Evidence for a correlation between the sizes of quiescent galaxies and local environment to z ∼ 2

Lani, Caterina; Almaini, O.; Hartley, W. G.; Mortlock, Alice; Häußler, Boris; Chuter, Robert; Simpson, Chris; Wel, Arjen van der; Grützbauch, Ruth; Conselice, Christopher J.; Bradshaw, E. J.; Cooper, Michael C.; Faber, S. M.; Grogin, Norman A.; Kocevski, Dale D.; Koekemoer, Anton M.; Lai, Kamson

doi:10.1093/mnras/stt1275

Cited by 88 publications

(137 citation statements)

References 80 publications

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“…The evolution is reminiscent of that observed in previous studies , although it may be even weaker, compared to the field, because of the much higher environmental density (if the trends observed by Lani et al 2013 can be extended to clusters). At the same time CRSGs also become less disk-dominated with decreasing redshift.…”

Section: Discussionsupporting

confidence: 60%

Section: Size Evolutionmentioning

confidence: 97%

“…The degree of size evolution appears to depend on environment: Lani et al (2013) and Damjanov et al (2015) also find evidence that size evolution is weaker in high density environments (by as much as 50% in Lani et al 2013 when looking at their densest systems). However, note that our clusters are considerably more massive than any of the objects studied by Lani et al (2013) or Damjanov et al (2015). Given the already known passive evolution in colour and luminosity, the small change in size observed for these galaxies appears to suggest early formation and assembly, with little subsequent evolution, especially by mergers, and most other changes being due to internal processes or more gentle external inputs, a conclusion also reached by Huertas-Company et al (2015) at least for the more massive spheroidals in the field.…”

Section: Size Evolutionmentioning

confidence: 97%

“…The objects studied in Paper I are also massive clusters, already possessing hot X-ray gas atmospheres, and have richnesses in excess of Abell class 1 at z > 1; they will evolve into very rare (∼ 10 −7 Mpc −3 ) systems of richness class above 2 in the present-day universe. Unlike previous studies that select for overdensities in wide-field images (e.g., Bundy et al 2010;Lani et al 2013), which are too small to identify rich systems, our targets are chosen as massive clusters at their respective redshifts, likely among the most massive systems in the Universe at their epoch, tracing the highest peaks of the dark matter distribution. For comparison, the largest structure studied by Lani et al (2013), corresponding to the system identified by Papovich et al (2012), only has a velocity dispersion of ∼ 250 km s −1 (Tran et al 2015) and does not possess extended X-ray emission (Tanaka et al 2013), indicating a far lower environmental density than any cluster in our sample.…”

Section: Sample Of Clustersmentioning

confidence: 99%

“…Cluster early type galaxies instead appear to have larger sizes than a similarly massive sample of quiescent field galaxies (Cerulo et al 2014;Delaye et al 2014) and to evolve more slowly (Kelkar et al 2015). Galaxy size evolution may also have significant environmental dependencies (Lani et al 2013;Damjanov et al 2015). In our previous study (De Propris et al 2015, hereafter Paper I), we explored the morphologies of a sample of CRSGs drawn from four rich clusters at 1 < z < 1.4 (mean redshift z ∼ 1.25).…”

Section: Introductionmentioning

confidence: 99%

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Morphological evolution of cluster red sequence galaxies in the past 9 Gyr

Propris¹,

Bremer²,

Phillipps³

2016

Mon. Not. R. Astron. Soc.

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Galaxies arrive on the red sequences of clusters at high redshift (z > 1) once their star formation is quenched and evolve passively thereafter. However, we have previously found that cluster red sequence galaxies (CRSGs) undergo significant morphological evolution subsequent to the cessation of star formation, at some point in the past 9-10 Gyr. Through a detailed study of a large sample of cluster red sequence galaxies spanning 0.2 < z < 1.4 we elucidate the details of this evolution. Below z ∼ 0.5 − 0.6 (in the last 5-6 Gyr) there is little or no morphological evolution in the population as a whole, unlike in the previous 4-5 Gyrs. Over this earlier time (i) disklike systems with Sérsic n < 2 progressively disappear, as (ii) the range of their axial ratios similarly decreases, removing the most elongated systems (those consistent with thin disks seen at an appreciable inclination angle), and (iii) radial colour gradients (bluer outwards) decrease in an absolute sense from significant age-related gradients to a residual level consistent with the metallicity-induced gradients seen in low redshift cluster members. The distribution of their effective radii shows some evidence of evolution, consistent with growth of at most a factor < 1.5 between z ∼ 1.4 and z ∼ 0.5, significantly less than for comparable field galaxies, while the distribution of their central (< 1kpc) bulge surface densities shows no evolution at least at z < 1. A simple model involving the fading and thickening of a disk component after comparatively recent quenching (after z ∼ 1.5) around an otherwise passively evolving older spheroid component is consistent with all of these findings.

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Section: Discussionsupporting

confidence: 60%

Section: Size Evolutionmentioning

confidence: 97%

Section: Size Evolutionmentioning

confidence: 97%

Section: Sample Of Clustersmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Morphological evolution of cluster red sequence galaxies in the past 9 Gyr

Propris¹,

Bremer²,

Phillipps³

2016

Mon. Not. R. Astron. Soc.

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Interactions of galaxies outside clusters and massive groups

Yadav

Chen

2018

J Astrophys Astron

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We investigate the dependence of physical properties of galaxies on small and large scale density environment. The galaxy population consists of mainly passively evolving galaxies in comparatively low density regions of Sloan Digital Sky Survey (SDSS). We adopt (i) local density, ρ 20 , derived using adaptive smoothing kernel, (ii) projected distance, r p , to the nearest neighbor galaxy and (iii) the morphology of the nearest neighbor galaxy as various definitions of environment parameters of every galaxy in our sample. In order to detect long-range interaction effects we divide galaxy interactions into four cases depending on morphology of target and neighbor galaxies. This study builds upon an earlier study by Park & Choi (2009) by including improved definitions of target and neighbor galaxies thus enabling us to better understand the effect of "the nearest neighbor" interaction on target galaxy. We report that the impact of interaction on galaxy properties is detectable at least out to the pair separation corresponding to the virial radius of (the neighbor) galaxies. This turn out to be mostly between 210 and 360 h −1 kpc for galaxies included in our study. We report that early type fraction, for isolated galaxies with r p > r vir,nei are almost ignorant of the background density and, has a very weak density dependence for closed pairs. Star formation activity of a a galaxy is found to be crucially dependent on neighbor galaxy morphology. We find star formation activity parameters and structure parameters of galaxies to be independent of the large scale background density. We also exhibit that changing the absolute magnitude of the neighbor galaxies does not affect significantly the star formation activity of those target galaxies whose morphology and luminosities are fixed.

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JKCS 041: a Coma cluster progenitor atz= 1.803

Andreon

Newman

Trinchieri

et al. 2014

A&A

113

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Using deep two-color near-infrared HST imaging and unbiased grism spectroscopy, we present a detailed study of the z = 1.803 JKCS 041 cluster. We confirm, for the first time for a high-redshift cluster, a mass of log M 14.2 in solar units using four different techniques based on the X-ray temperature, the X-ray luminosity, the gas mass, and the cluster richness. JKCS 041 is thus a progenitor of a local system like the Coma cluster. Our rich dataset and the abundant population of 14 spectroscopically confirmed red-sequence galaxies allows us to explore the past star formation history of this system in unprecedented detail. Our most interesting result is a prominent red sequence down to stellar masses as low as log M/M = 9.8, corresponding to a mass range of 2 dex. These quiescent galaxies are concentrated around the cluster center with a core radius of 330 kpc. There are only few blue members and avoid the cluster center. In JKCS 041 quenching was therefore largely completed by a look-back time of 10 Gyr, and we can constrain the epoch at which this occurred via spectroscopic age-dating of the individual galaxies. Most galaxies were quenched about 1.1 Gyr prior to the epoch of observation. The less-massive quiescent galaxies are somewhat younger, corresponding to a decrease in age of 650 Myr per mass dex, but the scatter in age at fixed mass is only 380 Myr (at log M/M = 11). There is no evidence for multiple epochs of star formation across galaxies. The size-mass relation of quiescent galaxies in JKCS 041 is consistent with that observed for local clusters within our uncertainties, and we place an upper limit of 0.4 dex on size growth at fixed stellar mass (95% confidence). Comparing our data on JKCS 041 with 41 clusters at lower redshift, we find that the form of the mass function of red sequence galaxies has hardly evolved in the past 10 Gyr, both in terms of its faint-end slope and characteristic mass. Despite observing JKCS 041 soon after its quenching and the three-fold expected increase in mass in the next 10 Gyr, it is already remarkably similar to present-day clusters.

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Evidence for a correlation between the sizes of quiescent galaxies and local environment to z ∼ 2

Cited by 88 publications

References 80 publications

Morphological evolution of cluster red sequence galaxies in the past 9 Gyr

Morphological evolution of cluster red sequence galaxies in the past 9 Gyr

Interactions of galaxies outside clusters and massive groups

JKCS 041: a Coma cluster progenitor atz= 1.803

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