Southern Cosmology Survey. Ii. Massive Optically Selected Clusters From 70 Square Degrees of the Sunyaev–zel'dovich Effect Common Survey Area

Menanteau, F.; Hughes, John P.; Barrientos, L. Felipe; Deshpande, Amruta J.; Hilton, Matthew; Infante, L.; Jiménez, Raúl; Kosowsky, Arthur; Moodley, Kavilan; Spergel, David N.; Verde, Licia

doi:10.1088/0067-0049/191/2/340

Cited by 40 publications

(40 citation statements)

References 50 publications

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“…The system SPT-CL J2332-5358 ranks among the hottest known clusters (T = 9.3 keV) and is exceptionally massive (M 200 1 × 10 15 M ). Our mass estimate is in excellent agreement with the ROSAT-based result of Menanteau et al (2010). The SZE-inferred mass reported by V10 is M 500 = 5.20 ± 0.86 ± 0.83 × 10 14 M , where the error bars represent the statistical and systematic uncertainties, both at 68% confidence.…”

Section: Discussionsupporting

confidence: 87%

“…We fitted the spectrum with a single temperature MEKAL model, fixing the column density to the galactic value n H = 1.62 × 10 20 cm −2 (Dickey & Lockman 1990), metal abundance to Z = 0.3 Z and redshift to z = 0.32 (photometric, High et al 2010; consitent with Menanteau et al 2010). To avoid biases stemming from analyzing low-count spectra, we used a minimally binned spectrum (≥1 cts/bin) and C-statistics.…”

Section: X-ray Spectroscopymentioning

confidence: 99%

“…These clusters were independently detected by SPT (V10) and confirmed to be coincident with overdensities of red galaxies (High et al 2010). In addition, SPT-CL J2332-5358 has been recently detected in the optical (SCSO J233227-535827, Menanteau et al 2010). This source is also coincident with the X-ray source 1RXS J233224.3-535840 in the ROSAT Bright Source Catalog (Voges et al 1999).…”

Section: Introductionmentioning

confidence: 99%

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XMM-Newton detection of two clusters of galaxies with strong SPT Sunyaev-Zel'dovich effect signatures

Šuhada¹,

Song

Böhringer³

et al. 2010

A&A

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We report on the discovery of two galaxy clusters, SPT-CL J2332-5358 and SPT-CL J2342-5411, in X-rays. These clusters were also independently detected through their Sunyaev-Zel'dovich effect by the South Pole Telescope, and in the optical band by the Southern Cosmology Survey. They are thus the first clusters detected under survey conditions by all major cluster search approaches. The X-ray detection is made within the frame of the XMM-BCS cluster survey utilizing a novel XMM-Newton mosaic-mode of observations. The present study makes the first scientific use of this operation mode. We estimate the X-ray spectroscopic temperature of SPT-CL J2332-5358 (at redshift z = 0.32) to be T = 9.3 +3.3 −1.9 keV, implying a high mass, M 500 = 8.8 ± 3.8 × 10 14 M . For SPT-CL J2342-5411, at z = 1.08, the available X-ray data do not allow us to directly estimate the temperature with good confidence. However, using our measured luminosity and scaling relations we estimate that T = 4.5 ± 1.3 keV and M 500 = 1.9 ± 0.8 × 10 14 M . We find a good agreement between the X-ray masses and those estimated from the Sunyaev-Zel'dovich effect.

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Section: Discussionsupporting

confidence: 87%

Section: X-ray Spectroscopymentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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XMM-Newton detection of two clusters of galaxies with strong SPT Sunyaev-Zel'dovich effect signatures

Šuhada¹,

Song

Böhringer³

et al. 2010

A&A

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“…The BCS obtained contiguous deep optical imaging in the griz bands across their survey fields, and these data have been processed using a development version 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 2011). These data are publicly available through the NOAO Survey Program and have been used by other groups to study clusters in the SPT survey region (Menanteau et al , 2010 High et al (2010). d Based on Chandra/XMM-Newton count rate in the 0.5-7.0 keV band, within 0.5 r 500 .…”

Section: Optical Imaging and Spectroscopymentioning

confidence: 99%

X-Ray Properties of the First Sunyaev-Zel'dovich Effect Selected Galaxy Cluster Sample From the South Pole Telescope

Andersson

Benson

Ade

et al. 2011

ApJ

145

169

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We present results of X-ray observations of a sample of 15 clusters selected via their imprint on the cosmic microwave background from the thermal Sunyaev-Zel'dovich (SZ) effect. These clusters are a subset of the first SZ-selected cluster catalog, obtained from observations of 178 deg 2 of sky surveyed by the South Pole Telescope (SPT). Using X-ray observations with Chandra and XMM-Newton, we estimate the temperature, T X , and mass, M g , of the intracluster medium within r 500 for each cluster. From these, we calculate Y X = M g T X and estimate the total cluster mass using an M 500 -Y X scaling relation measured from previous X-ray studies. The integrated Comptonization, Y SZ , is derived from the SZ measurements, using additional information from the X-ray-measured gas density profiles and a universal temperature profile. We calculate scaling relations between the X-ray and SZ observables and find results generally consistent with other measurements and the expectations from simple selfsimilar behavior. Specifically, we fit a Y SZ -Y X relation and find a normalization of 0.82 ± 0.07, marginally consistent with the predicted ratio of Y SZ /Y X = 0.91 ± 0.01 that would be expected from the density and temperature models used in this work. Using the Y X -derived mass estimates, we fit a Y SZ -M 500 relation and find a slope consistent with the self-similar expectation of Y SZ ∝ M 5/3 with a normalization consistent with predictions from other X-ray studies. We find that the SZ mass estimates, derived from cosmological simulations of the SPT survey, are lower by a factor of 0.78 ± 0.06 relative to the X-ray mass estimates. This offset is at a level of 1.3σ when considering the ∼15% systematic uncertainty for the simulation-based SZ masses. Overall, the X-ray measurements confirm that the scaling relations of the SZ-selected clusters are consistent with the properties of other X-ray-selected samples of massive clusters, even allowing for the broad redshift range (0.29 < z < 1.08) of the sample.

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“…Unavailability or infeasibility also occurs at lower redshift (e.g. Faloon et al 2013;Menanteau et al 2010), because of the cost of following up large cluster samples in X-ray.…”

Section: Introductionmentioning

confidence: 99%

The insignificant evolution of the richness-mass relation of galaxy clusters

Andreon

Congdon

2014

A&A

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We analysed the richness-mass scaling of 23 very massive clusters at 0.15 < z < 0.55 with homogenously measured weak-lensing masses and richnesses within a fixed aperture of 0.5 Mpc radius. We found that the richness-mass scaling is very tight (the scatter is <0.09 dex with 90% probability) and independent of cluster evolutionary status and morphology. This implies a close association between infall and evolution of dark matter and galaxies in the central region of clusters. We also found that the evolution of the richness-mass intercept is minor at most, and, given the minor mass evolution across the studied redshift range, the richness evolution of individual massive clusters also turns out to be very small. Finally, it was paramount to account for the cluster mass function and the selection function. Ignoring them would lead to larger biases than the (otherwise quoted) errors. Our study benefits from: a) weak-lensing masses instead of proxy-based masses thereby removing the ambiguity between a real trend and one induced by an accounted evolution of the used mass proxy; b) the use of projected masses that simplify the statistical analysis thereby not requiring consideration of the unknown covariance induced by the cluster orientation/triaxiality; c) the use of aperture masses as they are free of the pseudo-evolution of mass definitions anchored to the evolving density of the Universe; d) a proper accounting of the sample selection function and of the Malmquist-like effect induced by the cluster mass function; e) cosmological simulations for the computation of the cluster mass function, its evolution, and the mass growth of each individual cluster.

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Southern Cosmology Survey. Ii. Massive Optically Selected Clusters From 70 Square Degrees of the Sunyaev–zel'dovich Effect Common Survey Area

Cited by 40 publications

References 50 publications

XMM-Newton detection of two clusters of galaxies with strong SPT Sunyaev-Zel'dovich effect signatures

XMM-Newton detection of two clusters of galaxies with strong SPT Sunyaev-Zel'dovich effect signatures

X-Ray Properties of the First Sunyaev-Zel'dovich Effect Selected Galaxy Cluster Sample From the South Pole Telescope

The insignificant evolution of the richness-mass relation of galaxy clusters

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