J/A+A/682/A117 Star formation rates in z∼0.35 cluster galaxies (Vulcani+, 2024)
Evidence for enhanced star formation rates in z∼0.35 cluster galaxies undergoing
ram pressure stripping.
Vulcani B., Moretti A., Poggianti M.B., Radovich M., Werle A.,
Gullieuszik M., Fritz J., Bacchini C., Richard J.
<Astron. Astrophys. 682, A117 (2024)>
=2024A&A...682A.117V 2024A&A...682A.117V (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; Galaxies ; Redshifts
Keywords: galaxies: clusters: general - galaxies: evolution -
galaxies: general - galaxies: star formation
Abstract:
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-Mstar) 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-Mstar relation of the control sample, showing a systematic
enhancement of SFR at any given mass. The boost is > 3sigma 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
Sigma_SFR values overall, especially for Sigma_star
>107.5M☉/kpc^2. RPS seems to leave the same imprint on the
SFR-Mstar and SigmaSFR-Sigmastar relations both in the local
Universe and at z∼0.35.
Description:
Properties of the galaxies used in the analysis. Data are coming from
MUSE/VLT observations.
We measured SFRs from Hα emission for 29 ram-pressure-stripped
galaxies (25 with ionized tails, 4 truncated disks) and 26
control-sample galaxies.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 172 55 Properties of the galaxies analyzed in this paper
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Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 12 A12 --- ID Galaxy ID
16- 17 I2 h RAh Right ascension (J2000)
19- 20 I2 min RAm Right ascension (J2000)
22- 27 F6.3 s RAs Right ascension (J2000)
29 A1 --- DE- Declination sign (J2000)
30- 31 I2 deg DEd Declination (J2000)
33- 34 I2 arcmin DEm Declination (J2000)
36- 40 F5.2 arcsec DEs Declination (J2000)
42- 47 F6.4 --- z Spectroscopic redshift
49 I1 --- Memb [0/1] Cluster membership
(1= cluster member, 0 = field galaxy)
51 I1 --- Class [0/9] Galaxy class
(0 = undisturbed, 1 = RPS, 9 = unknown)
53- 68 E16.11 Msun Mass Stellar mass
70- 85 E16.11 Msun e_Mass Stellar mass error
87-107 F21.19 Msun/yr SFRdisk Disk SFR
109-130 E22.20 Msun/yr e_SFRdisk Disk SFR error
131-150 F20.18 Msun/yr SFRtot Total SFR
152-172 E21.20 Msun/yr e_SFRtot Total SFR error
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Acknowledgements:
Benedetta Vulcani, benedetta.vulcani(at)inaf.it
(End) Patricia Vannier [CDS] 11-Dec-2023