VIMOS Ultra-Deep Survey (VUDS): Witnessing the assembly of a massive cluster at<i>z</i>~ 3.3

Lemaux, B. C.; Cucciati, O.; Tasca, L.; Fèvre, O. Le; Zamorani, G.; Cassata, P.; Garilli, B.; Brun, V. Le; Maccagni, D.; Pentericci, L.; Thomas, Romain; Vanzella, E.; Zucca, E.; Amorín, R.; Bardelli, S.; Capak, P.; Cassarà, L. P.; Castellano, M.; Cimatti, A.; Cuby, Jean-Gabriel; Torre, S. de la; Durkalec, A.; Fontana, A.; Giavalisco, Mauro; Grazian, A.; Hathi, N. P.; Ilbert, O.; Moreau, C.; Paltani, S.; Ribeiro, B.; Salvato, M.; Schaerer, D.; Scodeggio, M.; Sommariva, V.; Talia, M.; Taniguchi, Y.; Tresse, L.; Vergani, D.; Wang, P. W.; Charlot, S.; Contini, T.; Fotopoulou, S.; Gal, R. R.; Kocevski, Dale D.; López-Sanjuan, C.; Lubin, Lori M.; Mellier, Y.; Sadibekova, T.; Scoville, N. Z.

doi:10.1051/0004-6361/201423828

Cited by 63 publications

(94 citation statements)

References 195 publications

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“…A well-defined selection function will allow us to robustly quantify the average properties of the galaxies in such a dense environment and to compare them with the galaxies in the field at the same z and with other overdensities found in the literature (e.g. Lemaux et al 2014). The synergy of spectroscopy and multi-band photometry in next-generation surveys like Euclid will allow several proto-cluster structures to be identified thanks to combination of depth and large surveyed areas.…”

Section: Discussionmentioning

confidence: 99%

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Discovery of a rich proto-cluster atz= 2.9 and associated diffuse cold gas in the VIMOS Ultra-Deep Survey (VUDS)

Cucciati

Zamorani

Lemaux

et al. 2014

A&A

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High-density environments are crucial places for studying the link between hierarchical structure formation and stellar mass growth in galaxies. In this work, we characterise a massive proto-cluster at z = 2.895 that we found in the COSMOS field using the spectroscopic sample of the VIMOS Ultra-Deep Survey (VUDS). This is one of the rare structures at z ∼ 3 not identified around an active galactic nucleus (AGN) or a radio galaxy, thus it represents an ideal laboratory for investigating the formation of galaxies in dense environments. The structure comprises 12 galaxies with secure spectroscopic redshift in an area of ∼7 × 8 , in a total z range of Δz = 0.016. The measured galaxy number overdensity is δ g = 12 ± 2. This overdensity has a total mass of M ∼ 8.1 × 10 14 M in a volume of 13 × 15 × 17 Mpc 3 . Simulations indicate that such an overdensity at z ∼ 2.9 is a proto-cluster, which will collapse in a cluster of total mass M z=0 ∼ 2.5 × 10 15 M at z = 0, i.e. a massive cluster in the local Universe. We analysed the properties of the galaxies within the overdensity, and we compared them with a control sample at the same redshift but outside the overdensity. We could not find any statistically significant difference between the properties (stellar mass, star formation rate, specific star formation rate, NUV-r and r − K colours) of the galaxies inside and outside the overdensity, but this result might be due to the lack of statistics or possibly to the specific galaxy population sampled by VUDS, which could be less affected by environment than the other populations not probed by the survey. The stacked spectrum of galaxies in the background of the overdensity shows a significant absorption feature at the wavelength of Lyα redshifted at z = 2.895 (λ = 4736 Å), with a rest frame equivalent width (EW) of 4 ± 1.4 Å. Stacking only background galaxies without intervening sources at z ∼ 2.9 along their line of sight, we find that this absorption feature has a rest frame EW of 10.8 ± 3.7 Å, with a detection S/N of ∼4. We verify that this measurement is not likely to be due to noise fluctuations. These EW values imply a high column density (N(HI) ∼ 3−20 × 10 19 cm −2 ), consistent with a scenario where such absorption is due to intervening cold streams of gas that are falling into the halo potential wells of the proto-cluster galaxies. Nevertheless, we cannot rule out the hypothesis that this absorption line is related to the diffuse gas within the overdensity.

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Section: Discussionmentioning

confidence: 99%

“…δ g ∼ 8.3 at z = 1.6 in Kurk et al 2009, δ g ∼ 16 at z ∼ 6 in Toshikawa et al 2012). We also refer the reader to Lemaux et al (2014), where we study a spectroscopic overdensity of δ g = 13.3 ± 6.6 found at z = 3.3 in the VVDS field using VUDS observations.…”

Section: The Overdensitymentioning

confidence: 99%

Discovery of a rich proto-cluster atz= 2.9 and associated diffuse cold gas in the VIMOS Ultra-Deep Survey (VUDS)

Cucciati

Zamorani

Lemaux

et al. 2014

A&A

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“…Some candidates without spectroscopic confirmation beyond z = 6 have also been found (Trenti et al 2012;Ishigaki et al 2016). Although the majority of protocluster members are young and star-forming galaxies, a red sequence, composed of bright and red galaxies, is found to appear in protoclusters around z ∼ 2-3 (e.g., Kurk et al 2004;Kodama et al 2007;Zirm et al 2008;Kubo et al 2013;Lemaux et al 2014). These color differences between protocluster and field galaxies is the result of different galaxy properties, such as age, dust, or metallicity.…”

Section: Introductionmentioning

confidence: 99%

A SYSTEMATIC SURVEY OF PROTOCLUSTERS AT z ∼ 3–6 IN THE CFHTLS DEEP FIELDS

Toshikawa

Kashikawa

Overzier

et al. 2016

ApJ

137

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We present the discovery of three protoclusters at z ∼ 3-4 with spectroscopic confirmation in the Canada-FranceHawaii Telescope Legacy Survey Deep Fields. In these fields, we investigate the large-scale projected sky distribution of z ∼ 3-6 Lyman-break galaxies and identify 21 protocluster candidates from regions that are overdense at more than 4σ overdensity significance. Based on cosmological simulations, it is expected that more than 76% of these candidates will evolve into a galaxy cluster of at least a halo mass of 1014 M e at z = 0. We perform follow-up spectroscopy for eight of the candidates using Subaru/FOCAS, Keck II/DEIMOS, and Gemini-N/GMOS. In total we target 462 dropout candidates and obtain 138 spectroscopic redshifts. We confirm three real protoclusters at z = 3-4 with more than five members spectroscopically identified and find one to be an incidental overdense region by mere chance alignment. The other four candidate regions at z ∼ 5-6 require more spectroscopic follow-up in order to be conclusive. A z = 3.67 protocluster, which has 11 spectroscopically confirmed members, shows a remarkable core-like structure composed of a central small region (<0.5 physical Mpc) and an outskirts region (∼1.0 physical Mpc). The Lyα equivalent widths of members of the protocluster are significantly smaller than those of field galaxies at the same redshift, while there is no difference in the UV luminosity distributions. These results imply that some environmental effects start operating as early as at z ∼ 4 along with the growth of the protocluster structure. This study provides an important benchmark for our analysis of protoclusters in the upcoming Subaru/HSC imaging survey and its spectroscopic follow-up with the Subaru/PFS that will detect thousands of protoclusters up to z ∼ 6.

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“…There are currently many techniques for finding highredshift protoclusters, including the serendipitous identification of redshift overdensities within spectroscopic surveys of Lyman Break Galaxies (LBGs), Lyα emitters (LAEs) or other magnitude-limited galaxy samples (Steidel et al 1998(Steidel et al , 2005Lemaux et al 2014;Chiang et al 2015;Harikane et al 2017), targeted searches for LAEs around radio galaxies (e.g., Venemans et al 2007), and Lyα forest tomography (Lee et al 2016). Based on these several methods, the number of known > z 2 protoclusters has grown dramatically over the past decade.…”

Section: Introductionmentioning

confidence: 99%

Understanding Large-scale Structure in the SSA22 Protocluster Region Using Cosmological Simulations^∗

Topping

Shapley

Steidel

et al. 2018

ApJ

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We investigate the nature and evolution of large-scale structure within the SSA22 protocluster region at z=3.09 using cosmological simulations. A redshift histogram constructed from current spectroscopic observations of the SSA22 protocluster reveals two separate peaks at z=3.065 (blue) and z=3.095 (red). Based on these data, we report updated overdensity and mass calculations for the SSA22 protocluster. We find d =  for the red, blue, and total peaks, respectively. We use the Small MultiDark Planck (SMDPL) simulation to identify comparably massivez 3 protoclusters, and uncover the underlying structure and ultimate fate of the SSA22 protocluster. For this analysis, we construct mock redshift histograms for each simulatedz 3 protocluster, quantitatively comparing them with the observed SSA22 data. We find that the observed double-peaked structure in the SSA22 redshift histogram corresponds not to a single coalescing cluster, but rather the proximity of a~- h M 10 15 1 protocluster and at least one > - h M 10 14 1 cluster progenitor. Such associations in the SMDPL simulation are easily understood within the framework of hierarchical clustering of dark matter halos. We finally find that the opportunity to observe such a phenomenon is incredibly rare, with an occurrence rate of

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VIMOS Ultra-Deep Survey (VUDS): Witnessing the assembly of a massive cluster atz~ 3.3

Cited by 63 publications

References 195 publications

Discovery of a rich proto-cluster atz= 2.9 and associated diffuse cold gas in the VIMOS Ultra-Deep Survey (VUDS)

Discovery of a rich proto-cluster atz= 2.9 and associated diffuse cold gas in the VIMOS Ultra-Deep Survey (VUDS)

A SYSTEMATIC SURVEY OF PROTOCLUSTERS AT z ∼ 3–6 IN THE CFHTLS DEEP FIELDS

Understanding Large-scale Structure in the SSA22 Protocluster Region Using Cosmological Simulations^∗

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VIMOS Ultra-Deep Survey (VUDS): Witnessing the assembly of a massive cluster atz~ 3.3

Cited by 63 publications

References 195 publications

Discovery of a rich proto-cluster atz= 2.9 and associated diffuse cold gas in the VIMOS Ultra-Deep Survey (VUDS)

Discovery of a rich proto-cluster atz= 2.9 and associated diffuse cold gas in the VIMOS Ultra-Deep Survey (VUDS)

A SYSTEMATIC SURVEY OF PROTOCLUSTERS AT z ∼ 3–6 IN THE CFHTLS DEEP FIELDS

Understanding Large-scale Structure in the SSA22 Protocluster Region Using Cosmological Simulations∗

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Understanding Large-scale Structure in the SSA22 Protocluster Region Using Cosmological Simulations^∗