A TALE OF DWARFS AND GIANTS: USING A<i>z</i>= 1.62 CLUSTER TO UNDERSTAND HOW THE RED SEQUENCE GREW OVER THE LAST 9.5 BILLION YEARS

Rudnick, Gregory; Tran, Kim‐Vy H.; Papovich, Casey; Momcheva, Ivelina; Willmer, Christopher N. A.

doi:10.1088/0004-637x/755/1/14

Cited by 55 publications

(85 citation statements)

References 92 publications

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“…Although a significant population of massive, quiescent, early-type galaxies in dense environments has been identified out to z 2 Gobat et al 2013), the results of Snyder et al (2012) indicate that most of the stellar mass on the red sequence is assembled at z < 2. This is in line with the findings by Rudnick et al (2012), who investigated in detail the quiescent population of the system XMM-LSS J02182-05102 at z = 1.62 and pointed out the importance of merging for the red-sequence build-up. However, the partial red sequences that are already in place in cluster environments at z > 1.4 appear to be all broadly consistent in color and slope with simple expectations from galaxy evolution models where the bulk of stars formed around z ∼ 3 (e.g., Snyder et al 2012;Hilton et al 2009;Muzzin et al 2013;Tanaka et al 2013;Willis et al 2013).…”

Section: Comparison With Other High-z Galaxy Clusterssupporting

confidence: 91%

“…This cut-off magnitude in observed red galaxy counts is directly related to the turn-over point of the quiescent galaxy luminosity function, as found previously in a high-z group environment at similar redshift (Rudnick et al 2012). …”

Section: Faint End Of the Red Sequencesupporting

confidence: 85%

“…3.6 confirms the reported trends that the faint end of the red sequence is increasingly underpopulated with increasing redshift (e.g., De Lucia et al 2004;Koyama et al 2007;Tanaka et al 2007Tanaka et al , 2013Stott et al 2009;Rudnick et al 2009Rudnick et al , 2012Fassbender et al 2011b;Lerchster et al 2011). Assuming a stellar mass of 10 11 M for a galaxy with characteristic magnitude Ks* (Strazzullo et al 2006), the observed truncation limit in XDCP J0044.0-2033 can be approximated to be on the order of M * ,trunc 0.25 × M * (Ks * ) ∼ 2.5 × 10 10 M .…”

Section: Comparison With Other High-z Galaxy Clusterssupporting

confidence: 83%

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Galaxy population properties of the massive X-ray luminous galaxy cluster XDCP J0044.0-2033 atz= 1.58

Fassbender

Nastasi

Santos

et al. 2014

A&A

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Context. Recent observational progress has enabled the detection of galaxy clusters and groups out to very high redshifts and for the first time allows detailed studies of galaxy population properties in these densest environments in what was formerly known as the "redshift desert" at z > 1.5. Aims. We aim to investigate various galaxy population properties of the massive X-ray luminous galaxy cluster XDCP J0044.0-2033 at z = 1.58, which constitutes the most extreme currently known matter-density peak at this redshift. Methods. We analyzed deep VLT/HAWK-I near-infrared data with an image quality of 0.5 and limiting Vega magnitudes (50% completeness) of 24.2 in J-and 22.8 in the Ks band, complemented by similarly deep Subaru imaging in i and V, Spitzer observations at 4.5 μm, and new spectroscopic observations with VLT/FORS 2. Results. We detect a cluster-associated excess population of about 90 galaxies, most of them located within the inner 30 (250 kpc) of the X-ray centroid, which follows a centrally peaked, compact NFW galaxy surface-density profile with a concentration of c 200 10. Based on the Spitzer 4.5 μm imaging data, we measure a total enclosed stellar mass of M * 500 (6.3 ± 1.6) × 10 12 M and a resulting stellar mass fraction of f * ,500 = M * ,500 /M 500 = (3.3 ± 1.4)%, consistent with local values. The total J-and Ks-band galaxy luminosity functions of the core region yield characteristic magnitudes J* and Ks* consistent with expectations from simple z f = 3 burst models. However, a detailed look at the morphologies and color distributions of the spectroscopically confirmed members reveals that the most massive galaxies are undergoing a very active mass-assembly epoch through merging processes. Consequently, the bright end of the cluster red sequence is not in place, while a red-locus population is present at intermediate magnitudes [Ks*, Ks* + 1.6], which is then sharply truncated at magnitudes fainter than Ks* + 1.6. The dominant cluster-core population comprises post-quenched galaxies transitioning toward the red sequence at intermediate magnitudes, while additionally a significant blue-cloud population of faint star-forming galaxies is present even in the densest central regions. Based on a color−color selection performed to separate different cluster galaxy types, we find that the blue star-forming population is concentrated in clumpy structures and dominates in particular at and beyond the R 500 radius. On the other hand, the fraction of post-starburst galaxies steadily increases toward the center, while the red-locus population and red-sequence transition galaxies seem to reach their peak fractions already at intermediate cluster-centric radii of about r ∼ 200 kpc. Conclusions. Our observations support the scenario in which the dominant effect of the dense z 1.6 cluster environment is an accelerated massassembly timescale (∼1 Gyr or shorter) through merging activity that is responsible for driving core galaxies across the mass-quenching threshold of log(M * /M ) 10.4. Beyond this ma...

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Section: Comparison With Other High-z Galaxy Clusterssupporting

confidence: 91%

Section: Faint End Of the Red Sequencesupporting

confidence: 85%

Section: Comparison With Other High-z Galaxy Clusterssupporting

confidence: 83%

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Galaxy population properties of the massive X-ray luminous galaxy cluster XDCP J0044.0-2033 atz= 1.58

Fassbender

Nastasi

Santos

et al. 2014

A&A

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“…A differential comparison that ameliorates these difficulties is to compare the number of red sequence galaxies no fainter than 1.5 magnitudes from the brightest quiescent galaxy, the flux limit of our data. In this magnitude interval there are 5 red sequence galaxies in MS1054-0321 (Figure 1 of Mei et al, 2009), 4 in IDCS J1426.5+3508 (Figure 6 of Stanford et al, 2012), 8 in IDCS J1433.2+3306 (Table 2 of Zeimann et al, 2012) and 12 in ClG J0218.3-0510 (Figure 2 of Rudnick et al, 2012). In so far as we can compare the clusters, there are similar numbers of red sequence galaxies.…”

Section: Is There a Red Sequence In The Large Scale Structure?mentioning

confidence: 76%

A Large-Scale Structure at Redshift 1.71 in the Lockman Hole

Henry

Aoki²,

Finoguenov

et al. 2013

ApJ

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We previously identified LH146, a diffuse X-ray source in the Lockman Hole, as a galaxy cluster at redshift 1.753. The redshift was based on one spectroscopic value, buttressed by seven additional photometric redshifts. We here confirm the previous spectroscopic redshift and present concordant spectroscopic redshifts for an additional eight galaxies. The average of these nine redshifts is 1.714 ± 0.012 (error on mean). Scrutiny of the galaxy distribution in redshift and the plane of the sky shows that there are two concentrations of galaxies near the X-ray source. In addition there are three diffuse X-ray sources spread along the axis connecting the galaxy concentrations. LH146 is one of these three and lies approximately at the center of the two galaxy concentrations and the outer two diffuse X-ray sources. We thus conclude that LH146 is at the redshift initially reported but it is not a single virialized galaxy cluster as previously assumed. Rather it appears to mark the approximate center of a larger region containing more objects. For brevity we term all these objects and their alignments as large scale structure. The exact nature of LH146 itself remains unclear.

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“…Distant clusters are the statistical ancestors of present-day clusters, so we can study the processes that drive galaxy evolution by comparing the galaxies within clusters at low and high redshifts. Distant clusters contain more blue, spiral galaxies with higher star formation rates than cluster members today (Poggianti et al 2009b), as well as a large fraction of post-starburst galaxies (Poggianti et al 2009a;Muzzin et al 2012) and a lack of low-mass red galaxies (e.g., De Lucia et al 2004;Rudnick et al 2012), all of which implies strong galaxy evolution.…”

Section: Introductionmentioning

confidence: 99%

The structure and evolution of a forming galaxy cluster atz= 1.62

Hatch

Muldrew

Cooke

et al. 2016

Mon. Not. R. Astron. Soc.

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We present a comprehensive picture of the Cl 0218.3−0510 protocluster at z = 1.623 across 10 co-moving Mpc. Using filters that tightly bracket the Balmer and 4000Å breaks of the protocluster galaxies we obtain precise photometric redshifts resulting in a protocluster galaxy sample that is 89 ± 5% complete and has a contamination of only 12 ± 5%. Both star forming and quiescent protocluster galaxies are located allowing us to map the structure of the forming cluster for the first time. The protocluster contains 6 galaxy groups, the largest of which is the nascent cluster. Only a small minority of the protocluster galaxies are in the nascent cluster (11%) or in the other galaxy groups (22%), as most protocluster galaxies reside between the groups. Unobscured star forming galaxies predominantly reside between the protocluster's groups, whereas red galaxies make up a large fraction of the groups' galactic content, so observing the protocluster through only one of these types of galaxies results in a biased view of the protocluster's structure. The structure of the protocluster reveals how much mass is available for the future growth of the cluster and we use the Millennium Simulation, scaled to a Planck cosmology, to predict that Cl 0218.3−0510 will evolve into a 2.7 +3.9 −1.7 × 10 14 M ⊙ cluster by the present day.

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A TALE OF DWARFS AND GIANTS: USING Az= 1.62 CLUSTER TO UNDERSTAND HOW THE RED SEQUENCE GREW OVER THE LAST 9.5 BILLION YEARS

Cited by 55 publications

References 92 publications

Galaxy population properties of the massive X-ray luminous galaxy cluster XDCP J0044.0-2033 atz= 1.58

Galaxy population properties of the massive X-ray luminous galaxy cluster XDCP J0044.0-2033 atz= 1.58

A Large-Scale Structure at Redshift 1.71 in the Lockman Hole

The structure and evolution of a forming galaxy cluster atz= 1.62

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