A MaxBCG Catalog of 13,823 Galaxy Clusters from the Sloan Digital Sky Survey

Koester, Benjamin P.; McKay, Timothy A.; Annis, J.; Wechsler, Risa H.; Evrard, A. E.; Bleem, L. E.; Becker, M. R.; Johnston, David; Sheldon, E.; Nichol, R. C.; Miller, Christopher J.; Scranton, Ryan; Bahcall, Neta A.; Barentine, John C.; Brewington, H.; Brinkmann, Jonathan; Harvanek, Michael; Kleinman, S. J.; Krzesiński, Jurek; Long, Daniel C.; Nitta, A.; Schneider, Donald P.; Sneddin, S.; Voges, W.; York, Donald G.

doi:10.1086/509599

Cited by 516 publications

(653 citation statements)

References 111 publications

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“…Milkeraitis et al, 2010;Adami et al, 2010), the SDSS has led to the publication of several moderately deep (z 0.5) and wide catalogs, which can contain upwards of 50,000 clusters (e.g. Koester et al, 2007;Wen et al, 2009;Hao et al, 2010;Szabo et al, 2011). Extensions that reach out to z ≈ 1 over 1000 deg 2 or more from current or near future photometric surveys -such as RCS-2, DES, Pan-STARRS, and HSC -will expand samples to the hundreds of thousands.…”

Section: The Current State Of Playmentioning

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%

“…Current cluster photometric redshift estimates have a dispersion of ≈ 0.01 (e.g. Koester et al, 2007), so controlling the scatter at the 0.03 level is not particularly problematic. The bias on the mean is more challenging, but current catalogs do achieve close to the necessary accuracy.…”

Section: Redshift Uncertaintiesmentioning

confidence: 99%

Observational probes of cosmic acceleration

et al. 2013

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“…This richness definition has been used for the MaxBCG catalog of Koester et al (2007a) of optically selected groups and clusters from the Sloan Digital Sky Survey (SDSS) in the redshift range 0.1 < z < 0.3. We follow Reyes et al (2008) for a self-consistent procedure to determine N 200 , which has been used and calibrated with a different definition of R 200 , evaluated relative to the mean density ρ mean of the Universe.…”

Section: Richness Measuresmentioning

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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“…The observational efficiency of this approach has led to it being used extensively in cluster detection (Gladders & Yee 2005;Wilson et al 2006) and adopted in several group and cluster finding algorithms (e.g. Koester et al 2007;Murphy, Geach & Bower 2012;Rykoff et al 2014). As discussed in Gladders & Yee, optical and infrared imaging of local and z > 1 galaxy clusters indicates the universal presence of an RS (e.g.…”

Section: Introductionmentioning

confidence: 99%

“…Baldry et al 2004;Bell et al 2004;Brinchmann et al 2004), with many studies supporting a high formation redshift of the stellar population of z f 2 (e.g. Ellis et al 1997;Smail et al 1998;Stanford et al 1998;Ponman, Cannon & Navarro 1999;López-Cruz, Barkhouse & Yee 2004;Gladders & Yee 2005;Miller et al 2005;Voit 2005;Mei et al 2006aMei et al ,b, 2009Mei et al , 2012Koester et al 2007;Gilbank et al 2008Gilbank et al , 2011Lidman et al 2008;Wilson et al 2009;Lin et al 2012). There is, however, some observational evidence for ongoing star formation in clusters at z 1, (e.g.…”

Section: Introductionmentioning

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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A MaxBCG Catalog of 13,823 Galaxy Clusters from the Sloan Digital Sky Survey

Cited by 516 publications

References 111 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

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

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