The GOGREEN survey: the internal dynamics of clusters of galaxies at redshift 0.9-1.4

Biviano, A.; van der Burg, R. F. J.; Balogh, M. L.; Munari, E.; Cooper, M. C.; De Lucia, G.; Demarco, R.; Jablonka, P.; Muzzin, A.; Nantais, J.; Old, L. J.; Rudnick, G.; Vulcani, B.; Wilson, G.; Yee, H. K. C.; Zaritsky, D.; Cerulo, P.; Chan, J.; Finoguenov, A.; Gilbank, D.; Lidman, C.; Pintos-Castro, I.; Shipley, H.

doi:10.48550/arxiv.2104.01183

Cited by 4 publications

(9 citation statements)

References 128 publications

(171 reference statements)

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“…The cluster centre is defined as the position of the brightest cluster galaxy (BCG) within each cluster, where the BCG is the most massive galaxy within 500 kpc of the main galaxy overdensity which has a redshift that is consistent with the cluster. We used the velocity dispersions, 𝜎, and 𝑅 200 calculated by Biviano et al (2021), except for the one cluster not in their sample, SpARCS0219, where we estimated the radius through 𝑅 200 = √ 3𝜎/10𝐻 (𝑧), where 𝐻 (𝑧) is the Hubble parameter at the cluster's redshift (Schneider 2006).…”

Section: The Gogreen and Gclass Cluster Surveysmentioning

confidence: 99%

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Satellite quenching was not important for z$\sim$1 clusters: most quenching occurred during infall

Werner,

Hatch,

Muzzin

et al. 2021

Preprint

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We quantify the relative importance of environmental quenching versus pre-processing in 𝑧 ∼ 1 clusters by analysing the infalling galaxy population in the outskirts of 15 galaxy clusters at 0.8 < 𝑧 < 1.4 drawn from the GOGREEN and GCLASS surveys. We find significant differences between the infalling galaxies and a control sample; in particular, an excess of massive quiescent galaxies in the infalling region. These massive infalling galaxies likely reside in larger dark matter haloes than similar-mass control galaxies because they have twice as many satellite galaxies. Furthermore, these satellite galaxies are distributed in an NFW profile with a larger scale radius compared to the satellites of the control galaxies. Based on these findings, we conclude that it may not be appropriate to use 'field' galaxies as a substitute for infalling pre-cluster galaxies when calculating the efficiency and mass dependency of environmental quenching in high redshift clusters. By comparing the quiescent fraction of infalling galaxies at 1 < 𝑅/R 200 < 3 to the cluster sample (𝑅/R 200 < 1) we find that almost all quiescent galaxies with masses > 10 11 M were quenched prior to infall, whilst up to half of lower mass galaxies were environmentally quenched after passing the virial radius. This means most of the massive quiescent galaxies in 𝑧 ∼ 1 clusters were self-quenched or pre-processed prior to infall.

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Section: The Gogreen and Gclass Cluster Surveysmentioning

confidence: 99%

“…Column 4 provides the redshift of the cluster. Columns 5 and 6 provide the intrinsic velocity dispersion and radius in proper Mpc fromBiviano et al (2021), except for the cluster marked with * where we estimated the radius from 𝜎 provided by GOGREEN DR1.…”

mentioning

confidence: 99%

Satellite quenching was not important for z$\sim$1 clusters: most quenching occurred during infall

Werner,

Hatch,

Muzzin

et al. 2021

Preprint

Self Cite

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“…This includes the cluster radius 𝑅 200 , defined as the radius within which the mean mass overdensity is 200 times the critical density at that redshift, and the corresponding mass 𝑀 200 . For most clusters, these are taken from Biviano et al (2021). SpARCS0219 and SpARCS1034 have too few spectroscopic members for the analysis in that paper, and the estimates of their 𝑅 200 are obtained from the velocity dispersions in Balogh et al (2021).…”

Section: The Gogreen Surveymentioning

confidence: 99%

“…When considering the spectroscopic subsample, we select cluster members as defined in Biviano et al (2021). The field sample consists of all non-members with spectroscopic redshifts 1 < 𝑧 < 1.5.…”

Section: Cluster Membershipmentioning

confidence: 99%

“…The width is arbitrarily defined, but selected to be a balance between making it small enough to reduce contamination from the other populations, while still wide enough to include a large population of transitioning galaxies. The definitions of field sample with spectra are identified as cluster members by Biviano et al (2021).…”

Section: Star-forming Quiescent and Green Valley Galaxiesmentioning

confidence: 99%

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The GOGREEN survey: Transition Galaxies and The Evolution of Environmental Quenching

McNab,

Balogh,

van der Burg

et al. 2021

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We measure the rate of environmentally-driven star formation quenching in galaxies at 𝑧 ∼ 1, using eleven massive (𝑀 ≈ 2 × 10 14 M ) galaxy clusters spanning a redshift range 1.0 < 𝑧 < 1.4 from the GOGREEN sample. We identify three different types of transition galaxies: "green valley" (GV) galaxies identified from their rest-frame (𝑁𝑈𝑉 − 𝑉) and (𝑉 − 𝐽) colours; "blue quiescent" (BQ) galaxies, found at the blue end of the quiescent sequence in (𝑈 − 𝑉) and (𝑉 − 𝐽) colour; and spectroscopic post-starburst (PSB) galaxies. We measure the abundance of these galaxies as a function of stellar mass and environment. For high stellar mass galaxies (log 𝑀/M > 10.5) we do not find any significant excess of transition galaxies in clusters, relative to a comparison field sample at the same redshift. It is likely that such galaxies were quenched prior to their accretion in the cluster, in group, filament or protocluster environments. For lower stellar mass galaxies (9.5 < log 𝑀/M < 10.5) there is a small but significant excess of transition galaxies in clusters, accounting for an additional ∼ 5 − 10 per cent of the population compared with the field. We show that our data are consistent with a scenario in which 20-30 per cent of low-mass, star-forming galaxies in clusters are environmentally quenched every Gyr, and that this rate slowly declines from 𝑧 = 1 to 𝑧 = 0. While environmental quenching of these galaxies may include a long delay time during which star formation declines slowly, in most cases this must end with a rapid (𝜏 < 1 Gyr) decline in star formation rate.

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The GOGREEN Survey: Evidence of an excess of quiescent disks in clusters at $1.0

Chan,

Wilson,

Balogh

et al. 2021

Preprint

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We present results on the measured shapes of 832 galaxies in 11 galaxy clusters at 1.0 < 𝑧 < 1.4 from the GOGREEN survey. We measure the axis ratio (𝑞), the ratio of the minor to the major axis, of the cluster galaxies from near-infrared Hubble Space Telescope imaging using Sérsic profile fitting and compare them with a field sample. We find that the median 𝑞 of both star-forming and quiescent galaxies in clusters increases with stellar mass, similar to the field. Comparing the axis ratio distributions between clusters and the field in four mass bins, the distributions for star-forming galaxies in clusters are consistent with those in the field. Conversely, the distributions for quiescent galaxies in the two environments are distinct, most remarkably in 10.1 ≤ log(𝑀/M ) < 10.5 where clusters show a flatter distribution, with an excess at low 𝑞. Modelling the distribution with oblate and triaxial components, we find that the cluster and field sample difference is consistent with an excess of flattened oblate quiescent galaxies in clusters. The oblate population contribution drops at high masses, resulting in a narrower 𝑞 distribution in the massive population than at lower masses. Using a simple accretion model, we show that the observed 𝑞 distributions and quenched fractions are consistent with a scenario where no morphological transformation occurs for the environmentally quenched population in the two intermediate mass bins. Our results suggest that environmental quenching mechanism(s) likely produce a population that has a different morphological mix than those resulting from the dominant quenching mechanism in the field.

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The GOGREEN survey: the internal dynamics of clusters of galaxies at redshift 0.9-1.4

Cited by 4 publications

References 128 publications

Satellite quenching was not important for z$\sim$1 clusters: most quenching occurred during infall

Satellite quenching was not important for z$\sim$1 clusters: most quenching occurred during infall

The GOGREEN survey: Transition Galaxies and The Evolution of Environmental Quenching

The GOGREEN Survey: Evidence of an excess of quiescent disks in clusters at $1.0

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