Galaxy Clusters Selected With the Sunyaev-Zel'dovich Effect From 2008 South Pole Telescope Observations

Vanderlinde, K.; Crawford, T. M.; Haan, T. de; Dudley, J. P.; Shaw, L.; Ade, Peter A. R.; Aird, K. A.; Benson, B. A.; Bleem, L. E.; Brodwin, M.; Carlstrom, J. E.; Chang, C. L.; Crites, A. T.; Desai, S.; Dobbs, M.; Foley, R. J.; George, E. M.; Gladders, M. D.; Hall, Nicholas R.; Halverson, N. W.; High, F. W.; Holder, G. P.; Holzapfel, W. L.; Hrubes, J. D.; Joy, M.; Keisler, R.; Knox, L.; Lee, A. T.; Leitch, E. M.; Loehr, A.; Lueker, M.; Marrone, Daniel P.; McMahon, Jeff; Mehl, J.; Meyer, S. S.; Mohr, J. J.; Montroy, T. E.; Ngeow, Chow-Choong; Padin, S.; Plagge, T.; Pryke, C.; Reichardt, Christian; Rest, A.; Ruel, J.; Ruhl, J. E.; Schaffer, K. K.; Shirokoff, E.; Song, J.; Spieler, H.; Stalder, B.; Staniszewski, Z.; Stark, A. A.; Stubbs, C. W.; Engelen, A. van; Vieira, J. D.; Williamson, A. R.; Yang, Yujin; Zahn, O.; Zenteno, A.

doi:10.1088/0004-637x/722/2/1180

Cited by 321 publications

(413 citation statements)

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“…Unfortunately, achieving sufficient sensitivity to detect low mass clusters in SZ is technologically very challenging. For instance, the current SPT, ACT, and Planck surveys are expected to be complete at all redshifts above mass thresholds of 7 × 10 14 M ⊙ , 10 15 M ⊙ , and 2 × 10 15 M ⊙ respectively (Vanderlinde et al, 2010;Marriage et al, 2011;Planck Collaboration et al, 2011a); while these limits will go down, they will not reach thresholds comparable to those of X-ray or optical cluster selection. Consequently, while these experiments are currently the best avenue to probe the z ≈ 1 massive cluster population, on a 3 − 5 year time scale the focus of cluster detection is likely to shift towards optical and X-ray.…”

Section: Cluster Findingmentioning

confidence: 98%

“…The first three successful cluster SZ surveys -using the South Pole Telescope (SPT), the Atacama Cosmology Telescope (ACT), and the Planck satellite -are all currently ongoing. All three projects have released SZ-selected cluster samples (Vanderlinde et al, 2010;Marriage et al, 2011;Planck Collaboration et al, 2011a;Williamson et al, 2011;Reichardt et al, 2013). These samples tend to be of very massive clusters (see Figure 27) and, in the case of ACT and SPT, extend to z ≈ 2, with the upper limit set by the lack of massive galaxy clusters above this redshift.…”

Section: The Current State Of Playmentioning

confidence: 99%

“…However, recent work that uses stacked weak lensing analysis for mass calibration (Johnston et al, 2007;Mandelbaum et al, 2008;Sheldon et al, 2009) has allowed optical samples to achieve the same level of precision as X-ray samples , with comparable levels of systematic error. Constraints from SZ selected samples are emerging (Vanderlinde et al, 2010;Sehgal et al, 2011;Reichardt et al, 2013), and while they are currently weak because of the relatively large uncertainty in the SZ-mass scaling relation, the extensive follow-up campaigns that are currently underway will reduce this scaling uncertainty and bring these constraints to a level comparable to those from optical and X-ray cluster catalogs (e.g. High et al, 2012;Hoekstra et al, 2012;Planck Collaboration, 2012;Rozo et al, 2012d).…”

Section: The Current State Of Playmentioning

confidence: 99%

“…Vanderlinde et al, 2010;Sehgal et al, 2011). The main difficulty that simulation methods face is our incomplete understanding of baryonic physics, particularly galaxy formation feedback processes.…”

Section: Calibrating the Observable-mass Relationmentioning

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: Cluster Findingmentioning

confidence: 98%

Section: The Current State Of Playmentioning

confidence: 99%

Section: The Current State Of Playmentioning

confidence: 99%

Section: Calibrating the Observable-mass Relationmentioning

confidence: 99%

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Observational probes of cosmic acceleration

et al. 2013

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“…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

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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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From Nearby Galaxy Clusters to Cosmological Distances

Grijs

2011

An Introduction to Distance Measurement in Astronomy

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Galaxy Clusters Selected With the Sunyaev-Zel'dovich Effect From 2008 South Pole Telescope Observations

Cited by 321 publications

References 72 publications

Observational probes of cosmic acceleration

Observational probes of cosmic acceleration

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

From Nearby Galaxy Clusters to Cosmological Distances

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