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| Main Authors: | , , , , , , |
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| Format: | Preprint |
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2025
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| Online Access: | https://arxiv.org/abs/2505.21983 |
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| _version_ | 1866916763957985280 |
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| author | López-Gutiérrez, M. M. Bravo-Alfaro, H. Rahna, P. T. Mamon, G. A. Jaffé, Y. L. Madrigal-Ayala, L. F. Acosta-Espinoza, E. |
| author_facet | López-Gutiérrez, M. M. Bravo-Alfaro, H. Rahna, P. T. Mamon, G. A. Jaffé, Y. L. Madrigal-Ayala, L. F. Acosta-Espinoza, E. |
| contents | During the fall of late-type galaxies into clusters, they can experiment a variety of evolutionary mechanisms according their local environment. Consequently, studying the UV emission and the cold gas of late-type galaxies provide key insights in the evolution of short-lived starburst and galaxy quenching. In this work, we conduted a study of two 28' fields observed with UVIT-AstroSat in the central region of the Abell cluster A496 ($z=0.033$), including HI, data from NRAO VLA. We reported 22 cluster members detected in FUV; all of them are detected in HI, or have upper limits for the HI-mass. We find our FUV detected galaxies generally have higher specific star formation rates than other star forming galaxies. Most of the FUV galaxies with masses above 10$^9 \mathrm{M}_{\odot}$,and showing high sSFR have no close neighbors, pointing at RPS as the dominant mechanism affecting them. In contrast, most of the low-mass FUV objects present at least one companion, suggesting that tidal interactions also play an important role in the triggering of infalling galaxies. Combining the FUV-SFR with the HI properties of the observed galaxies in A496 we identify an evolutionary sequence consisting of five stages: (1) Pre-triggering, (2) Initial SF-triggering, (3) Peak of star-formation, (4) SF-fading, and (5) SF-quenching. During this path, normal gas-rich objects reach a gas-deficiency phase with SFR well below the main sequence. This process, prior to becoming a full passive galaxy, can be accomplished within a few 10$^{8}$ yr. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2505_21983 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Tracing Galaxy Evolution in infalling galaxies of Abell 496: From Starburst to Quenching López-Gutiérrez, M. M. Bravo-Alfaro, H. Rahna, P. T. Mamon, G. A. Jaffé, Y. L. Madrigal-Ayala, L. F. Acosta-Espinoza, E. Astrophysics of Galaxies During the fall of late-type galaxies into clusters, they can experiment a variety of evolutionary mechanisms according their local environment. Consequently, studying the UV emission and the cold gas of late-type galaxies provide key insights in the evolution of short-lived starburst and galaxy quenching. In this work, we conduted a study of two 28' fields observed with UVIT-AstroSat in the central region of the Abell cluster A496 ($z=0.033$), including HI, data from NRAO VLA. We reported 22 cluster members detected in FUV; all of them are detected in HI, or have upper limits for the HI-mass. We find our FUV detected galaxies generally have higher specific star formation rates than other star forming galaxies. Most of the FUV galaxies with masses above 10$^9 \mathrm{M}_{\odot}$,and showing high sSFR have no close neighbors, pointing at RPS as the dominant mechanism affecting them. In contrast, most of the low-mass FUV objects present at least one companion, suggesting that tidal interactions also play an important role in the triggering of infalling galaxies. Combining the FUV-SFR with the HI properties of the observed galaxies in A496 we identify an evolutionary sequence consisting of five stages: (1) Pre-triggering, (2) Initial SF-triggering, (3) Peak of star-formation, (4) SF-fading, and (5) SF-quenching. During this path, normal gas-rich objects reach a gas-deficiency phase with SFR well below the main sequence. This process, prior to becoming a full passive galaxy, can be accomplished within a few 10$^{8}$ yr. |
| title | Tracing Galaxy Evolution in infalling galaxies of Abell 496: From Starburst to Quenching |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2505.21983 |