Clusters of Galaxies in the First Half of the Universe from the IRAC Shallow Survey

By Peter Eisenhardt, M. Brodwin, R. Chary, R. Propris, Anthony H. Gonzalez, L. A. Moustakas, A. Stanford, Daniel Stern, E. L. Wright. 2008

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We have identified 335 galaxy cluster and group candidates, 106 of which are at z > 1, using a 4.5 μm-selected sample of objects from a 7.25 deg2 region in the Spitzer Infrared Array Camera (IRAC) Shallow Survey. Clusters were identified as three-dimensional overdensities using a wavelet algorithm, based on photometric redshift probability distributions derived from IRAC and NOAO Deep Wide-Field Survey data. We estimate only ~10% of the detections are spurious. To date 12 of the z > 1 candidates have been confirmed spectroscopically, at redshifts from 1.06 to 1.41. Velocity dispersions of ~750 km s−1 for two of these argue for total cluster masses well above 1014 M☉, as does the mass estimated from the rest-frame near-infrared stellar luminosity. Although not selected to contain a red sequence, some evidence for red sequences is present in the spectroscopically confirmed clusters, and brighter galaxies are systematically redder than the mean galaxy color in clusters at all redshifts. The mean I − [ 3.6] color for cluster galaxies up to z ∼ 1 is well matched by a passively evolving model in which stars are formed in a 0.1 Gyr burst starting at redshift zf = 3. At z > 1, a wider range of formation histories is needed, but higher formation redshifts (i.e., zf > 3) are favored for most clusters.

Subfields: Astronomy and Astrophysics, Instrumentation

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Citations in the corpus

The WISE AGN Catalog (2017, methodology): “…the AGN and Galaxy Evolution Survey (AGES; Kochanek et al. 2012), which obtained deep optical spectra of 23, 745 sources in the field, and are supplemented with deeper spectroscopy of ∼ 2, 000 sources obtained with various facilities, although primarily from Keck (e.g., Eisenhardt et al. 2008).”
Observational probes of cosmic acceleration (2012, methodology): “In the near future, such searches will rely on Spitzer data, as in the case of ISCS (Eisenhardt et al., 2008), SpARCS (Wilson et al.”
A WEAK LENSING STUDY OF X-RAY GROUPS IN THE COSMOS SURVEY: FORM AND EVOLUTION OF THE MASS–LUMINOSITY RELATION (2009, background): “Groups and clusters of galaxies, formed through the gravitational collapse of massive dark matter halos, are now readily identified up to redshift one and even beyond (e.g. Stanford et al. 2006; Eisenhardt et al. 2008).”
SPECTROSCOPIC CONFIRMATION OF TWO MASSIVE RED-SEQUENCE-SELECTED GALAXY CLUSTERS AT z ∼ 1.2 IN THE SpARCS-NORTH CLUSTER SURVEY (2008, methodology): “…thus far been confined to modest areas (ranging from 0.5 - 8.5 deg2) they have been extremely successful at detecting z > 1 clusters (e.g., Stanford et al. 2005; Brodwin et al. 2006; van Breuklen et al. 2007; Zatloukal et al. 2007; Krick et al. 2008; Eisenhardt et al. 2008; Muzzin et al. 2008).”
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THE CLUSTER LENSING AND SUPERNOVA SURVEY WITH HUBBLE: AN OVERVIEW (2011, background): “These observations include the detection of perhaps 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)…”
Cosmic chronometers: constraining the equation of state of dark energy. I: H(z) measurements (2009, unknown): “In the redshift range 0.5 z 1, fewer rich X-ray clusters are known, so we targeted (and confirmed) two of the richest Spitzer mid-infrared selected cluster candidates from the IRAC Shallow Cluster Survey [45].”
GALAXY CLUSTERS DISCOVERED VIA THE SUNYAEV–ZEL'DOVICH EFFECT IN THE 2500-SQUARE-DEGREE SPT-SZ SURVEY (2014, background): “Clusters identified in this manner typically contain of tens to thousands of galaxies (e.g., Abell 1958; Gladders & Yee 2000; Koester et al. 2007; Eisenhardt et al. 2008; Wen et al. 2012; Rykoff et al. 2014).”
THE SUPERNOVA DELAY TIME DISTRIBUTION IN GALAXY CLUSTERS AND IMPLICATIONS FOR TYPE-Ia PROGENITORS AND METAL ENRICHMENT (2010, background): “Optical spectroscopy and multiwavelength photometry of cluster galaxies has shown consistently that the bulk of their stars were formed within short episodes (∼ 100 Myr) at z ∼ 3 (e.g., Daddi et al. 2000; Stanford et al. 2005; Eisenhardt et al. 2008).”
MID-INFRARED SELECTION OF ACTIVE GALACTIC NUCLEI WITH THE WIDE-FIELD INFRARED SURVEY EXPLORER. I. CHARACTERIZING WISE-SELECTED ACTIVE GALACTIC NUCLEI IN COSMOS (2012, background): “This sequence, due to massive galaxies at z ∼> 1.2 (e.g., Stern et al. 2005; Eisenhardt et al. 2008; Papovich 2008), typically outnumbers the AGN sequence since even very shallow (< 90 sec) IRAC pointings easily reach well below the characteristic brightness of early-type galaxies out to z ∼ 2,…”
A SPITZER-SELECTED GALAXY CLUSTER AT z = 1.62 (2010, methodology): “This was motivated by other cluster–member selection methods using photometric–redshift–selected samples (Brunner & Lubin 2000; Halliday et al. 2004; Eisenhardt et al. 2008; Pelló et al. 2009).”
THE SPITZER DEEP, WIDE-FIELD SURVEY (2009, background): “Essentially, the negative K-correction of a passively evolving population formed at high redshift (z 3) produces a roughly constant apparent magnitude in the shorter-wavelength IRAC bands for 0.7 z 2 (see Figure 1 of Eisenhardt et al. 2008).”
The realm of the galaxy protoclusters (2016, background): “The IRAC Shallow Cluster Survey (ISCS; Eisenhardt et al., 2008) and its higher redshift extension, the IRAC Distant Cluster Survey (IDCS; Stanford et al., 2012), searched for redshift overdensities to identify a large sample of z > 1 cluster candidates of which many have since been confirmed,…”
THE HUBBLE SPACE TELESCOPE CLUSTER SUPERNOVA SURVEY. V. IMPROVING THE DARK-ENERGY CONSTRAINTS ABOVE z > 1 AND BUILDING AN EARLY-TYPE-HOSTED SUPERNOVA SAMPLE (2011, methodology): “A separate series of papers, ten to date, reports on cluster studies from the HST Cluster SN Survey: Brodwin et al. (2010); Eisenhardt et al. (2008); Jee et al. (2009); Hilton et al. (2007, 2009); Huang et al. (2009); Santos et al. (2009); Strazzullo et al. (2010); Rosati et al. (2009); and Jee et…”
Type-Ia Supernova Rates and the Progenitor Problem: A Review (2011, background): “…photometry of cluster galaxies has shown consistently that the bulk of their stars were formed within short episodes (∼ 100 Myr) at z ∼ 3 (e.g., Daddi et al. 2000; Saracco et al. 2003; Stanford et al. 2005; van Dokkum and van der Marel 2007; Jimenez et al. 2007; Eisenhardt et al. 2008).”
THE ERA OF STAR FORMATION IN GALAXY CLUSTERS (2013, background): “In particular, it offers a more physically motivated explanation for the apparent pure passive evolution seen in z < 1 cluster studies (e.g., Stanford et al. 1998; van Dokkum and van der Marel 2007; Muzzin et al. 2008).”
ROBUST OPTICAL RICHNESS ESTIMATION WITH REDUCED SCATTER (2011, background): “This feature allows for high-contrast detection of galaxy clusters with optical data, both locally and out to high redshift (e.g., Gladders & Yee 2000; Eisenhardt et al. 2008).”