A SPITZER-SELECTED GALAXY CLUSTER AT z = 1.62

By C. Papovich, Ivelina G. Momcheva, C. Willmer, K. Finkelstein, S. Finkelstein, K. Tran, M. Brodwin, J. Dunlop, D. Farrah, S. Khan and 19 more. 2010

210 citations recorded by the source corpus.

We report the discovery of a galaxy cluster at z = 1.62 located in the Spitzer Wide-Area Infrared Extragalactic survey XMM–LSS field. This structure was selected solely as an overdensity of galaxies with red Spitzer/Infrared Array Camera colors, satisfying ([3.6] − [4.5])AB> − 0.1 mag. Photometric redshifts derived from the Subaru XMM Deep Survey (BViz bands), the UKIRT Infrared Deep Survey–Ultra-Deep Survey (UKIDSS–UDS, JK bands), and from the Spitzer Public UDS survey (3.6–8.0 μm) show that this cluster corresponds to a surface density of galaxies at z ≈ 1.6 that is >20σ above the mean at this redshift. We obtained optical spectroscopic observations of galaxies in the cluster region using IMACS on the Magellan telescope. We measured redshifts for seven galaxies in the range z = 1.62–1.63 within 2.8 arcmin (<1.4 Mpc) of the astrometric center of the cluster. A posteriori analysis of the XMM data in this field reveal a weak (4σ) detection in the [0.5–2 keV] band compatible with the expected thermal emission from such a cluster. The color–magnitude diagram of the galaxies in this cluster shows a prominent red sequence, dominated by a population of red galaxies with (z − J)>1.7 mag. The photometric-redshift probability distributions for the red galaxies are strongly peaked at z = 1.62, coincident with the spectroscopically confirmed galaxies. The rest-frame (U − B) color and scatter of galaxies on the red sequence are consistent with a mean luminosity-weighted age of 1.2 ± 0.1 Gyr, yielding a formation redshift , and corresponding to the last significant star formation period in these galaxies.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/05d378f30fafc6ad23515fe982a7eb22d795dd5c

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In Astronomy and Astrophysics

1. P. V. van Dokkum
2. M. Franx
3. P. Hopkins
4. Christopher J. Conselice
5. L. Hernquist
6. C. Conroy
7. I. Labbé
8. Richard S. Ellis

In Instrumentation

1. P. V. van Dokkum
2. M. Franx
3. Christopher J. Conselice
4. I. Labbé
5. C. Conroy
6. Richard S. Ellis
7. R. Bouwens
8. P. Hopkins

Citations in the corpus

• ANCIENT LIGHT FROM YOUNG COSMIC CITIES: PHYSICAL AND OBSERVATIONAL SIGNATURES OF GALAXY PROTO-CLUSTERS (2013, background): “CEP 20921-400, São Cristóvão, Rio de Janeiro-RJ, Brazil quence, and ICM in place, suggesting formation redshifts for most of their stellar contents much beyond 2 (Blakeslee et al. 2003; Mei et al. 2006; Andreon 2008; Papovich et al. 2010; Rettura et al. 2010, 2011; Fassbender et al. 2011b).”
• The XMM Cluster Survey:Optical analysis methodology and the first data release (2011, methodology): “…homogeneous between clusters at the same redshift and has been detected to z > 1 (Lidman et al. 2008; Mei et al. 2009; Hilton et al. 2009; Papovich et al. 2010), meaning it can be used as a tool for cluster detection out to high redshifts (e.g. Gladders & Yee 2000; Gladders & Yee 2005;…”
• The DEIMOS 10K Spectroscopic Survey Catalog of the COSMOS Field (2018, background): “At z>1.4 there are about 5 known clusters, of which 2 have masses above M1014 (Papovich et al. 2010; Mantz et al. 2016).”
• A mature cluster with X-ray emission at z = 2.07 (2010, background): “The density of this structure is thus similar to that reported for the recently discovered galaxy cluster atz = 1.62 (Papovich et al. 2010).”
• The VISTA deep extragalactic observations (VIDEO) survey (2012, background): “Once found, such galaxy clusters can be studied in great detail in terms of their galaxy populations (e.g. Papovich et al. 2010; Tran et al. 2010), and AGN content (e.g. van Breukelen et al. 2009; Martini, Sivakoff & Mulchaey 2009), to trace how galaxies form and evolve in closed and dense…”
• IMACS: The Inamori-Magellan Areal Camera and Spectrograph on Magellan-Baade (2011, methodology): “In 2010 IMACS was used to obtain spectra that confirmed the photometric redshift of the most distant cluster of galaxies found to date, z ¼ 1:62 (Papovich et al. 2010).”
• The rising star formation histories of distant galaxies and implications for gas accretion with time (2010, background): “3 galaxies with suppressed or absent star-formation (e.g., Kriek et al. 2006; van Dokkum et al. 2009; Papovich et al. 2010), although such systems are much rarer or absent at z & 3.5 (Brammer & van Dokkum 2007; Stutz et al. 2008).”
• REVERSAL OF FORTUNE: CONFIRMATION OF AN INCREASING STAR FORMATION–DENSITY RELATION IN A CLUSTER AT z = 1.62 (2010, background): “3-05101, a Spitzer-selected galaxy cluster at z = 1.62 (Papovich et al. 2010, hereafter Pap10).”
• METALLICITY-DEPENDENT QUENCHING OF STAR FORMATION AT HIGH REDSHIFT IN SMALL GALAXIES (2011, background): “This is consistent with observational findings by Papovich et al. (2010).”
• The realm of the galaxy protoclusters (2016, background): “One of the candidates was spectroscopically confirmed to be at z = 1.62 (Papovich et al., 2010), while another z = 2.00 cluster2 having a strong red sequence of early-type galaxies was also identified using this tech- 2 We should note that several of these objects would be classified as…”
• A GMBCG GALAXY CLUSTER CATALOG OF 55,424 RICH CLUSTERS FROM SDSS DR7 (2010, background): “It has been shown that red-sequence galaxies exist in clusters of varied richness and extend to redshift z ∼ 1.6 (Bower et al. 1992; Smail et al. 1998; Barrientos 1999; Mullis et al. 2005; Eisenhardt et al. 2005; Papovich et al. 2010).”
• THE CLUSTER LENSING AND SUPERNOVA SURVEY WITH HUBBLE: AN OVERVIEW (2011, background): “…unexpectedly massive galaxy clusters at z > 1 (Stanford et al. 2006; Eisenhardt et al. 2008; Jee et al. 2009; Huang et al. 2009; Rosati et al. 2009; Papovich et al. 2010; Schwope et al. 2010; Gobat et al. 2011; Jee et al. 2011; Foley et al. 2011) and the finding that some clusters at intermediate…”
• CANDELS MULTIWAVELENGTH CATALOGS: SOURCE IDENTIFICATION AND PHOTOMETRY IN THE CANDELS UKIDSS ULTRA-DEEP SURVEY FIELD (2013, background): “, QSOs (Smail et al. 2008), Lyα emit- 7 http://irsa.ipac.caltech.edu/data/SPITZER/SpUDS/ 8 http://www.cfa.harvard.edu/SEDS 4 ters (Ouchi et al. 2008), galaxy cluster members (Geach et al. 2007; van Breukelen et al. 2007; Papovich et al. 2010; Tanaka et al. 2010; Finoguenov et al. 2010).”
• 3D-HST WFC3-SELECTED PHOTOMETRIC CATALOGS IN THE FIVE CANDELS/3D-HST FIELDS: PHOTOMETRY, PHOTOMETRIC REDSHIFTS, AND STELLAR MASSES (2014, methodology): “The F140W coverage has a hole because the final pointing, UDS-18, was moved to the western-most edge of the CANDELS coverage to carry out G141 observations of the IRC0812A z = 1.62 cluster (Papovich et al. 2010).”