The KMOS Cluster Survey (KCS). III. Fundamental Plane of Cluster Galaxies at z ≃ 1.80 in JKCS 041*

Prichard, Laura; Davies, Roger L.; Beifiori, A.; Chan, J.; Cappellari, Michele; Houghton, R. C. W.; Mendel, J. Trevor; Bender, R.; Galametz, A.; Saglia, R.; Stott, John P.; Wilman, David J.; Lewis, Ian; Sharples, R. M.; Wegner, Michael

doi:10.3847/1538-4357/aa96a6

Cited by 24 publications

(23 citation statements)

References 127 publications

(288 reference statements)

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“…We assumed, as reference, the coefficients of the local The resulting evolution with redshift of M dyn /LB of cluster spheroids is ∆log(M dyn /LB)=(−0.5 ± 0.1)z, (filled black triangle), in agreement with many previous estimates (e Beifiori et al 2017;Prichard et al 2017). We do not detect significant differences in the evolution of M dyn /LB of individual clusters.…”

Section: The Evolution Of M Dyn /Lbsupporting

confidence: 71%

“…Other studies suggest that a structural evolution of individual galaxies (a variation of Re and σe) besides their simple aging is required to account for the FP evolution (e.g. Saglia et al 2010Saglia et al , 2016Beifiori et al 2017) even if progenitor bias could affect significantly this interpretation (Prichard et al 2017). Moreover, while some authors find a steepening of the FP slope with redshift (Jørgensen et al 2006;Jørgensen & Chiboucas 2013;di Serego Alighieri et al 2005), other authors do not detect any variation (e.g.…”

Section: Introductionmentioning

confidence: 99%

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The Fundamental Plane of cluster spheroidal galaxies at z ∼ 1.3: evidence for mass-dependent evolution

Saracco

Gargiulo

Barbera

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present spectroscopic observations obtained at the Large Binocular Telescope in the field of the cluster XLSSJ0223-0436 at z = 1.22. We confirm 12 spheroids cluster members and determine stellar velocity dispersion for 7 of them. We combine these data with those in the literature for clusters RXJ0848+4453 at z = 1.27 (8 galaxies) and XMMJ2235-2557 at z = 1.39 (7 galaxies) to determine the Fundamental Plane of cluster spheroids. We find that the FP at z ∼ 1.3 is offset and rotated (∼ 3σ) with respect to the local FP. The offset corresponds to a mean evolution ∆log(M dyn /L B )=(-0.5±0.1)z. High-redshift galaxies follow a steeper mass-dependenthigher-mass galaxies (log(M dyn /M ⊙ )≥11.5) have a higher-formation redshift (z f ≥6.5) than lower-mass ones (z f ≤2 for log(M dyn /M ⊙ ≤10)), with a median z f ≃ 2.5 for the whole sample. Also, galaxies with higher stellar mass density host stellar populations formed earlier than those in lower density galaxies. At fixed IMF, M dyn /M * varies systematically with mass and mass density. It follows that the evolution of the stellar populations (M * /L B ) accounts for the observed evolution of M dyn /L B for M dyn > 10 11 M ⊙ galaxies, while accounts for ∼85% of the evolution at M dyn < 10 11 M ⊙ . We find no evidence in favour of structural evolution of individual galaxies, while we find evidences that spheroids later added to the population may account for the observed discrepancy between ∆log(M dyn /L B ) and ∆ log(M * /L B ) at masses < 10 11 M ⊙ . Thus, the evolution of the FP of cluster spheroids is consistent with the mass-dependent and mass density-dependent evolution of their stellar populations superimposed to a minor contribution of spheroids joining the population at later times.

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Section: The Evolution Of M Dyn /Lbsupporting

confidence: 71%

Section: Introductionmentioning

confidence: 99%

The Fundamental Plane of cluster spheroidal galaxies at z ∼ 1.3: evidence for mass-dependent evolution

Saracco

Gargiulo

Barbera

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…5 also shows for reference the constraints derived using only the RS or IRAC colors, respectively (blue and green symbols, as indicated). In particular, following results from previous investigations of the formation epoch of bright RS galaxies in massive clusters in this redshift range (e.g., Strazzullo et al 2010;Andreon et al 2014;Cooke et al 2016;Beifiori et al 2017;Prichard et al 2017), the RS-only redshift estimate obtained assuming a formation redshift z f = 3 as typically suggested by such studies is explicitly marked in the figure. Finally, in both panels we also show (red stars) the available spectroscopic redshifts for the clusters SPT-CLJ2040 (z = 1.478; Bayliss et al 2014) and SPT-CLJ0607 (z = 1.401; Khullar et al 2019), and the current best redshift constraint for SPT-CLJ0459 (see discussion below).…”

Section: Cluster Redshift Constraintsmentioning

confidence: 96%

Galaxy populations in the most distant SPT-SZ clusters

Strazzullo

Pannella

Mohr

et al. 2019

A&A

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We present the first results from a galaxy population study in the highest redshift galaxy clusters identified in the 2500 deg2 South Pole Telescope Sunyaev Zel’dovich effect (SPT-SZ) survey, which is sensitive to M500 ≳ 3 × 1014 M⊙ clusters from z ∼ 0.2 out to the highest redshifts where such massive structures exist. The cluster selection is to first order independent of galaxy properties, making the SPT-SZ sample particularly well suited for cluster galaxy population studies. We carried out a four-band imaging campaign with the Hubble and Spitzer Space Telescopes of the five z ≳ 1.4, S/NSZE > 5 clusters, that are among the rarest most massive clusters known at this redshift. All five clusters show clear overdensities of red galaxies whose colors agree with the initial cluster redshift estimates, although one (SPT-CLJ0607–4448) shows a galaxy concentration much less prominent than the others. The highest redshift cluster in this sample, SPT-CLJ0459–4947 at z ∼ 1.72, is the most distant M500 > 1014 M⊙ cluster discovered thus far through its intracluster medium, and is one of only three known clusters in this mass range at z ≳ 1.7, regardless of selection. Based on UVJ-like photometric classification of quiescent and star-forming galaxies, we find that the quiescent fraction in the cluster central regions (r/r500 < 0.7) is higher than in the field at the same redshift, with corresponding environmental quenching efficiencies typically in the range ∼0.5 − 0.8 for stellar masses log(M/M⊙) > 10.85. We have explored the impact of emission from star formation on the selection of this sample, concluding that all five clusters studied here would still have been detected with S/NSZE> 5, even if they had the same quiescent fraction as measured in the field. Our results thus point towards an efficient suppression of star formation in the central regions of the most massive clusters, occurring already earlier than z ∼ 1.5.

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“…In paper I of KCS (Beifiori et al 2017), we present the analysis of the fundamental plane for three overdensities at 1.39 < z < 1.61 in the KCS sample. The structural and kinematic properties of the galaxies in the overdensity at z = 1.8 are presented in paper III of KCS (Prichard et al 2017). The study of the stellar populations of the passive galaxies in the three overdensities in Beifiori et al (2017) will be presented in a forthcoming paper (Houghton et al, in prep).…”

Section: Introductionmentioning

confidence: 99%

The KMOS Cluster Survey (KCS). II. The Effect of Environment on the Structural Properties of Massive Cluster Galaxies at Redshift 1.39 < z < 1.61*

Chan

Beifiori

Saglia

et al. 2018

ApJ

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We present results on the structural properties of massive passive galaxies in three clusters at 1.39 < z < 1.61 from the KMOS Cluster Survey. We measure light-weighted and mass-weighted sizes from optical and nearinfrared Hubble Space Telescope imaging and spatially resolved stellar mass maps. The rest-frame R-band sizes of these galaxies are a factor of ∼ 2 − 3 smaller than their local counterparts. The slopes of the relation between the stellar mass and the light-weighted size are consistent with recent studies in clusters and the field. Their mass-weighted sizes are smaller than the rest frame R-band sizes, with an average mass-weighted to light-weighted size ratio that varies between ∼ 0.45 and 0.8 among the clusters. We find that the median light-weighted size of the passive galaxies in the two more evolved clusters is ∼ 24% larger than for field galaxies, independent of the use of circularized effective radii or semi-major axes. These two clusters also show a smaller size ratio than the less evolved cluster, which we investigate using color gradients to probe the underlying M * /L H 160 gradients. The median color gradients are ∇z − H ∼ −0.4 mag dex −1 , twice the local value. Using stellar populations models, these gradients are best reproduced by a combination of age and metallicity gradients. Our results favor the minor merger scenario as the dominant process responsible for the observed galaxy properties and the environmental differences at this redshift. The environmental differences support that clusters experience accelerated structural evolution compared to the field, likely via an epoch of enhanced minor merger activity during cluster assembly.

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The KMOS Cluster Survey (KCS). III. Fundamental Plane of Cluster Galaxies at z ≃ 1.80 in JKCS 041*

Cited by 24 publications

References 127 publications

The Fundamental Plane of cluster spheroidal galaxies at z ∼ 1.3: evidence for mass-dependent evolution

The Fundamental Plane of cluster spheroidal galaxies at z ∼ 1.3: evidence for mass-dependent evolution

Galaxy populations in the most distant SPT-SZ clusters

The KMOS Cluster Survey (KCS). II. The Effect of Environment on the Structural Properties of Massive Cluster Galaxies at Redshift 1.39 < z < 1.61*

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