| Issue |
A&A
Volume 682, February 2024
|
|
|---|---|---|
| Article Number | A117 | |
| Number of page(s) | 9 | |
| Section | Extragalactic astronomy | |
| DOI | https://doi.org/10.1051/0004-6361/202348135 | |
| Published online | 08 February 2024 | |
Evidence for enhanced star formation rates in z ∼ 0.35 cluster galaxies undergoing ram pressure stripping⋆
1
INAF – Osservatorio astronomico di Padova, Vicolo Osservatorio 5, 35122 Padova, Italy
e-mail: benedetta.vulcani@inaf.it
2
Instituto de Radioastronomia y Astrofisica, UNAM, Campus Morelia, AP 3-72, CP 58089 Morelia, Mexico
3
Univ. Lyon, Univ. Lyon 1, ENS de Lyon, CNRS, Centre de Recherche Astrophysique de Lyon UMR5574, 69230 Saint-Genis-Laval, France
Received:
3
October
2023
Accepted:
22
November
2023
Ram-pressure stripping (RPS) is the mechanism most often invoked to explain the observed differences between cluster and field galaxies. In the local Universe, its effect on the star-forming properties of the galaxies has been largely elucidated and the general consensus is that this process first compresses the gas available in galaxy disks, boosting the star formation for a limited amount of time, and then removes the remaining gas, leading to quenching. Much less is known about the effect and preponderance of RPS at higher redshifts, due to the lack of statistical samples. Exploiting VLT/MUSE observations of galaxies at 0.2 < z < 0.55 and a published catalog of ram-pressure-stripped galaxies, we compare the global star formation rate–mass (SFR–M*) relation of 29 cluster galaxies undergoing RPS to that of 26 undisturbed field and cluster galaxies that constitute our control sample. Stripping galaxies occupy the upper envelope of the SFR–M* relation of the control sample, showing a systematic enhancement of SFR at any given mass. The boost is > 3σ when considering the SFR occurring in both the tail and the disk of the galaxies. The enhancement is also seen on local scales: Considering spatially resolved data, ram-pressure stripped galaxies have large ΣSFR values overall, especially for Σ* > 107.5 M⊙ kpc−2. RPS seems to leave the same imprint on the SFR–M* and ΣSFR–Σ* relations both in the local Universe and at z ∼ 0.35.
Key words: galaxies: clusters: general / galaxies: evolution / galaxies: formation / galaxies: general / galaxies: star formation
Full Table 1 is available at the CDS via anonymous ftp to cdsarc.cds.unistra.fr (130.79.128.5) or via https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/682/A117
© The Authors 2024
Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
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