H α-based star formation rates in and around <i>z</i> ∼ 0.5 EDisCS clusters

Cooper, Jennifer; Rudnick, Gregory; Brammer, Gabriel; Desjardins, Tyler D.; Mann, Justin L.; Weiner, Benjamin J.; Aragón-Salamanca, Alfonso; Lucia, G. De; Desai, Vandana; Finn, Rose; Jablonka, P.; Jaffé, Yara L.; Moustakas, John; Spérone-Longin, D.; Teplitz, Harry I.; Vulcani, Benedetta; Zaritsky, Dennis

doi:10.1093/mnras/stab3184

Cited by 5 publications

(1 citation statement)

References 129 publications

(196 reference statements)

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“…On the contrary, studies on galaxy samples based on a local parametrisation of environment do not find differences in the SFR-M of galaxies at different densities (Peng et al 2010;Wĳesinghe et al 2012, but see also Popesso et al 2011 at high z). Also Cooper et al (2022) do not detect a suppressed population at intermediate redshift, but their sensitivity limits are probably too high to detect the low-SFR population.…”

Section: Discussionmentioning

confidence: 92%

The Local Cluster Survey II: disc-dominated cluster galaxies with suppressed star formation

Finn

Vulcani

Rudnick

et al. 2023

Monthly Notices of the Royal Astronomical Society

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We investigate the role of dense environments in suppressing star formation by studying $\rm \log _{10}(M_\star /M_\odot ) > 9.7$ star-forming galaxies in nine clusters from the Local Cluster Survey (0.0137 < z < 0.0433) and a large comparison field sample drawn from the Sloan Digital Sky Survey. We compare the star-formation rate (SFR) versus stellar mass relation as a function of environment and morphology. After carefully controlling for mass, we find that in all environments, the degree of SFR suppression increases with increasing bulge-to-total (B/T) ratio. In addition, the SFRs of cluster and infall galaxies at a fixed mass are more suppressed than their field counterparts at all values of B/T. These results suggest a quenching mechanism that is linked to bulge growth that operates in all environments and an additional mechanism that further reduces the SFRs of galaxies in dense environments. We limit the sample to B/T ≤ 0.3 galaxies to control for the trends with morphology and find that the excess population of cluster galaxies with suppressed SFRs persists. We model the timescale associated with the decline of SFRs in dense environments and find that the observed SFRs of the cluster core galaxies are consistent with a range of models including: a mechanism that acts slowly and continuously over a long (2 − 5 Gyr) timescale, and a more rapid (<1 Gyr) quenching event that occurs after a delay period of 1 − 6 Gyr. Quenching may therefore start immediately after galaxies enter clusters.

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Section: Discussionmentioning

confidence: 92%

The Local Cluster Survey II: disc-dominated cluster galaxies with suppressed star formation

Finn

Vulcani

Rudnick

et al. 2023

Monthly Notices of the Royal Astronomical Society

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Ram pressure stripping in the z ∼ 0.5 galaxy cluster MS 0451.6-0305

Durret

Degott

Lobo

et al. 2022

A&A

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Context. The pressure exerted by the ambient hot X-ray gas on cluster galaxies can lead to the presence of ram pressure stripped (RPS) galaxies, characterized by asymmetric shapes, and, in some cases, tails of blue stars and/or X-ray gas, with increased star formation. Aims. With the aim of increasing the known sample of RPS galaxies at redshift z ∼ 0.5, notably higher than most RPS samples presently known, we extended our searches for such galaxies to the cluster MS 0451.6-0305. Methods. Our study is based on Hubble Space Telescope (HST) imaging in the F814W band (corresponding to a restframe wavelength of 529 nm), covering a region of about 6 × 6 Mpc2, an eight magnitude ground-based catalogue with photometric redshifts, and a spectroscopic redshift catalogue. We defined as cluster members a spectroscopic redshift sample of 359 galaxies within ±4σv of the mean cluster velocity, and a photometric redshift sample covering the [0.48, 0.61] range. We searched for RPS galaxies in the HST images and tested the error on their classification with a Zooniverse collaboration. We also computed the phase space diagram of RPS candidates in the spectroscopic sample. Finally, we ran the LePhare stellar population synthesis code through the GAZPAR interface to analyze and compare the properties of RPS and non-RPS galaxies. Results. We find 56 and 273 RPS candidates in the spectroscopic and photometric redshift samples, respectively. They are distributed throughout the cluster and tend to avoid high density regions. The phase space diagram gives the percentages of virialized, backsplash, and infall galaxies. RPS galaxy candidates typically show rather high star formation rates, young ages, and relatively low masses. We compare all our results to those previously obtained for the massive merging cluster MACS J0717+3745, at a similar redshift. Conclusions. This study increases by at least 56 objects if we only consider galaxies with spectroscopic redshifts, and probably much more if galaxies with photometric redshifts are taken into account. This study increases the number of RPS candidates at redshift z > 0.5, and confirms that they host, on average, younger stellar populations and strongly form stars when compared with non-RPS counterparts. The fact that RPS candidates with spectroscopic and with photometric redshifts have comparable properties shows that large samples of such objects could be gathered based on multi-band photometry only, a promising result in view of the very large imaging surveys planned in the coming years (DES, Euclid, LSST, etc.).

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A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE)

Boselli,

Fossati,

Côté

et al. 2023

A&A

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We use a complete set of deep narrow-band imaging data for 384 galaxies gathered during the Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE) to derive the first Hα luminosity function of the Virgo cluster within its virial radius. The data, which are sensitive to the emission of a single O-early B ionising star, allow us to cover the whole dynamic range of the Hα luminosity function (1036 ≤ L(Hα)≤1042 erg s−1). After they are corrected for [NII] contamination and dust attenuation, the data are used to derive the star formation rate function in the range 10−4 ≲ SFR ≲ 10 M⊙ yr−1. These luminosity functions are derived for gas-rich and gas-poor systems and for objects belonging to the different substructures of the Virgo cluster. They are then compared to those derived at other frequencies or using different tracers of star formation in Virgo, in other nearby and high-z clusters, in the field, and finally to those predicted by the IllustrisTNG cosmological hydrodynamical simulations (TNG50 and TNG100). The Hα luminosity function of the Virgo cluster is fairly flat (α = −1.07 when fitted with a Schechter function) in the range 1038.5 ≲ L(Hα)≲1040.5 erg s−1, and it abruptly decreases at lower luminosities. When compared to those derived for other nearby clusters and for the field, the slope and the characteristic luminosity of the Schechter function change as a function of the dynamical mass of the system, of the temperature of the X-rays gas, and of the dynamical pressure exerted on the interstellar medium of galaxies moving at high velocity within the intracluster medium. All these trends can be explained in a scenario in which the activity of star formation of galaxies is reduced in massive clusters due to their hydrodynamical interaction with the surrounding medium, suggesting once again that ram-pressure stripping is the dominant mechanism affecting galaxy evolution in local clusters of dynamical mass Mcluster ≳ 1014 M⊙. The comparison with the IllustrisTNG cosmological hydrodynamical simulations shows a more pronounced decrease at the faint end of the distribution. If the Virgo cluster is representative of typical nearby clusters of similar mass, this difference suggests that the stripping process in simulated galaxies in these environments is more efficient than observed.

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H α-based star formation rates in and around z ∼ 0.5 EDisCS clusters

Cited by 5 publications

References 129 publications

The Local Cluster Survey II: disc-dominated cluster galaxies with suppressed star formation

The Local Cluster Survey II: disc-dominated cluster galaxies with suppressed star formation

Ram pressure stripping in the z ∼ 0.5 galaxy cluster MS 0451.6-0305

A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE)

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