GALAXY CLUSTERS SELECTED WITH THE SUNYAEV–ZEL'DOVICH EFFECT FROM 2008 SOUTH POLE TELESCOPE OBSERVATIONS

By F. High, B. Stalder, J. Song, P. Ade, K. Aird, S. Allam, R. Armstrong, W. Barkhouse, B. Benson, E. Bertin and 61 more. 2010

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We present a detection-significance-limited catalog of 21 Sunyaev–Zel'dovich-selected galaxy clusters. These clusters, along with one unconfirmed candidate, were identified in 178 deg2 of sky surveyed in 2008 by the South Pole Telescope (SPT) to a depth of 18 μK arcmin at 150 GHz. Optical imaging from the Blanco Cosmology Survey (BCS) and Magellan telescopes provided photometric (and in some cases spectroscopic) redshift estimates, with catalog redshifts ranging from z = 0.15 to z>1, with a median z = 0.74. Of the 21 confirmed galaxy clusters, 3 were previously identified as Abell clusters, 3 were presented as SPT discoveries in Staniszewski et al., and 3 were first identified in a recent analysis of BCS data by Menanteau et al.; the remaining 12 clusters are presented for the first time in this work. Simulated observations of the SPT fields predict the sample to be nearly 100% complete above a mass threshold of M200 ≈ 5 × 1014 M☉ h−1 at z = 0.6. This completeness threshold pushes to lower mass with increasing redshift, dropping to ∼4 × 1014 M☉ h−1 at z = 1. The size and redshift distribution of this catalog are in good agreement with expectations based on our current understanding of galaxy clusters and cosmology. In combination with other cosmological probes, we use this cluster catalog to improve estimates of cosmological parameters. Assuming a standard spatially flat wCDM cosmological model, the addition of our catalog to the WMAP seven-year results yields σ8 = 0.81 ± 0.09 and w = −1.07 ± 0.29, a ∼50% improvement in precision on both parameters over WMAP7 alone.

Subfields: Astronomy and Astrophysics, Electrical and Electronic Engineering, Instrumentation

View Paper: https://www.semanticscholar.org/paper/07a54d22fcd0cf1baedf65f200d02bc04e97a779

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Citations in the corpus

THE ATACAMA COSMOLOGY TELESCOPE: COSMOLOGY FROM GALAXY CLUSTERS DETECTED VIA THE SUNYAEV–ZEL'DOVICH EFFECT (2010, methodology): “We assume for the relation between the SZ signal and mass the general parameterized form36 36 Note that the form of this relation is analogous to that in Vanderlinde et al. (2010). y true = A ( M true M0 )B( 1 + z 1 + z0 )C , (5) where M0 = 5 × 1014 M h−1 and z0 = 0.5.”
The MCXC: a meta-catalogue of x-ray detected clusters of galaxies (2010, background): “…the South Pole Telescope (SPT, Carlstrom et al. 2009) survey, the Atacama Cosmology Telescope (ACT, Fowler et al. 2007), and Planck (Tauber et al. 2010), are actively ongoing and have started providing the first SZ-selected cluster catalogues (e.g., Vanderlinde et al. 2010; Menanteau et al. 2010).”
Weighing the Giants - I. Weak-lensing masses for 51 massive galaxy clusters: project overview, data analysis methods and cluster images (2012, background): “Current and up-coming cluster surveys, such as the South Pole Telescope survey (SPT, Vanderlinde et al. 2010), the Atacama Cosmology Telescope (ACT, Sehgal et al. 2011), Planck (Planck Collaboration et al. 2011), the Dark Energy Survey (The Dark Energy Survey Collaboration 2005, DES), and eROSITA…”
A mature cluster with X-ray emission at z = 2.07 (2010, background): “Assuming Gaussian initial conditions and concordance cosmology withσ8 = 0.8 (Vanderlinde et al. 2010), the probability of finding a dark matter halo withz ≥ 2.07 and a mass greater than 5×1013 M⊙ in the survey area of 400 arcmin2 is 3.3×10−2.”
GALAXY CLUSTERS DISCOVERED VIA THE SUNYAEV–ZEL'DOVICH EFFECT IN THE 2500-SQUARE-DEGREE SPT-SZ SURVEY (2014, methodology): “…using preexisting imaging from the Blanco Cosmology Survey (BCS; Menanteau et al. 2010b; Desai et al. 2012; Bleem et al. 2015, see Section 4.3) as well as targeted imaging on the Blanco/ MOSAIC-II49, and Magellan/IMACS imagers (Dressler et al. 2006) (see High et al. 2010 for more details).”
Planck2013 results. XXIX. ThePlanckcatalogue of Sunyaev-Zeldovich sources (2013, methodology): “At millimetre wavelengths, we cross-check thePlanckSZ catalogue with the recent ACT and SPT samples (Menanteau et al. 2010; Vanderlinde et al. 2010; Williamson et al. 2011), including the most recent data that increased the number of SZ detections and updated the redshift estimates for the clusters…”
A MEASUREMENT OF THE DAMPING TAIL OF THE COSMIC MICROWAVE BACKGROUND POWER SPECTRUM WITH THE SOUTH POLE TELESCOPE (2011, result): “…question, we consider the galaxy cluster abundance measurement of Vikhlinin et al. (2009), which directly and tightly constrains σ8 and is consistent with other measurements of structure at low to medium redshift (Rozo et al. 2010; Mantz et al. 2010b; Vanderlinde et al. 2010; Sehgal et al. 2010b).”
IMPACT OF CLUSTER PHYSICS ON THE SUNYAEV–ZEL'DOVICH POWER SPECTRUM (2010, background): “…(Kosowsky 2003) and Planck5 are currently surveying the microwave sky with the goal of identifying clusters via their SZ signature on the cosmic microwave background (CMB), thus constructing large catalogs of galaxy clusters that are uniformly selected by SZ flux (Vanderlinde et al. 2010).”
X-RAY PROPERTIES OF THE FIRST SUNYAEV–ZEL'DOVICH EFFECT SELECTED GALAXY CLUSTER SAMPLE FROM THE SOUTH POLE TELESCOPE (2010, methodology): “…of the DES data management system (Ngeow et al. 2006; Mohr et al. 2008) and then used in the study of the galaxy population and in the redshift estimation of the first SPT survey fields (Ngeow et al. 2009; Staniszewski et al. 2009; High et al. 2010; Brodwin et al. 2010; Zenteno et al. 2010).”
Towards a realistic population of simulated galaxy groups and clusters (2013, background): “Simultaneously, large optical cluster catalogues became available from the Sloan Digital Sky Survey (SDSS; York et al. 2000) and Sunyaev–Zel’dovich (hereafter SZ) observations progressed from the first reliable detections of individual objects (e.g. Birkinshaw, Hughes & Arnaud 1991; Jones et al. 199”
The XMM Cluster Survey:Optical analysis methodology and the first data release (2011, methodology): “For example, Song et al. (2011) and High et al. (2010) achieve typical uncertainties of 2 per cent in ∆z/(1 + z), to z < 0.5 and z < 1 respectively, using multi-colour data (both studies use the mean colour of the red-sequence as the cluster redshift estimator).”
COSMOLOGICAL CONSTRAINTS FROM GALAXY CLUSTERS IN THE 2500 SQUARE-DEGREE SPT-SZ SURVEY (2016, background): “%) purity, and the redshift cut allows for a nearly redshift-independent selection function (Vanderlinde et al. 2010, hereafter V10).”
The Atacama Cosmology Telescope: Sunyaev-Zel'dovich selected galaxy clusters at 148 GHz from three seasons of data (2013, methodology): “In cases where suitable X-ray or optical constraints on the cluster scale are not available, authors have constructed empirical scaling relations based on alternative SZ statistics, such as the amplitude returned by some particular filter [98], or the maximum S/N over some ensemble of filters [114].”