AMiBA: SCALING RELATIONS BETWEEN THE INTEGRATED COMPTON-<i>y</i>AND X-RAY-DERIVED TEMPERATURE, MASS, AND LUMINOSITY

Huang, Chih-Wei L.; Wu, Jiun-Huei Proty; Ho, P. T. P.; Koch, Patrick M.; Liao, Yu-Wei; Lin, Kai-Yang; Liu, Guo-Chin; Molnar, Sandor M.; Nishioka, Hiroaki; Umetsu, Keiichi; Wang, Fu-Cheng; Altamirano, Pablo; Birkinshaw, Mark; Chang, Chia‐Hao; Chang, Shu-Hao; Chang, Su-Wei; Chen, Ming-Tang; Chiueh, Tzihong; Han, Chih-Chiang; Huang, Yau-De; Hwang, Yuh-Jing; Jiang, Homin; Kesteven, Michael; Kubo, Derek; Li, Chao-Te; Martin-Cocher, Pierre; Oshiro, Peter; Raffin, Philippe; Wei, Tashun; Wilson, W. E.

doi:10.1088/0004-637x/716/1/758

Cited by 15 publications

(14 citation statements)

References 42 publications

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“…These instruments thereby provide additional data outside of the survey areas of the dedicated survey instruments (notably in the Northern Hemisphere), in part to further improve the SZEobservable/mass calibration. Some examples of SZE results derived from such instruments are: the Atacama Pathfinder Experiment-SZ (APEX-SZ) (Nord et al 2009), the Arcminute Microkelvin Imager (AMI) (AMI Consortium et al 2012), the SZ Array (SZA) (Reese et al 2012), the Array for Microwave Background Anisotropy (AMiBA) (Huang et al 2010), and Bolocam (Sayers et al 2011). There have also been a handful of SZEobservable/mass scaling relations derived from pointed observations of previously known clusters (e.g., Bonamente et al 2008;Marrone et al 2009Marrone et al , 2012Plagge et al 2010;Bender et al 2014).…”

Section: Introductionmentioning

confidence: 99%

GALAXY CLUSTER SCALING RELATIONS BETWEEN BOLOCAM SUNYAEV–ZEL’DOVICH EFFECT ANDCHANDRAX-RAY MEASUREMENTS

Czakon

Sayers

Mantz

et al. 2015

ApJ

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We present scaling relations between the integrated Sunyaev-Zel'dovich Effect (SZE) signal, Y SZ , its X-ray analogue, Y X ≡M gas T X , and total mass, M tot , for the 45 galaxy clusters in the Bolocam X-ray-SZ (BOXSZ) sample. All parameters are integrated within r 2500 . Y 2500 values are measured using SZE data collected with Bolocam, operating at 140 GHz at the Caltech Submillimeter Observatory (CSO). The temperature, T X , and mass, M gas,2500 , of the intracluster medium are determined using X-ray data collected with Chandra, and M tot is derived from M gas assuming a constant gas mass fraction. Our analysis accounts for several potential sources of bias, including: selection effects, contamination from radio point sources, and the loss of SZE signal due to noise filtering and beam-smoothing effects. We measure the Y 2500 -Y X scaling to have a power-law index of 0.84 ± 0.07, and a fractional intrinsic scatter in Y 2500 of (21 ± 7)% at fixed Y X , both of which are consistent with previous analyses. We also measure the scaling between Y 2500 and M 2500 , finding a power-law index of 1.06 ± 0.12 and a fractional intrinsic scatter in Y 2500 at fixed mass of (25 ± 9)%. While recent SZE scaling relations using X-ray mass proxies have found power-law indices consistent with the self-similar prediction of 5/3, our measurement stands apart by differing from the self-similar prediction by approximately 5σ. Given the good agreement between the measured Y 2500 -Y X scalings, much of this discrepancy appears to be caused by differences in the calibration of the X-ray mass proxies adopted for each particular analysis.

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Section: Introductionmentioning

confidence: 99%

GALAXY CLUSTER SCALING RELATIONS BETWEEN BOLOCAM SUNYAEV–ZEL’DOVICH EFFECT ANDCHANDRAX-RAY MEASUREMENTS

Czakon

Sayers

Mantz

et al. 2015

ApJ

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“…other cluster observables, especially those which trace mass (e.g., Benson et al 2004;Bonamente et al 2008;McInnes et al 2009;Marrone et al 2009;Melin et al 2011;Huang et al 2010;Plagge et al 2010;Culverhouse et al 2010). The SZ/X-ray and SZ/optical lensing correlations provide the mass calibration necessary for understanding the cluster mass function through cosmic time.…”

Section: Introductionmentioning

confidence: 99%

THE ATACAMA COSMOLOGY TELESCOPE: SUNYAEV-ZEL'DOVICH-SELECTED GALAXY CLUSTERS AT 148 GHz IN THE 2008 SURVEY

Marriage¹,

Acquaviva²,

Ade³

et al. 2011

ApJ

257

227

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We report on 23 clusters detected blindly as Sunyaev-Zel'dovich (SZ) decrements in a 148 GHz, 455 deg 2 map of the southern sky made with data from the Atacama Cosmology Telescope 2008 observing season. All SZ detections announced in this work have confirmed optical counterparts. Ten of the clusters are new discoveries. One newly discovered cluster, ACT-CL J0102−4915, with a redshift of 0.75 (photometric), has an SZ decrement comparable to the most massive systems at lower redshifts. Simulations of the cluster recovery method reproduce the sample purity measured by optical follow-up. In particular, for clusters detected with a signal-to-noise ratio greater than six, simulations are consistent with optical follow-up that demonstrated this subsample is 100% pure. The simulations further imply that the total sample is 80% complete for clusters with mass in excess of 6 × 10 14 solar masses referenced to the cluster volume characterized by 500 times the critical density. The Compton y-X-ray luminosity mass comparison for the 11 best-detected clusters visually agrees with both self-similar and non-adiabatic, simulation-derived scaling laws.

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“…In order to fully use cluster surveys for cosmological purposes, independent and robust estimates of the cluster masses are needed. Several studies have explored the relation between the integrated SZ signal Y and total cluster mass M for massive clusters (M > 10 14 M ⊙ ) (i.e., Benson et al 2004;Bonamente et al 2008;Melin et al 2011;Huang et al 2010;Plagge et al 2010). The integrated SZ signal is defined as…”

Section: Introductionmentioning

confidence: 99%

The Atacama Cosmology Telescope: Detection of Sunyaev-Zel'dovich Decrement in Groups and Clusters Associated With Luminous Red Galaxies

Hand

Appel

Battaglia

et al. 2011

ApJ

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We present a detection of the Sunyaev-Zel'dovich (SZ) decrement associated with the Luminous Red Galaxy (LRG) sample of the Sloan Digital Sky Survey. The SZ data come from 148 GHz maps of the equatorial region made by the Atacama Cosmology Telescope (ACT). The LRG sample is divided by luminosity into four bins, and estimates for the central SZ temperature decrement are calculated through a stacking process. We detect and account for a bias of the SZ signal due to weak radio sources. We use numerical simulations to relate the observed decrement to Y 200 and clustering properties to relate the galaxy luminosity to halo mass. We also use a relation between brightest cluster galaxy luminosity and cluster mass based on stacked gravitational lensing measurements to estimate the characteristic halo masses. The masses are found to be around 10 14 M ⊙ .

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AMiBA: SCALING RELATIONS BETWEEN THE INTEGRATED COMPTON-yAND X-RAY-DERIVED TEMPERATURE, MASS, AND LUMINOSITY

Cited by 15 publications

References 42 publications

GALAXY CLUSTER SCALING RELATIONS BETWEEN BOLOCAM SUNYAEV–ZEL’DOVICH EFFECT ANDCHANDRAX-RAY MEASUREMENTS

GALAXY CLUSTER SCALING RELATIONS BETWEEN BOLOCAM SUNYAEV–ZEL’DOVICH EFFECT ANDCHANDRAX-RAY MEASUREMENTS

THE ATACAMA COSMOLOGY TELESCOPE: SUNYAEV-ZEL'DOVICH-SELECTED GALAXY CLUSTERS AT 148 GHz IN THE 2008 SURVEY

The Atacama Cosmology Telescope: Detection of Sunyaev-Zel'dovich Decrement in Groups and Clusters Associated With Luminous Red Galaxies

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