MaxBCG: A Red‐Sequence Galaxy Cluster Finder

Koester, Benjamin P.; McKay, Timothy A.; Annis, J.; Wechsler, Risa H.; Evrard, A. E.; Rozo, Eduardo; Bleem, L. E.; Sheldon, E.; Johnston, David

doi:10.1086/512092

Cited by 348 publications

(530 citation statements)

References 104 publications

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“…A more modern and better calibrated richness measure is N 200 (Koester et al 2007b;Reyes et al 2008), the number of E/S0 ridgeline member galaxies within R 200 , fainter than the BCG and brighter than 0.4 L * . 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.…”

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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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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“…The first is to locate the cluster overdensity and determine the cluster centre, the second is to choose which galaxies are members of the cluster and the final step is to use the properties of this membership to estimate a cluster mass. Popular cluster finding techniques include using Red Sequence filtering techniques (e.g., Gladders & Yee 2000;Murphy et al 2012;Rykoff et al 2014) and brightest cluster galaxy (BCG) searches (e.g., Yang et al 2005a;Koester et al 2007). Friends-Of-Friends (FOF) group-finding algorithm based methods are also widely used (e.g., Berlind et al 2006;Li & Yee 2008;Jian et al 2014;Tempel et al 2014, see FOF optimisation study of Duarte & Mamon, 2014), along with methods based upon Voronoi tessellation (e.g., Marinoni et al 2002;Lopes et al 2004;van Breukelen & Clewley 2009;Soares-Santos et al 2011).…”

Section: Introductionmentioning

confidence: 99%

Galaxy Cluster Mass Reconstruction Project – II. Quantifying scatter and bias using contrasting mock catalogues

Old

Wojtak

Mamon

et al. 2015

Monthly Notices of the Royal Astronomical Society

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This article is the second in a series in which we perform an extensive comparison of various galaxy-based cluster mass estimation techniques that utilise the positions, velocities and colours of galaxies. Our aim is to quantify the scatter, systematic bias and completeness of cluster masses derived from a diverse set of 25 galaxy-based methods using two contrasting mock galaxy catalogues based on a sophisticated halo occupation model and a semi-analytic model. Analysing 968 clusters, we find a wide range in the RMS errors in log M 200c delivered by the different methods (0.18 to 1.08 dex, i.e., a factor of ∼1.5 to 12), with abundance matching and richness methods providing the best results, irrespective of the input model assumptions. In addition, certain methods produce a significant number of catastrophic cases where the mass is under-or over-estimated by a factor greater than 10. Given the steeply falling high-mass end of the cluster mass function, we recommend that richness or abundance matching-based methods are used in conjunction with these methods as a sanity check for studies selecting high mass clusters. We see a stronger correlation of the recovered to input number of galaxies for both catalogues in comparison with the group/cluster mass, however, this does not guarantee that the correct member galaxies are being selected. We do not observe significantly higher scatter for either mock galaxy catalogues. Our results have implications for cosmological analyses that utilise the masses, richnesses, or abundances of clusters, which have different uncertainties when different methods are used.

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“…At the same time, the advent of multi-band photometric data has led to dramatic improvements in optical cluster finding and an explosion of algorithms (e.g. Gladders & Yee 2005;Koester et al 2007;Wen & Han 2013;Hao et al 2010;Szabo et al 2011, and many others).…”

Section: Introductionmentioning

confidence: 99%

The X-CLASS−redMaPPer galaxy cluster comparison

Sadibekova

Pierre

Clerc

et al. 2014

A&A

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Context. This paper is the first in a series undertaking a comprehensive correlation analysis between optically selected and X-rayselected cluster catalogues. The rationale of the project is to develop a holistic picture of galaxy clusters utilising optical and X-raycluster-selected catalogues with well-understood selection functions. Aims. Unlike most of the X-ray/optical cluster correlations to date, the present paper focuses on the non-matching objects in either waveband. We investigate how the differences observed between the optical and X-ray catalogues may stem from (1) a shortcoming of the detection algorithms; (2) dispersion in the X-ray/optical scaling relations; or (3) substantial intrinsic differences between the cluster populations probed in the X-ray and optical bands. The aim is to inventory and elucidate these effects in order to account for selection biases in the further determination of X-ray/optical cluster scaling relations. Methods. We correlated the X-CLASS serendipitous cluster catalogue extracted from the XMM archive with the redMaPPer optical cluster catalogue derived from the Sloan Digital Sky Survey (DR8). We performed a detailed and, in large part, interactive analysis of the matching output from the correlation. The overlap between the two catalogues has been accurately determined and possible cluster positional errors were manually recovered. The final samples comprise 270 and 355 redMaPPer and X-CLASS clusters, respectively. X-ray cluster matching rates were analysed as a function of optical richness. In the second step, the redMaPPer clusters were correlated with the entire X-ray catalogue, containing point and uncharacterised sources (down to a few 10 −15 erg s −1 cm −2 in the [0.5−2] keV band). A stacking analysis was performed for the remaining undetected optical clusters. Results. We find that all rich (λ ≥ 80) clusters are detected in X-rays out to z = 0.6. Below this redshift, the richness threshold for X-ray detection steadily decreases with redshift. Likewise, all X-ray bright clusters are detected by redMaPPer. After correcting for obvious pipeline shortcomings (about 10% of the cases both in optical and X-ray), ∼50% of the redMaPPer (down to a richness of 20) are found to coincide with an X-CLASS cluster; when considering X-ray sources of any type, this fraction increases to ∼80%; for the remaining objects, the stacking analysis finds a weak signal within 0.5 Mpc around the cluster optical centres. The fraction of clusters totally dominated by AGN-type emission appears to be a few percent. Conversely, ∼40% of the X-CLASS clusters are identified with a redMaPPer (down to a richness of 20) − part of the non-matches being due to the X-CLASS sample extending further out than redMaPPer (z < 1.5 vs. z < 0.6), but extending the correlation down to a richness of 5 raises the matching rate to ∼65%. Conclusions. This state-of-the-art study involving two well-validated cluster catalogues has shown itself to be complex, and it points to a number of issues inherent to blind c...

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MaxBCG: A Red‐Sequence Galaxy Cluster Finder

Cited by 348 publications

References 104 publications

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

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

Galaxy Cluster Mass Reconstruction Project – II. Quantifying scatter and bias using contrasting mock catalogues

The X-CLASS−redMaPPer galaxy cluster comparison

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