simulation suite IllustrisTNG 300-1 to study the signatures of their evolutionary history on observable properties. We measure the radial number density profile, phase space distribution, and splashback radius for galaxies of different masses and colours over the redshift range z = 0−1. The three primary physical effects which shape the galaxy distribution within clusters are the galaxy quenching, angular momentum distribution, and dynamical friction. We find three distinct populations of galaxies by applying a Gaussian mixture model to their distribution in colour and mass. They have distinct evolutionary histories and leave distinct signatures on their distribution around cluster haloes. We find that low-mass red galaxies show the most concentrated distribution in clusters and the largest splashback radius, while high-mass red galaxies show a less concentrated distribution and a smaller splashback radius. Blue galaxies, which mostly quench into the low-mass red population, have the shallowest distribution within the clusters, with those on radial orbits quenched rapidly before reaching pericentre. Comparison with the distribution of galaxies from the Dark Energy Survey survey around Sunyaev–Zeldovich clusters from the Atacama Cosmology Telescope and South Pole Telescope surveys shows evidence for differences in galaxy evolution between simulations and data. Article in Journal/Newspaper South pole Max Planck Society: MPG.PuRe South Pole Monthly Notices of the Royal Astronomical Society 512 3 4378 4393 |
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Max Planck Society: MPG.PuRe |
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description |
We study the population of galaxies around galaxy clusters in the hydrodynamic simulation suite IllustrisTNG 300-1 to study the signatures of their evolutionary history on observable properties. We measure the radial number density profile, phase space distribution, and splashback radius for galaxies of different masses and colours over the redshift range z = 0−1. The three primary physical effects which shape the galaxy distribution within clusters are the galaxy quenching, angular momentum distribution, and dynamical friction. We find three distinct populations of galaxies by applying a Gaussian mixture model to their distribution in colour and mass. They have distinct evolutionary histories and leave distinct signatures on their distribution around cluster haloes. We find that low-mass red galaxies show the most concentrated distribution in clusters and the largest splashback radius, while high-mass red galaxies show a less concentrated distribution and a smaller splashback radius. Blue galaxies, which mostly quench into the low-mass red population, have the shallowest distribution within the clusters, with those on radial orbits quenched rapidly before reaching pericentre. Comparison with the distribution of galaxies from the Dark Energy Survey survey around Sunyaev–Zeldovich clusters from the Atacama Cosmology Telescope and South Pole Telescope surveys shows evidence for differences in galaxy evolution between simulations and data. |
format |
Article in Journal/Newspaper |
author |
Dacunha, T. Belyakov, M. Adhikari, S. Shin, T. Goldstein, S. Jain, B. |
spellingShingle |
Dacunha, T. Belyakov, M. Adhikari, S. Shin, T. Goldstein, S. Jain, B. Connecting galaxy evolution in clusters with their radial profiles and phase space distribution: results from the IllustrisTNG hydrodynamical simulations |
author_facet |
Dacunha, T. Belyakov, M. Adhikari, S. Shin, T. Goldstein, S. Jain, B. |
author_sort |
Dacunha, T. |
title |
Connecting galaxy evolution in clusters with their radial profiles and phase space distribution: results from the IllustrisTNG hydrodynamical simulations |
title_short |
Connecting galaxy evolution in clusters with their radial profiles and phase space distribution: results from the IllustrisTNG hydrodynamical simulations |
title_full |
Connecting galaxy evolution in clusters with their radial profiles and phase space distribution: results from the IllustrisTNG hydrodynamical simulations |
title_fullStr |
Connecting galaxy evolution in clusters with their radial profiles and phase space distribution: results from the IllustrisTNG hydrodynamical simulations |
title_full_unstemmed |
Connecting galaxy evolution in clusters with their radial profiles and phase space distribution: results from the IllustrisTNG hydrodynamical simulations |
title_sort |
connecting galaxy evolution in clusters with their radial profiles and phase space distribution: results from the illustristng hydrodynamical simulations |
publishDate |
2022 |
url |
http://hdl.handle.net/21.11116/0000-000B-52F5-4 http://hdl.handle.net/21.11116/0000-000B-52F7-2 |
geographic |
South Pole |
geographic_facet |
South Pole |
genre |
South pole |
genre_facet |
South pole |
op_source |
Monthly Notices of the Royal Astronomical Society |
op_relation |
info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stac392 http://hdl.handle.net/21.11116/0000-000B-52F5-4 http://hdl.handle.net/21.11116/0000-000B-52F7-2 |
op_rights |
info:eu-repo/semantics/closedAccess |
op_doi |
https://doi.org/10.1093/mnras/stac392 |
container_title |
Monthly Notices of the Royal Astronomical Society |
container_volume |
512 |
container_issue |
3 |
container_start_page |
4378 |
op_container_end_page |
4393 |
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1775355868962881536 |