The galaxy mass-size relation in CARLA clusters and proto-clusters at 1.4 &lt; <i>z</i> &lt; 2.8: Larger cluster galaxy sizes

Afanasiev, Anton V.; Mei, S.; Fu, Hao; Shankar, Francesco; Amodeo, Stefania; Stern, Daniel; Cooke, Elizabeth A.; Gonzalez, Anthony H.; Noirot, Gaël; Rettura, Alessandro; Wylezalek, Dominika; Breuck, C. De; Hatch, N. A.; Stanford, S. A.; Vernet, J.

doi:10.1051/0004-6361/202244634

Cited by 12 publications

(2 citation statements)

References 155 publications

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“…Using single power-law fitting, the recent work by Afanasiev et al (2023) studied the size-mass relation for the galaxies in 15 clusters at 1.4 < z < 2.8 from the CARLA survey. It is found that the size-mass relation does not evolve much from z ∼ 2 to the present, and their sizes evolve in a similar way for cluster and field galaxies.…”

Section: Size-mass Relation Fitting and Environment Effectmentioning

confidence: 99%

Galaxy Clusters from the DESI Legacy Imaging Surveys. II. Environmental Effects on the Size–Mass Relation

Chen,

Gu,

Zou

et al. 2024

ApJ

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To investigate the environmental effects on the growth of galaxies, we study the size–mass relation across a broad range of environments with a vast sample of approximately 32 million galaxies at z < 0.5 from the DESI Legacy Imaging Surveys. This sample is divided into three subsamples representing galaxies within three different environments: brightest cluster galaxies (BCGs), other cluster galaxies, and field galaxies. The BCGs in our large sample are dominated by quiescent galaxies (QGs), while only a minority (∼13%) of BCGs are star-forming galaxies (SFGs). To demonstrate the influence of the environment on size growth, we attempt to observe the difference in size–mass relation for these three subsamples. In general, the slope differences between QGs and SFGs within various environments are significant and tend to be greater at higher redshifts. For the mass-complete subsamples at z < 0.5, BCGs are found to have the highest slope of size–mass relation, and no difference in size–mass relation is found between cluster members and field galaxies. To assess whether the observed slope differences stem from the variations in environment or mass distribution, we construct the mass-matched subsamples for QGs and SFGs. As a result, both QGs and SFGs show negligible differences in the slope of the size–mass relation among the galaxies within three distinct environments, indicating that stellar mass is the most fundamental factor driving the size evolution at z < 0.5, though the mass growth mode for QGs and SFGs may have been affected by galaxy environment.

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Section: Size-mass Relation Fitting and Environment Effectmentioning

confidence: 99%

Galaxy Clusters from the DESI Legacy Imaging Surveys. II. Environmental Effects on the Size–Mass Relation

Chen,

Gu,

Zou

et al. 2024

ApJ

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“…At z  1-2, however, the situation is less clear. A few recent works show that there is little environmental dependence on the sizes of SFGs at these redshifts (Afanasiev et al 2023;Strazzullo et al 2023), while some other works focusing on (proto)clusters at higher redshifts with more active star formation reveal that a significant fraction of massive cluster SFGs appear to be more compact than field galaxies (Wang et al 2016;Pérez-Martínez et al 2023). This indicates that these starbursting (proto) clusters, in which their massive SFG members are going through a major phase of mass assembly, may represent the best laboratory to witness environmental effects at work for cluster SFGs.…”

Section: Introductionmentioning

confidence: 99%

Accelerated Structural Evolution of Galaxies in a Starbursting Cluster at z = 2.51

Wang

et al. 2023

ApJL

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Structural properties of cluster galaxies during their peak formation epoch, z ∼ 2–4 provide key information on whether and how the environment affects galaxy formation and evolution. Based on deep Hubble Space Telescope (HST)/Wide Field Camera 3 (WFC3) imaging toward the z = 2.51 cluster, J1001, we explore environmental effects on the structure, color gradients, and stellar populations of a statistical sample of cluster star-forming galaxies (SFGs). We find that the cluster SFGs are on average smaller than their field counterparts. This difference is most pronounced at the high-mass end (M ⋆ > 1010.5 M ⊙), with nearly all of them lying below the mass–size relation of field galaxies. The high-mass cluster SFGs are also generally old, with a steep negative color gradient, indicating an early formation time likely associated with strong dissipative collapse. For low-mass cluster SFGs, we unveil a population of compact galaxies with steep positive color gradients that are not seen in the field. This suggests that the low-mass compact cluster SFGs may have already experienced strong environmental effects, e.g., tidal/ram pressure stripping, in this young cluster. These results provide evidence on the environmental effects at work in the earliest formed clusters with different roles in the formation of low- and high-mass galaxies.

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Morphology-density relation, quenching, and mergers in CARLA clusters and protoclusters at 1.4 < z < 2.8

Mei

Hatch

Amodeo

et al. 2023

A&A

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At redshifts of z 1.3, early-type galaxies (ETGs) and passive galaxies are mainly found in dense environments, such as galaxy clusters. However, it remains unclear whether these well-known morphology-density and passive-density relations have already been established at higher redshifts. To address this question, we performed an in-depth study of galaxies in 16 spectroscopically confirmed clusters at 1.3 < z < 2.8 from the Clusters Around Radio-Loud AGN (CARLA) survey. Our clusters span a total stellar mass in the range of 11.3 < log( M c * M ) < 12.6 (approximate halo mass in the range of 13.5 log(M c h M ) 14.5). Our main finding is that the morphology-density and passive-density relations are already in place at z ∼ 2. The cluster at z = 2.8 shows a similar fraction of ETG as in the other clusters in its densest region, however, only one cluster does not provide enough statistics to confirm that the morphology-density relation is already in place at z ∼ 3. The cluster ETG and passive fractions depend mainly on local environment and only slightly on galaxy mass; also, they do not depend on the global environment. At lower local densities, where ΣN < 700 gal/Mpc 2 , the CARLA clusters exhibit a similar ETG fraction as the field, in contradiction to clusters at z = 1, which already exhibit higher ETG fractions. This implies that the densest regions influence the morphology of galaxies first, with lower density local environments either taking longer or only influencing galaxy morphology at later cosmological times. Interestingly, we find evidence of high merger fractions in our clusters with respect to the CANDELS fields, but the merger fractions do not significantly depend on local environment. This suggests that merger remnants in the lowest density regions can reform disks fueled by cold gas flows, but those in the highest density regions are cut off from the gas supply and will become passive ETGs. The percentages of active ETGs, with respect to the total ETG population, are 21 ± 6% and 59 ± 14% at 1.35 < z <1.65 and 1.65 < z < 2.05, respectively, and about half of them are mergers or asymmetric in both redshift bins. All the spectroscopically confirmed CARLA clusters have properties that are consistent with clusters and proto-clusters, confirming that radio-loud active galactic nuclei are lighthouses for dense environments. The differences between our results and other findings that point to enhanced star formation and starbursts in cluster cores at similar redshifts are probably due to differences in the sample selection criteria; for example, selection of different environments hosting galaxies with different accretion and pre-processing histories.

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The galaxy mass-size relation in CARLA clusters and proto-clusters at 1.4 < z < 2.8: Larger cluster galaxy sizes

Cited by 12 publications

References 155 publications

Galaxy Clusters from the DESI Legacy Imaging Surveys. II. Environmental Effects on the Size–Mass Relation

Galaxy Clusters from the DESI Legacy Imaging Surveys. II. Environmental Effects on the Size–Mass Relation

Accelerated Structural Evolution of Galaxies in a Starbursting Cluster at z = 2.51

Morphology-density relation, quenching, and mergers in CARLA clusters and protoclusters at 1.4 < z < 2.8

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