SPECTROSCOPIC CONFIRMATION OF A PROTOCLUSTER AT z ≈ 3.786

Dey, Arjun; Lee, Kyoung-Soo; Reddy, Naveen A.; Cooper, Michael C.; Inami, Hanae; Hong, Sungryong; Gonzalez, Anthony H.; Jannuzi, Buell T.

doi:10.3847/0004-637x/823/1/11

Cited by 56 publications

(96 citation statements)

References 65 publications

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“…An overdensity is found by Saito et al (2015) around the radio galaxy TN J1338-1942 at redshift 3.1, with δ Σ = 2.8 ± 0.5. At z = 3.78, two or three overdensities with similar δ Σ values are found by Lee et al (2014); Dey et al (2016), with δ Σ = 2.5−2.8. The largest overdensity by far lies in the SSA22 field (Steidel et al 2000), with a surface density contrast δ Σ = 5 ± 2 (Steidel et al 2000; Matsuda et al 2004Matsuda et al , 2005Yamada et al 2012).…”

Section: Measurement Of Surface and Volume Overdensitymentioning

confidence: 68%

Discovery of a Protocluster Associated with a Lyα Blob Pair at z = 2.3

Badescu

Yang

Bertoldi

et al. 2017

ApJ

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Bright Lyα blobs (LABs) -extended nebulae with sizes of ∼100 kpc and Lyα luminosities of ∼10 44 erg s −1 -often reside in overdensities of compact Lyα emitters (LAEs) that may be galaxy protoclusters. The number density, variance, and internal kinematics of LABs suggest that they themselves trace group-like halos. Here we test this hierarchical picture, presenting deep, wide-field Lyα narrowband imaging of a 1• × 0.5• region around a LAB pair at z = 2.3 discovered previously by a blind survey. We find 183 Lyα emitters, including the original LAB pair and three new LABs with Lyα luminosities of (0.9-1.3)×1043 erg s −1 and isophotal areas of 16-24 arcsec 2 . Using the LAEs as tracers and a new kernel density estimation method, we discover a large-scale overdensity (Boötes J1430+3522) with a surface density contrast of δ Σ = 2.7, a volume density contrast of δ ∼ 10.4, and a projected diameter of ≈ 20 comoving Mpc. Comparing with cosmological simulations, we conclude that this LAE overdensity will evolve into a present-day Coma-like cluster with log (M/M ) ∼ 15.1 ± 0.2. In this and three other wide-field LAE surveys re-analyzed here, the extents and peak amplitudes of the largest LAE overdensities are similar, not increasing with survey size, implying that they were indeed the largest structures then and do evolve into rich clusters today. Intriguingly, LABs favor the outskirts of the densest LAE concentrations, i.e., intermediate LAE overdensities of δ Σ = 1 − 2. We speculate that these LABs mark infalling proto-groups being accreted by the more massive protocluster.

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Section: Measurement Of Surface and Volume Overdensitymentioning

confidence: 68%

Discovery of a Protocluster Associated with a Lyα Blob Pair at z = 2.3

Badescu

Yang

Bertoldi

et al. 2017

ApJ

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“…For example, Lee et al (2014) found three overdensities at z = 3.78 within a 75 × 75 × 25 cMpc 3 volume. Dey et al (2016) provided follow-up spectroscopic coverage to that extended system, which may be part of a filament stretching ∼ 170 cMpc. More recently, Zheng et al 3 around an overdensity discovered by Balestra et al (2010) and listed in the CCPC1 as CCPC-z28-002.…”

Section: Mass Estimatesmentioning

confidence: 99%

THE CANDIDATE CLUSTER AND PROTOCLUSTER CATALOG (CCPC). II. SPECTROSCOPICALLY IDENTIFIED STRUCTURES SPANNING 2 < z < 6.6

Franck

McGaugh

2016

ApJ

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The Candidate Cluster and Protocluster Catalog (CCPC) is a list of objects at redshifts z > 2 composed of galaxies with spectroscopically confirmed redshifts that are coincident on the sky and in redshift. These protoclusters are identified by searching for groups in volumes corresponding to the expected size of the most massive protoclusters at these redshifts. In CCPC1 we identified 43 candidate protoclusters among 14,000 galaxies between 2.74 < z < 3.71. Here we expand our search to more than 40,000 galaxies with spectroscopic redshifts z > 2.00, resulting in an additional 173 candidate structures. The most significant of these are 36 protoclusters with overdensities δ gal > 7. We also identify three large proto-supercluster candidates containing multiple protoclusters at z = 2.3, 3.5 and z = 6.56. Eight candidates with N ≥ 10 galaxies are found at redshifts z > 4.0. The last system in the catalog is the most distant spectroscopic protocluster candidate known to date at z = 6.56.

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“…Lyα equivalent widths (EWs) have been used extensively as an estimator for the star formation rate of galaxies in the high redshift universe (Dijkstra & Westra 2010), find evidence that the EWs are stronger at z = 2.8. Dey et al (2016) do not find such EW dependence at z = 3.8, while Toshikawa et al (2016) finds smaller EW 0 in a protocluster at z = 3.67 when compared to the field. Hayashi et al (2011) and Hayashi et al (2012) find only the reddest galaxies in their structures have statistically significant environmental dependence.…”

Section: Introductionmentioning

confidence: 85%

“…Similar studies that trace the Lyα emission of protocluster galaxies find that they are generally brighter , less dusty (although this may be a selection effect), and younger (Dey et al 2016). Lyα equivalent widths (EWs) have been used extensively as an estimator for the star formation rate of galaxies in the high redshift universe (Dijkstra & Westra 2010), find evidence that the EWs are stronger at z = 2.8.…”

Section: Introductionmentioning

confidence: 96%

“…These protoclusters exist at a wide range of redshifts, each within their infancy and characterized by the rapid changes expected in a ΛCDM universe (Chiang et al 2013;Muldrew et al 2015). Particularly for the individual case studies (Hatch et al 2011;Hayashi et al 2012;Cooke et al 2015;Dey et al 2016;Zheng et al 2016), different instruments and selection techniques were used, which targeted different populations of galaxies. Furthermore, the galaxy properties themselves were not all analyzed in the same manner.…”

Section: Introductionmentioning

confidence: 99%

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Spitzer’s View of the Candidate Cluster and Protocluster Catalog (CCPC)

Franck

McGaugh

2017

ApJ

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The Candidate Cluster and Protocluster Catalog (CCPC) contains 218 galaxy overdensities composed of more than 2000 galaxies with spectroscopic redshifts spanning the first few Gyrs after the Big Bang (2.0 ≤ z < 6.6). We use Spitzer archival data to track the underlying stellar mass of these overdense regions in various temporal cross sections by building rest-frame near-infrared luminosity functions across the span of redshifts.This exercise maps the stellar growth of protocluster galaxies, as halos in the densest environments should be the most massive from hierarchical accretion. The characteristic apparent magnitude, m * (z), is relatively flat from 2.0 ≤ z < 6.6, consistent with a passive evolution of an old stellar population. This trend maps smoothly to lower redshift results of cluster galaxies from other works. We find no difference in the luminosity functions of galaxies in the field versus protoclusters at a given redshift, apart from their density.

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SPECTROSCOPIC CONFIRMATION OF A PROTOCLUSTER AT z ≈ 3.786

Cited by 56 publications

References 65 publications

Discovery of a Protocluster Associated with a Lyα Blob Pair at z = 2.3

Discovery of a Protocluster Associated with a Lyα Blob Pair at z = 2.3

THE CANDIDATE CLUSTER AND PROTOCLUSTER CATALOG (CCPC). II. SPECTROSCOPICALLY IDENTIFIED STRUCTURES SPANNING 2 < z < 6.6

Spitzer’s View of the Candidate Cluster and Protocluster Catalog (CCPC)

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