Connecting galaxy evolution in clusters with their radial profiles and phase space distribution: results from the IllustrisTNG hydrodynamical simulations
ABSTRACT 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 fo...
Published in: | Monthly Notices of the Royal Astronomical Society |
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Oxford University Press (OUP)
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Online Access: | http://dx.doi.org/10.1093/mnras/stac392 https://academic.oup.com/mnras/advance-article-pdf/doi/10.1093/mnras/stac392/42502826/stac392.pdf https://academic.oup.com/mnras/article-pdf/512/3/4378/43294041/stac392.pdf |
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croxfordunivpr:10.1093/mnras/stac392 2024-01-28T10:09:13+01:00 Connecting galaxy evolution in clusters with their radial profiles and phase space distribution: results from the IllustrisTNG hydrodynamical simulations Dacunha, Tara Belyakov, Matthew Adhikari, Susmita Shin, Tae-hyeon Goldstein, Samuel Jain, Bhuvnesh U.S. Department of Energy 2022 http://dx.doi.org/10.1093/mnras/stac392 https://academic.oup.com/mnras/advance-article-pdf/doi/10.1093/mnras/stac392/42502826/stac392.pdf https://academic.oup.com/mnras/article-pdf/512/3/4378/43294041/stac392.pdf en eng Oxford University Press (OUP) https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model Monthly Notices of the Royal Astronomical Society volume 512, issue 3, page 4378-4393 ISSN 0035-8711 1365-2966 Space and Planetary Science Astronomy and Astrophysics journal-article 2022 croxfordunivpr https://doi.org/10.1093/mnras/stac392 2023-12-29T09:38:44Z ABSTRACT 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 Oxford University Press (via Crossref) South Pole Monthly Notices of the Royal Astronomical Society |
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Oxford University Press (via Crossref) |
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croxfordunivpr |
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English |
topic |
Space and Planetary Science Astronomy and Astrophysics |
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Space and Planetary Science Astronomy and Astrophysics Dacunha, Tara Belyakov, Matthew Adhikari, Susmita Shin, Tae-hyeon Goldstein, Samuel Jain, Bhuvnesh Connecting galaxy evolution in clusters with their radial profiles and phase space distribution: results from the IllustrisTNG hydrodynamical simulations |
topic_facet |
Space and Planetary Science Astronomy and Astrophysics |
description |
ABSTRACT 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. |
author2 |
U.S. Department of Energy |
format |
Article in Journal/Newspaper |
author |
Dacunha, Tara Belyakov, Matthew Adhikari, Susmita Shin, Tae-hyeon Goldstein, Samuel Jain, Bhuvnesh |
author_facet |
Dacunha, Tara Belyakov, Matthew Adhikari, Susmita Shin, Tae-hyeon Goldstein, Samuel Jain, Bhuvnesh |
author_sort |
Dacunha, Tara |
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 |
publisher |
Oxford University Press (OUP) |
publishDate |
2022 |
url |
http://dx.doi.org/10.1093/mnras/stac392 https://academic.oup.com/mnras/advance-article-pdf/doi/10.1093/mnras/stac392/42502826/stac392.pdf https://academic.oup.com/mnras/article-pdf/512/3/4378/43294041/stac392.pdf |
geographic |
South Pole |
geographic_facet |
South Pole |
genre |
South pole |
genre_facet |
South pole |
op_source |
Monthly Notices of the Royal Astronomical Society volume 512, issue 3, page 4378-4393 ISSN 0035-8711 1365-2966 |
op_rights |
https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model |
op_doi |
https://doi.org/10.1093/mnras/stac392 |
container_title |
Monthly Notices of the Royal Astronomical Society |
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1789338925667450880 |