The galaxy mass-size relation in CARLA clusters and proto-clusters at 1.4 < z < 2.8: larger cluster galaxy sizes
The galaxy mass-size relation in CARLA clusters and proto-clusters at 1.4 < z < 2.8: larger cluster galaxy sizes
We study the galaxy mass-size relation in 15 spectroscopically confirmed clusters at 1.4 < z < 2.8 from the CARLA survey. Our clusters span a total stellar mass in the range 11.3 < log(M∗c/M· ) < 12.6 (with an approximate halo mass in the range 13.5 ≲ log(Mhc/M· ) ≲ 14.5). Our main finding is that cluster passive early-type galaxies (ETGs) at z ≳ 1.5 with a mass log(M/M· ) > 10.5 are systematically 0.2 0.3dex larger (≳3′) than field ETGs at a similar redshift and mass from the CANDELS survey. The passive ETG average size evolution with redshift is slower at 1 < z < 2 when compared to the field. This could be explained by early-epoch differences in the formation and early evolution of galaxies in haloes of a different mass, as predicted by models. It does not exclude that other physical mechanisms, such as strong compaction and gas dissipation in field galaxies, followed by a sequence of mergers may have also played a significant role in the field ETG evolution, but not necessarily in the evolution of cluster galaxies. Our passive ETG mass-size relation shows a tendency to flatten at 9.6 < log(M/M· ) < 10.5, where the average size is log(Re/kpc) = 0.05 ± 0.22, which is broadly consistent with galaxy sizes in the field and in the local Universe. This implies that galaxies in the low end of the mass-size relation do not evolve much from z ∼ 2 to the present, and that their sizes evolve in a similar way in clusters and in the field. Brightest cluster galaxies lie on the same mass-size relation as satellites, suggesting that their size evolution is not different from satellites at redshift z ≳ 2. Half of the active early-type galaxies, which are 30% of our ETG sample, follow the field passive galaxy mass-size relation, and the other half follow the field active galaxy mass-size relation. These galaxies likely went through a recent merger or neighbor galaxy interaction, and would most probably quench at a later epoch and increase the fraction of passive ETGs in clusters. We do not observe a large population of compact galaxies (only one), as is observed in the field at these redshifts, implying that the galaxies in our clusters are not observed in an epoch close to their compaction.
CD, Galaxies: clusters: general, Galaxies: elliptical and lenticular, Galaxies: evolution, Galaxies: structure, Large-scale structure of Universe
Afanasiev, Anton V.
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Mei, Simona
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Fu, Hao
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Shankar, Francesco
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Amodeo, Stefania
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Stern, Daniel
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Cooke, Elizabeth A.
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Gonzalez, Anthony H.
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Noirot, Gaël
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Rettura, Alessandro
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Wylezalek, Dominika
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Breuck, Carlos De
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Hatch, Nina A.
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Stanford, Spencer A.
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Vernet, Joël
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10 February 2023
Afanasiev, Anton V.
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Mei, Simona
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Fu, Hao
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Shankar, Francesco
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Amodeo, Stefania
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Stern, Daniel
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Cooke, Elizabeth A.
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Gonzalez, Anthony H.
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Noirot, Gaël
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Rettura, Alessandro
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Wylezalek, Dominika
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Breuck, Carlos De
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Hatch, Nina A.
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Stanford, Spencer A.
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Vernet, Joël
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Afanasiev, Anton V., Mei, Simona, Fu, Hao, Shankar, Francesco, Amodeo, Stefania, Stern, Daniel, Cooke, Elizabeth A., Gonzalez, Anthony H., Noirot, Gaël, Rettura, Alessandro, Wylezalek, Dominika, Breuck, Carlos De, Hatch, Nina A., Stanford, Spencer A. and Vernet, Joël
(2023)
The galaxy mass-size relation in CARLA clusters and proto-clusters at 1.4 < z < 2.8: larger cluster galaxy sizes.
Astronomy and Astrophysics, 670, [A95].
(doi:10.1051/0004-6361/202244634).
Abstract
We study the galaxy mass-size relation in 15 spectroscopically confirmed clusters at 1.4 < z < 2.8 from the CARLA survey. Our clusters span a total stellar mass in the range 11.3 < log(M∗c/M· ) < 12.6 (with an approximate halo mass in the range 13.5 ≲ log(Mhc/M· ) ≲ 14.5). Our main finding is that cluster passive early-type galaxies (ETGs) at z ≳ 1.5 with a mass log(M/M· ) > 10.5 are systematically 0.2 0.3dex larger (≳3′) than field ETGs at a similar redshift and mass from the CANDELS survey. The passive ETG average size evolution with redshift is slower at 1 < z < 2 when compared to the field. This could be explained by early-epoch differences in the formation and early evolution of galaxies in haloes of a different mass, as predicted by models. It does not exclude that other physical mechanisms, such as strong compaction and gas dissipation in field galaxies, followed by a sequence of mergers may have also played a significant role in the field ETG evolution, but not necessarily in the evolution of cluster galaxies. Our passive ETG mass-size relation shows a tendency to flatten at 9.6 < log(M/M· ) < 10.5, where the average size is log(Re/kpc) = 0.05 ± 0.22, which is broadly consistent with galaxy sizes in the field and in the local Universe. This implies that galaxies in the low end of the mass-size relation do not evolve much from z ∼ 2 to the present, and that their sizes evolve in a similar way in clusters and in the field. Brightest cluster galaxies lie on the same mass-size relation as satellites, suggesting that their size evolution is not different from satellites at redshift z ≳ 2. Half of the active early-type galaxies, which are 30% of our ETG sample, follow the field passive galaxy mass-size relation, and the other half follow the field active galaxy mass-size relation. These galaxies likely went through a recent merger or neighbor galaxy interaction, and would most probably quench at a later epoch and increase the fraction of passive ETGs in clusters. We do not observe a large population of compact galaxies (only one), as is observed in the field at these redshifts, implying that the galaxies in our clusters are not observed in an epoch close to their compaction.
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2212.00031v2
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Accepted/In Press date: 21 November 2022
e-pub ahead of print date: 10 February 2023
Published date: 10 February 2023
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Funding Information:
This work is based on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy Inc., under NASA contract NAS 5-26555. These observations are associated with program GO-13740. Support for program GO-13740 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy Inc., under NASA contract NAS 5-26555. HF and FS acknowledge support from the European Union’s Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie Grant agreement No. 860744. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. We thank Ignacio Trujillo, Arjen van der Wel, Igor Chilingarian, and Francoise Combes for useful comments. We thank Leo Girardi for his help with the TRILEGAL model. We thank Université Paris Cité, which founded AA’s Ph.D. research. SM thanks Jet Propulsion Laboratory, California Institute of Technology, for hosting her in the context of this project. The work of DS was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. GN acknowledges funding support from the Natural Sciences and Engineering Research Council (NSERC) of Canada through a Discovery Grant and Discovery Accelerator Supplement, and from the Canadian Space Agency through Grant 18JWST-GTO1. NAH thanks the Science and Technology Facilities Council, UK, consolidated Grant ST/T000171/1. This work was supported by the French Space Agency (CNES). We thank the anonymous referee for her/his careful reading of the manuscript and useful suggestions that helped to improve the paper.
Publisher Copyright:
© 2023 The Authors.
Keywords:
CD, Galaxies: clusters: general, Galaxies: elliptical and lenticular, Galaxies: evolution, Galaxies: structure, Large-scale structure of Universe
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Local EPrints ID: 477651
URI: http://eprints.soton.ac.uk/id/eprint/477651
PURE UUID: cde7e4ef-d9a6-4ffd-852f-cf14ee66618d
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Date deposited: 12 Jun 2023 16:42
Last modified: 17 Mar 2024 02:17
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Contributors
Author:
Anton V. Afanasiev
Author:
Simona Mei
Author:
Stefania Amodeo
Author:
Daniel Stern
Author:
Elizabeth A. Cooke
Author:
Anthony H. Gonzalez
Author:
Gaël Noirot
Author:
Alessandro Rettura
Author:
Dominika Wylezalek
Author:
Carlos De Breuck
Author:
Nina A. Hatch
Author:
Spencer A. Stanford
Author:
Joël Vernet
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