X-RAY EMISSION FROM TWO INFRARED-SELECTED GALAXY CLUSTERS AT<i>z</i>&gt; 1.4 IN THE IRAC SHALLOW CLUSTER SURVEY

Brodwin, M.; Stern, Daniel; Vikhlinin, A.; Stanford, S. A.; Gonzalez, Anthony H.; Eisenhardt, Peter; Ashby, M. L. N.; Bautz, M. W.; Dey, Arjun; Forman, W.; Gettings, D.; Hickox, R. C.; Jannuzi, Buell T.; Jones, C.; Mancone, Conor L.; Miller, Eric D.; Moustakas, Leonidas A.; Ruel, J.; Snyder, Greg; Zeimann, Gregory R.

doi:10.1088/0004-637x/732/1/33

Cited by 70 publications

(87 citation statements)

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“…Clustering (Brodwin et al 2007), extended X-ray emission (Brodwin et al 2011), weak-lensing (Jee et al 2011), and stellar masses (Eisenhardt et al 2008) support the view that these are massive (M 10 14 M ) clusters and are the precursors to present-day massive (M ∼ 10 15 M ) clusters. These observations thus provide a valuable window into the evolution of galaxies within the most massive halos in the universe by revealing the time during which most of their stellar mass formed and assembled from smaller pieces.…”

Section: Discussionmentioning

confidence: 55%

“…There are 335 ISCS cluster and group candidates, 106 of which are at z > 1. Over 20 clusters at z > 1 have now been spectroscopically confirmed with W. M. Keck Telescope and/ or HST spectroscopy (Stanford et al 2005(Stanford et al , 2012Elston et al 2006;Brodwin et al 2006Brodwin et al , 2011Eisenhardt et al 2008;G. Zeimann et al 2012, in preparation;M.…”

Section: Cluster Catalogmentioning

confidence: 95%

“…a Color width in magnitudes used to define the RSG selection region; see Section 3.2. b Spectroscopy for parts of this sample were described by Stanford et al (2005), Elston et al (2006), Brodwin et al (2006Brodwin et al ( , 2011, and Eisenhardt et al (2008). Updated membership identification, including those confirmed with the HST WFC3 grism, will be described by G. Zeimann et al (2012, in preparation) and M. Brodwin et al (2012, in preparation).…”

Section: Notesmentioning

confidence: 99%

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Assembly of the Red Sequence in Infrared-Selected Galaxy Clusters From the Irac Shallow Cluster Survey

Snyder

Brodwin

Mancone

et al. 2012

ApJ

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We present results for the assembly and star formation histories (SFHs) of massive (∼L * ) red sequence galaxies (RSGs) in 11 spectroscopically confirmed, infrared-selected galaxy clusters at 1.0 < z < 1.5, the precursors to present-day massive clusters with M ∼ 10 15 M . Using rest-frame optical photometry, we investigate evolution in the color and scatter of the RSG population, comparing with models of possible SFHs. In contrast to studies of central cluster galaxies at lower redshift (z < 1), these data are clearly inconsistent with the continued evolution of stars formed and assembled primarily at a single, much earlier time. Specifically, we find that the colors of massive cluster galaxies at z ≈ 1.5 imply that the bulk of star formation occurred at z ∼ 3, whereas by z ≈ 1 their colors imply formation at z ∼ 2; therefore these galaxies exhibit approximately the same luminosity-weighted stellar age at 1 < z < 1.5. This likely reflects star formation that occurs over an extended period, the effects of significant progenitor bias, or both. Our results generally indicate that massive cluster galaxy populations began forming a significant mass of stars at z 4, contained some red spheroids by z ≈ 1.5, and were actively assembling much of their final mass during 1 < z < 2 in the form of younger stars. Qualitatively, the slopes of the cluster color-magnitude relations are consistent with no significant evolution relative to local clusters.

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Section: Discussionmentioning

confidence: 55%

Section: Cluster Catalogmentioning

confidence: 95%

Section: Notesmentioning

confidence: 99%

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Assembly of the Red Sequence in Infrared-Selected Galaxy Clusters From the Irac Shallow Cluster Survey

Snyder

Brodwin

Mancone

et al. 2012

ApJ

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“…Similar X-ray flux estimations were derived in galaxy proto-clusters at comparable high redshifts Papovich et al 2010;Gobat et al 2011), although, as for the MRC 0156-252 field, both these proto-clusters also host a number of X-ray AGN that made it challenging to estimate a reliable X-ray flux for the ICM. These estimations are still however ∼5−10 times fainter than the X-ray emission in the highest redshift confirmed X-ray selected galaxy clusters (e.g., z ∼ 1.6; Fassbender et al 2011) or mid-infrared selected galaxy clusters (z = 1.75; Stanford et al 2012) and (z ∼ 1.4−1.5; Brodwin et al 2011) which are most probably more advanced collapsed galaxy structures than the present proto-cluster.…”

Section: X-ray Extended Emission From the Icm?mentioning

confidence: 55%

A large-scale galaxy structure atz = 2.02 associated with the radio galaxy MRC 0156-252

Galametz

Stern

Pentericci

et al. 2013

A&A

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We present the spectroscopic confirmation of a structure of galaxies surrounding the radio galaxy MRC 0156-252 at z = 2.02. The structure was initially discovered as an overdensity of both near-infrared selected z > 1.6 and mid-infrared selected z > 1.2 galaxy candidates. We used the VLT/FORS2 multi-object spectrograph to target ∼80 high-redshift galaxy candidates, and obtain robust spectroscopic redshifts for more than half the targets. The majority of the confirmed sources are star-forming galaxies at z > 1.5. In addition to the radio galaxy, two of its close-by companions (<6 ) also show AGN signatures. Ten sources, including the radio galaxy, lie within | z − 2.020 | <0.015 (i.e., velocity offsets <1500 km s −1 ) and within projected 2 Mpc comoving of the radio galaxy. Additional evidence suggests not only that the galaxy structure associated with MRC 0156-252 is a forming galaxy cluster but also that this structure is most probably embedded in a larger-scale structure.

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“…Both surveys have discovered and spectroscopically confirmed candidate galaxy clusters out to redshift z 1.5 (e.g., Stanford et al, 2005;Brodwin et al, 2006;Eisenhardt et al, 2008;Muzzin et al, 2009;Wilson et al, 2009;Demarco et al, 2010), with some recent detections reaching z 2 Zeimann et al, 2012). Additionally, some of these systems have also been detected in X-rays and/or SZ (Brodwin et al, 2011;Andreon and Moretti, 2011;Brodwin et al, 2012). These early results are encouraging and suggest that IR detection of high redshift clusters can play an important role in the future of cluster cosmology.…”

Section: The Current State Of Playmentioning

confidence: 84%

Observational probes of cosmic acceleration

et al. 2013

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The accelerating expansion of the universe is the most surprising cosmological discovery in many decades, implying that the universe is dominated by some form of "dark energy" with exotic physical properties, or that Einstein's theory of gravity breaks down on cosmological scales. The profound implications of cosmic acceleration have inspired ambitious efforts to understand its origin, with experiments that aim to measure the history of expansion and growth of structure with percent-level precision or higher. We review in detail the four most well established methods for making such measurements: Type Ia supernovae, baryon acoustic oscillations (BAO), weak gravitational lensing, and the abundance of galaxy clusters. We pay particular attention to the systematic uncertainties in these techniques and to strategies for controlling them at the level needed to exploit "Stage IV" dark energy facilities such as BigBOSS, LSST, Euclid, and WFIRST. We briefly review a number of other approaches including redshift-space distortions, the Alcock-Paczynski effect, and direct measurements of the Hubble constant H 0 . We present extensive forecasts for constraints on the dark energy equation of state and parameterized deviations from General Relativity, achievable with Stage III and Stage IV experimental programs that incorporate supernovae, BAO, weak lensing, and cosmic microwave background data. We also show the level of precision required for clusters or other methods to provide constraints competitive with those of these fiducial programs. We emphasize the value of a balanced program that employs several of the most powerful methods in combination, both to cross-check systematic uncertainties and to take advantage of complementary information. Surveys to probe cosmic acceleration produce data sets that support a wide range of scientific investigations, and they continue the longstanding astronomical tradition of mapping the universe in ever greater detail over ever larger scales.

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X-RAY EMISSION FROM TWO INFRARED-SELECTED GALAXY CLUSTERS ATz> 1.4 IN THE IRAC SHALLOW CLUSTER SURVEY

Cited by 70 publications

References 56 publications

Assembly of the Red Sequence in Infrared-Selected Galaxy Clusters From the Irac Shallow Cluster Survey

Assembly of the Red Sequence in Infrared-Selected Galaxy Clusters From the Irac Shallow Cluster Survey

A large-scale galaxy structure atz = 2.02 associated with the radio galaxy MRC 0156-252

Observational probes of cosmic acceleration

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