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

Eisenhardt, Peter; Brodwin, M.; Gonzalez, Anthony H.; Stanford, Adam; Stern, Daniel; Barmby, P.; Brown, M. J. I.; Dawson, Kyle; Dey, Arjun; Doi, Mamoru; Galametz, A.; Jannuzi, Buell T.; Kochanek, C. S.; Meyers, J.; Morokuma, Tomoki; Moustakas, Leonidas A.

doi:10.1086/590105

Cited by 265 publications

(394 citation statements)

References 85 publications

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“…Today, there are two independent efforts aiming to detect galaxy clusters using IR data: the IRAC Shallow Cluster Survey (ISCS; Eisenhardt et al, 2008) and the Spitzer Adaptation of the Red-Sequence Cluster Survey (SpARCS; Wilson et al, 2006). 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).…”

Section: The Current State Of Playmentioning

confidence: 99%

“…However, as discussed in §6.3.2, space-based near-IR imaging is highly desirable for extending (rest-frame) optical cluster catalogs to z ≈ 2. 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, 2006), and the recently approved 100 deg 2 Spitzer-SPT Deep Field. Additional IR data is or will soon be available from surveys like VHS, UKIDSS, and WISE, which may allow for high redshift cluster finding (Gettings et al, 2012).…”

Section: Space Vs Groundmentioning

confidence: 99%

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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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Section: The Current State Of Playmentioning

confidence: 99%

Section: Space Vs Groundmentioning

confidence: 99%

Observational probes of cosmic acceleration

et al. 2013

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“…(v) Snyder et al (2012): Snyder et al, present Hubble Space Telescope follow up observations of clusters selected from the Spitzer/IRAC Shallow Cluster Survey (ISCS; Eisenhardt et al 2008). They provide photometry for these clusters in the H 160 band and one of the I 814 , i 775 or z 850 bands.…”

Section: O B S E Rvat I O Na L Data S E T Smentioning

confidence: 99%

The abundance and colours of galaxies in high-redshift clusters in the cold dark matter cosmology

Merson¹,

Baugh²,

González-Pérez³

et al. 2015

Mon. Not. R. Astron. Soc.

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High redshift galaxy clusters allow us to examine galaxy formation in extreme environments.Here we compile data for 15 z > 1 galaxy clusters to test the predictions from a state-of-theart semi-analytical model of galaxy formation. The model gives a good match to the slope and zero-point of the cluster red sequence. The model is able to match the cluster galaxy luminosity function at faint and bright magnitudes, but under-estimates the number of galaxies around the break in the cluster luminosity function. We find that simply assuming a weaker dust attenuation improves the model predictions for the cluster galaxy luminosity function, but worsens the predictions for the red sequence at bright magnitudes. Examination of the properties of the bright cluster galaxies suggests that the default dust attenuation is large due to these galaxies having large reservoirs of cold gas as well as small radii. We find that matching the luminosity function and colours of high redshift cluster galaxies, whilst remaining consistent with local observations, poses a challenge for galaxy formation models.

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“…Stanford et al 2005;Eisenhardt et al 2008;Wilson et al 2009;Muzzin et al 2009). While at local redshifts dynamical mass estimators can provide robust measurements for relaxed clusters even for rather small spectroscopic samples (e.g.…”

Section: Velocity Dispersionmentioning

confidence: 99%

“…van Breukelen et al 2006), and the mid-infrared (MIR) with Spitzer (e.g. Stanford et al 2005;Eisenhardt et al 2008;Wilson et al 2009;Muzzin et al 2009;Demarco et al 2010). The first detections of galaxy clusters based on the SunyaevZeldovich effect (SZE) (Staniszewski et al 2009;Vanderlinde et al 2010) have opened another promising window for the selection and study of massive distant systems.…”

Section: Introductionmentioning

confidence: 99%

A pan-chromatic view of the galaxy cluster XMMU J1230.3+1339 atz= 0.975

Fassbender

Böhringer

Santos

et al. 2011

A&A

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Context. Observations of the formation and evolution of massive galaxy clusters and their matter components provide crucial constraints on cosmic structure formation, the thermal history of the intracluster medium (ICM), galaxy evolution, transformation processes, and gravitational and hydrodynamic interaction physics of the subcomponents. Aims. We characterize the global multi-wavelength properties of the X-ray selected galaxy cluster XMMU J1230.3+1339 at z = 0.975, a new system discovered within the XMM-Newton Distant Cluster Project (XDCP). We measure and compare various widely used mass proxies and identify multiple cluster-associated components from the inner core region out to the large-scale structure environment.Methods. We present a comprehensive galaxy cluster study based on a joint analysis of X-ray data, optical imaging and spectroscopy observations, weak lensing results, and radio properties for achieving a detailed multi-component view on a system at z ∼ 1. Results. We find an optically very rich and massive system with M 200 (4.2 ± 0.8) × 10 14 M , T X,2500 5.3 +0.7 −0.6 keV, and L bol X,500 (6.5 ± 0.7) × 10 44 erg s −1 . We have identified a central fly-through group close to core passage and find marginally extended 1.4 GHz radio emission possibly associated with the turbulent wake region of the merging event. On the cluster outskirts we see evidence for an on-axis infalling group with a second brightest cluster galaxy (BCG) and indications for an additional off-axis group accretion event. We trace two galaxy filaments beyond the nominal cluster radius and provide a tentative reconstruction of the 3D-accretion geometry of the system. Conclusions. In terms of total mass, ICM structure, optical richness, and the presence of two dominant BCG-type galaxies, the newly confirmed cluster XMMU J1230.3+1339 is likely the progenitor of a system very similar to the local Coma cluster, differing by 7.6 Gyr of structure evolution. This new system is an ideally suited astrophysical model laboratory for in-depth follow-up studies on the aggregation of baryons in the cold and hot phases.

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

Cited by 265 publications

References 85 publications

Observational probes of cosmic acceleration

Observational probes of cosmic acceleration

The abundance and colours of galaxies in high-redshift clusters in the cold dark matter cosmology

A pan-chromatic view of the galaxy cluster XMMU J1230.3+1339 atz= 0.975

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