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| Main Authors: | , , , , , , , , , , , , , |
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| Format: | Preprint |
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2024
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| Subjects: | |
| Online Access: | https://arxiv.org/abs/2411.08155 |
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| _version_ | 1866917858643017728 |
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| author | Ortiz, M. Espinoza Guaita, L. Demarco, R. Calabró, A. Pentericci, L. Castellano, M. Artale, M. Celeste Hathi, N. P. Koekemoer, Anton M. Mannucci, F. Hibon, P. McLeod, D. J. Gargiulo, A. Pompei, E. |
| author_facet | Ortiz, M. Espinoza Guaita, L. Demarco, R. Calabró, A. Pentericci, L. Castellano, M. Artale, M. Celeste Hathi, N. P. Koekemoer, Anton M. Mannucci, F. Hibon, P. McLeod, D. J. Gargiulo, A. Pompei, E. |
| contents | Context: Understanding galaxy evolution in dense environments, particularly proto-clusters, is crucial for studying mechanisms driving star formation and quenching. Aims: This study examines how two proto-cluster over-densities at 3 < z < 4 impact star formation rate (SFR), stellar mass, and morphology, focusing on quenched galaxies. Methods: We identified proto-cluster over-densities in the Chandra Deep Field South (CDFS) and Ultra Deep Survey (UDS) regions of the VANDELS survey. Using spectral energy distribution analysis, Bayesian methods (BEAGLE and BAGPIPES) helped derive best-fit parameters and U-V and V-J rest-frame colours (UVJ), classifying galaxies as quenched or star-forming based on UVJ diagrams and specific star formation rates (sSFR). TNG300 simulations aided interpretation. Results: Two of 13 proto-cluster over-densities host quenched galaxies with red U-V colours, low sSFR, and properties like massive passive galaxies. These quenched members are redder, older, more massive, and more compact. The highest-density peaks at z=3.55 and z=3.43 have dark matter halo masses consistent with proto-clusters and host AGNs, with five and three AGNs, respectively. Compared to field galaxies, these quenched members are in denser environments. TNG300 simulations suggest proto-clusters with quenched galaxies at high redshift evolve to contain more passive galaxies by z=1. Conclusions: The over-densities host massive quenched galaxies and AGNs in their densest peaks. Simulations reveal that sSFR for passive galaxies in proto-clusters was high at z=6, with median mass growth rates of 96% from z=6 to z=3. Conditions for mass assembly likely involve galaxy interactions and high gas accretion in dense environments. Black hole growth and AGN feedback appear to drive quenching at z=3, aligning with the properties of quenched galaxies observed in our study. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2411_08155 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | The VANDELS Survey: Star formation and quenching in two over-densities at 3 < z < 4 Ortiz, M. Espinoza Guaita, L. Demarco, R. Calabró, A. Pentericci, L. Castellano, M. Artale, M. Celeste Hathi, N. P. Koekemoer, Anton M. Mannucci, F. Hibon, P. McLeod, D. J. Gargiulo, A. Pompei, E. Astrophysics of Galaxies Context: Understanding galaxy evolution in dense environments, particularly proto-clusters, is crucial for studying mechanisms driving star formation and quenching. Aims: This study examines how two proto-cluster over-densities at 3 < z < 4 impact star formation rate (SFR), stellar mass, and morphology, focusing on quenched galaxies. Methods: We identified proto-cluster over-densities in the Chandra Deep Field South (CDFS) and Ultra Deep Survey (UDS) regions of the VANDELS survey. Using spectral energy distribution analysis, Bayesian methods (BEAGLE and BAGPIPES) helped derive best-fit parameters and U-V and V-J rest-frame colours (UVJ), classifying galaxies as quenched or star-forming based on UVJ diagrams and specific star formation rates (sSFR). TNG300 simulations aided interpretation. Results: Two of 13 proto-cluster over-densities host quenched galaxies with red U-V colours, low sSFR, and properties like massive passive galaxies. These quenched members are redder, older, more massive, and more compact. The highest-density peaks at z=3.55 and z=3.43 have dark matter halo masses consistent with proto-clusters and host AGNs, with five and three AGNs, respectively. Compared to field galaxies, these quenched members are in denser environments. TNG300 simulations suggest proto-clusters with quenched galaxies at high redshift evolve to contain more passive galaxies by z=1. Conclusions: The over-densities host massive quenched galaxies and AGNs in their densest peaks. Simulations reveal that sSFR for passive galaxies in proto-clusters was high at z=6, with median mass growth rates of 96% from z=6 to z=3. Conditions for mass assembly likely involve galaxy interactions and high gas accretion in dense environments. Black hole growth and AGN feedback appear to drive quenching at z=3, aligning with the properties of quenched galaxies observed in our study. |
| title | The VANDELS Survey: Star formation and quenching in two over-densities at 3 < z < 4 |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2411.08155 |