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Measurement of Galaxy Cluster Integrated Comptonization and Mass Scaling Relations with the South Pole Telescope

Saliwanchik, B. R. and Lueker, M. and Padin, S. and Shirokoff, E. and Vieira, J. D. (2015) Measurement of Galaxy Cluster Integrated Comptonization and Mass Scaling Relations with the South Pole Telescope. Astrophysical Journal, 799 (2). Art. No. 137. ISSN 0004-637X. https://resolver.caltech.edu/CaltechAUTHORS:20150306-132050855

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Abstract

We describe a method for measuring the integrated Comptonization (Y_(SZ)) of clusters of galaxies from measurements of the Sunyaev-Zel'dovich (SZ) effect in multiple frequency bands and use this method to characterize a sample of galaxy clusters detected in the South Pole Telescope (SPT) data. We use a Markov Chain Monte Carlo method to fit a β-model source profile and integrate Y_(SZ) within an angular aperture on the sky. In simulated observations of an SPT-like survey that include cosmic microwave background anisotropy, point sources, and atmospheric and instrumental noise at typical SPT-SZ survey levels, we show that we can accurately recover β-model parameters for inputted clusters. We measure Y_(SZ) for simulated semi-analytic clusters and find that Y_(SZ) is most accurately determined in an angular aperture comparable to the SPT beam size. We demonstrate the utility of this method to measure Y_(SZ) and to constrain mass scaling relations using X-ray mass estimates for a sample of 18 galaxy clusters from the SPT-SZ survey. Measuring Y_(SZ) within a 0.'75 radius aperture, we find an intrinsic log-normal scatter of 21% ± 11% in Y_(SZ) at a fixed mass. Measuring Y_(SZ) within a 0.3 Mpc projected radius (equivalent to 0.'75 at the survey median redshift z = 0.6), we find a scatter of 26% ± 9%. Prior to this study, the SPT observable found to have the lowest scatter with mass was cluster detection significance. We demonstrate, from both simulations and SPT observed clusters that Y_(SZ) measured within an aperture comparable to the SPT beam size is equivalent, in terms of scatter with cluster mass, to SPT cluster detection significance.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1088/0004-637X/799/2/137DOIArticle
http://iopscience.iop.org/0004-637X/799/2/137PublisherArticle
http://arxiv.org/abs/1312.3015UNSPECIFIEDDiscussion Paper
Additional Information:© 2015 American Astronomical Society. Received 2013 December 10; accepted 2014 November 20; published 2015 January 22. The South Pole Telescope program is supported by the National Science Foundation through grant ANT-0638937. Partial support is also provided by the NSF Physics Frontier Center grant PHY-0114422 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation, and the Gordon and Betty Moore Foundation. We acknowledge the use of the Legacy Archive for Microwave Background Data Analysis (LAMBDA). Support for LAMBDA is provided by the NASA Office of Space Science. Galaxy cluster research at Harvard is supported by NSF grant AST-1009012. Galaxy cluster research at SAO is supported in part by NSF grants AST-1009649 and MRI-0723073. The McGill group acknowledges funding from the National Sciences and Engineering Research Council of Canada, Canada Research Chairs program, and the Canadian Institute for Advanced Research. The Munich group was supported by The Cluster of Excellence “Origin and Structure of the Universe,” funded by the Excellence Initiative of the Federal Government of Germany, EXC project number 153. R.J.F. is supported by a Clay Fellowship, and B.A.B. is supported by a KICP Fellowship. A.P. is supported by an NSF Graduate Research Fellowship under grant No. DGE-1144152. J.H.L. is supported by NASA through the Einstein Fellowship Program under grant No. PF2-130094. M.M. acknowledges support provided by NASA through a Hubble Fellowship grant from STScI. M.D. acknowledges support from an Alfred P. Sloan Research Fellowship, W.F. and C.J. acknowledge support from the Smithsonian Institution, and B.S. acknowledges support from the Brinson Foundation. Facilities: Blanco (MOSAIC), CXO (ACIS), Gemini-South (GMOS), Magellan:Baade (IMACS), Magellan:Clay (LDSS3), SPT, XMM (EPIC)
Funders:
Funding AgencyGrant Number
NSFANT-0638937
NSF Physics Frontier CenterPHY-0114422
Kavli FoundationUNSPECIFIED
Gordon and Betty Moore FoundationUNSPECIFIED
NASAUNSPECIFIED
NSFAST-1009012
NSFAST-1009649
NSFMRI-0723073
Natural Sciences and Engineering Research Council of Canada (NSERC)UNSPECIFIED
Canada Research Chairs programUNSPECIFIED
Canadian Institute for Advanced Research (CIAR)UNSPECIFIED
Excellence Initiative of the Federal Government of GermanyEXC 153
Clay FellowshipUNSPECIFIED
KICP FellowshipUNSPECIFIED
NSF Graduate Research FellowshipDGE-1144152
NASA Einstein FellowshipPF2-130094
NASA Hubble Fellowship STScIUNSPECIFIED
Alfred P. Sloan FoundationUNSPECIFIED
Smithsonian InstitutionUNSPECIFIED
Brinson FoundationUNSPECIFIED
Subject Keywords:galaxies: clusters: general; methods: data analysis; X-rays: galaxies: clusters
Issue or Number:2
Record Number:CaltechAUTHORS:20150306-132050855
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20150306-132050855
Official Citation:Measurement of Galaxy Cluster Integrated Comptonization and Mass Scaling Relations with the South Pole Telescope B. R. Saliwanchik et al. 2015 ApJ 799 137
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:55607
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:06 Mar 2015 21:55
Last Modified:03 Oct 2019 08:07

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