Projection, Spatial Correlations, and Anisotropies in a Large and Complete Sample of Abell Clusters

Miller, Christopher J.; Batuski, D. J.; Slinglend, K.; Hill, John M.

doi:10.1086/307748

Cited by 30 publications

(62 citation statements)

References 61 publications

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“…Comparing the r 0 value obtained with those found using other low‐redshift cluster samples shows good agreement, e.g. r 0 = 26.0 ± 4.5 Mpc h −1 (Borgani, Plionis & Kolokotronis 1999), 19.4 ≤ r 0 ≤ 23.3 Mpc h −1 (Miller et al 1999), 18.8 ± 0.9 Mpc h −1 (Collins et al 2000). See Nichol (2001) for a good review of r 0 values for various cluster samples.…”

Section: Correlation Functionsupporting

confidence: 56%

Friends-of-friends groups and clusters in the 2SLAQ catalogue

Farrens

Abdalla

Cypriano

et al. 2011

Monthly Notices of the Royal Astronomical Society

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We present a catalogue of galaxy groups and clusters selected using a friends‐of‐friends (FoF) algorithm with a dynamic linking length from the 2dF‐SDSS LRG and QSO (2SLAQ) luminous red galaxy survey. The linking parameters for the code are chosen through an analysis of simulated 2SLAQ haloes. The resulting catalogue includes 313 clusters containing 1152 galaxies. The galaxy groups and clusters have an average velocity dispersion of km s−1 and an average size of Mpc h−1. Galaxies from regions of 1 deg2 and centred on the galaxy clusters were downloaded from the Sloan Digital Sky Survey Data Release 6. Investigating the photometric redshifts and cluster red sequence of these galaxies shows that the galaxy clusters detected with the FoF algorithm are reliable out to z∼ 0.6. We estimate masses for the clusters using their velocity dispersions. These mass estimates are shown to be consistent with 2SLAQ mock halo masses. Further analysis of the simulation haloes shows that clipping out low‐richness groups with large radii improves the purity of catalogue from 52 to 88 per cent, while retaining a completeness of 94 per cent. Finally, we test the two‐point correlation function of our cluster catalogue. We find a best‐fitting power‐law model, ξ(r) = (r/r0)γ, with parameters r0= 24 ± 4 Mpc h−1 and γ=−2.1 ± 0.2, which are in agreement with other low‐redshift cluster samples and consistent with a Λ cold dark matter universe.

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Section: Correlation Functionsupporting

confidence: 56%

Friends-of-friends groups and clusters in the 2SLAQ catalogue

Farrens

Abdalla

Cypriano

et al. 2011

Monthly Notices of the Royal Astronomical Society

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“…Historically, cluster richness has been described using the Abell richness class (ARC), first defined by Abell (1958). Several studies have shown that the Abell richness parameter is not a welldefined quantity and is subjected to numerous observational biases, including projection effects (e.g., Lucey 1983;van Haarlem et al 1997;Miller et al 1999). For our cluster sample, we have elected to use the parameter B gc (Yee & López-Cruz 1999;Yee & Ellingson 2003) to characterize optical cluster richness.…”

Section: Optical Cluster Richnessmentioning

confidence: 99%

ChaMP Serendipitous Galaxy Cluster Survey

Barkhouse

Green

Vikhlinin

et al. 2006

ApJ

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We present a survey of serendipitous extended X-ray sources and optical cluster candidates from the Chandra Multiwavelength Project (ChaMP). Our main goal is to make an unbiased comparison of X-ray and optical cluster detection methods. In 130 archival Chandra pointings covering 13 deg 2 , we use a wavelet decomposition technique to detect 55 extended sources, of which 6 are nearby single galaxies. Our X-ray cluster catalog reaches a typical flux limit of about $10 À14 ergs cm À2 s À1, with a median cluster core radius of 21 00 . For 56 of the 130 X-ray fields, we use the ChaMP's deep NOAO 4 m MOSAIC g 0 , r 0 , and i 0 imaging to independently detect cluster candidates using a Voronoi tessellation and percolation (VTP) method. Red-sequence filtering decreases the galaxy fore-and background contamination and provides photometric redshifts to z $ 0:7. From the overlapping 6.1 deg 2 X-ray/optical imaging, we find 115 optical clusters (of which 11% are in the X-ray catalog) and 28 X-ray clusters (of which 46% are in the optical VTP catalog). The median redshift of the 13 X-ray/optical clusters is 0.41, and their median X-ray luminosity (0.5-2 keV ) is L X ¼ 2:65 AE 0:19 ð Þ; 10 43 ergs s À1. The clusters in our sample that are only detected in our optical data are poorer on average ($4 ) than the X-ray/optically matched clusters, which may partially explain the difference in the detection fractions.

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“…The extent of these effects is also surprisingly unknown; measures of completeness and contamination in the Abell catalog disagree by factors of a few. For instance, Miller et al (1999) claim that under-or overestimation of richness is not a significant problem, whereas van Haarlem, Frenk, & White (1997) suggest that one-third of Abell clusters have incorrect richnesses, and that one-third of rich (R ! 1) clusters are missed.…”

Section: Limitations Of Existing Catalogsmentioning

confidence: 99%

“…The largest study of R ! 1 clusters (Miller et al 1999) suggests projection effects are not of great concern for the Abell catalog; however, completeness cannot be gauged without deeper samples. Unfortunately, some of these problems will plague any optically selected cluster sample, including our own, but objective selection criteria and a strong statistical understanding of the catalog can mitigate their effects.…”

Section: Limitations Of Existing Catalogsmentioning

confidence: 99%

The Northern Sky Optical Cluster Survey. II. An Objective Cluster Catalog for 5800 Square Degrees

Gal

Carvalho

Lopes

et al. 2003

The Astronomical Journal

120

119

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We present a new, objectively defined catalog of candidate galaxy clusters based on the galaxy catalogs from the digitized Second Palomar Observatory Sky Survey. This cluster catalog, derived from the best calibrated plates in the high-latitude (|b| > 30 ) northern Galactic cap region, covers 5800 deg 2 and contains 8155 candidate clusters. A simple adaptive kernel density mapping technique, combined with the SExtractor object detection algorithm, is used to detect galaxy overdensities, which we identify as clusters. Simulations of the background galaxy distribution and clusters of varying richnesses and redshifts allow us to optimize detection parameters and measure the completeness and contamination rates for our catalog. Cluster richnesses and photometric redshifts are measured, using integrated colors and magnitudes for each cluster. An extensive spectroscopic survey is used to confirm the photometric results. This catalog, with well-characterized sample properties, provides a sound basis for future studies of cluster physics and large-scale structure.

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Projection, Spatial Correlations, and Anisotropies in a Large and Complete Sample of Abell Clusters

Cited by 30 publications

References 61 publications

Friends-of-friends groups and clusters in the 2SLAQ catalogue

Friends-of-friends groups and clusters in the 2SLAQ catalogue

ChaMP Serendipitous Galaxy Cluster Survey

The Northern Sky Optical Cluster Survey. II. An Objective Cluster Catalog for 5800 Square Degrees

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