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dc.contributor.authorSaro, A.
dc.contributor.authorBocquet, S.
dc.contributor.authorMohr, J.
dc.contributor.authorRozo, E.
dc.contributor.authorBenson, B. A.
dc.contributor.authorDodelson, S.
dc.contributor.authorRykoff, E. S.
dc.contributor.authorBleem, L.
dc.contributor.authorAbbott, T. M. C.
dc.contributor.authorAbdalla, F. B.
dc.contributor.authorAllen, S.
dc.contributor.authorAnnis, J.
dc.contributor.authorBenoit-Levy, A.
dc.contributor.authorBrooks, D.
dc.contributor.authorBurke, D. L.
dc.contributor.authorCapasso, R.
dc.contributor.authorCarnero Rosell, A.
dc.contributor.authorCarrasco Kind, M.
dc.contributor.authorCarretero, J.
dc.contributor.authorChiu, I.
dc.contributor.authorCrawford, T. M.
dc.contributor.authorCunha, C. E.
dc.contributor.authorD'Andrea, C. B.
dc.contributor.authorda Costa, L. N.
dc.contributor.authorDesai, S.
dc.contributor.authorDietrich, J. P.
dc.contributor.authorEvrard, A. E.
dc.contributor.authorNeto, A. Fausti
dc.contributor.authorFlaugher, B.
dc.contributor.authorFosalba, P.
dc.contributor.authorFrieman, J.
dc.contributor.authorGangkofner, C.
dc.contributor.authorGaztanaga, E.
dc.contributor.authorGerdes, D. W.
dc.contributor.authorGiannantonio, T.
dc.contributor.authorGrandis, S.
dc.contributor.authorGruen, D.
dc.contributor.authorGruendl, R. A.
dc.contributor.authorGupta, N.
dc.contributor.authorGutierrez, G.
dc.contributor.authorHolzapfel, W. L.
dc.contributor.authorJames, D. J.
dc.contributor.authorKuehn, K.
dc.contributor.authorKuropatkin, N.
dc.contributor.authorLima, M.
dc.contributor.authorMarshall, J. L.
dc.contributor.authorMcDonald, M.
dc.contributor.authorMelchior, P.
dc.contributor.authorMenanteau, F.
dc.contributor.authorMiquel, R.
dc.contributor.authorOgando, R.
dc.contributor.authorPlazas, A. A.
dc.contributor.authorRapetti, D.
dc.contributor.authorReichardt, C. L.
dc.contributor.authorReil, K.
dc.contributor.authorRomer, A. K.
dc.contributor.authorSanchez, E.
dc.contributor.authorScarpine, V.
dc.contributor.authorSchubnell, M.
dc.contributor.authorSevilla-Noarbe, I.
dc.contributor.authorSmith, R. C.
dc.contributor.authorSoares-Santos, M.
dc.contributor.authorSoergel, B.
dc.contributor.authorStrazzullo, V.
dc.contributor.authorSuchyta, E.
dc.contributor.authorSwanson, M. E. C.
dc.contributor.authorTarle, G.
dc.contributor.authorThomas, D.
dc.contributor.authorVikram, V.
dc.contributor.authorWalker, A. R.
dc.contributor.authorZenteno, A.
dc.date.accessioned2017-06-27T16:35:42Z
dc.date.available2017-06-27T16:35:42Z
dc.date.issued2017-07
dc.identifier.citationOptical-SZE scaling relations for DES optically selected clusters within the SPT-SZ Survey 2017, 468 (3):3347 Monthly Notices of the Royal Astronomical Societyen
dc.identifier.issn0035-8711
dc.identifier.issn1365-2966
dc.identifier.doi10.1093/mnras/stx594
dc.identifier.urihttp://hdl.handle.net/10150/624426
dc.description.abstractWe study the Sunyaev-Zel'dovich effect (SZE) signature in South Pole Telescope (SPT) data for an ensemble of 719 optically identified galaxy clusters selected from 124.6 deg(2) of the Dark Energy Survey (DES) science verification data, detecting a clear stacked SZE signal down to richness lambda similar to 20. The SZE signature is measured using matched-filtered maps of the 2500 deg(2) SPT-SZ survey at the positions of the DES clusters, and the degeneracy between SZE observable and matched-filter size is broken by adopting as priors SZE and optical mass-observable relations that are either calibrated using SPT-selected clusters or through the Arnaud et al. (A10) X-ray analysis. We measure the SPT signal-to-noise zeta - lambda relation and two integrated Compton-y Y500-lambda relations for the DES-selected clusters and compare these to model expectations that account for the SZE-optical centre offset distribution. For clusters with lambda > 80, the two SPT-calibrated scaling relations are consistent with the measurements, while for the A10-calibrated relation the measured SZE signal is smaller by a factor of 0.61 +/- 0.12 compared to the prediction. For clusters at 20 < lambda < 80, the measured SZE signal is smaller by a factor of similar to 0.20-0.80 (between 2.3 sigma and 10 sigma significance) compared to the prediction, with the SPT-calibrated scaling relations and larger lambda clusters showing generally better agreement. We quantify the required corrections to achieve consistency, showing that there is a richness-dependent bias that can be explained by some combination of (1) contamination of the observables and (2) biases in the estimated halo masses. We also discuss particular physical effects associated with these biases, such as contamination of. from line-of-sight projections or of the SZE observables from point sources, larger offsets in the SZE-optical centring or larger intrinsic scatter in the lambda-mass relation at lower richnesses.
dc.description.sponsorshipDFG Cluster of Excellence 'Origin and Structure of the Universe'; Transregio programme 'The Dark Universe' [TR33]; Ludwig-Maximilians-Universitat; National Science Foundation [PLR-1248097, AST-1138766]; NSF Physics Frontier Center [PHY-1125897]; Kavli Foundation; Gordon and Betty Moore Foundation [GBMF 947]; US Department of Energy; US National Science Foundation; Ministry of Science and Education of Spain; Science and Technology Facilities Council of the United Kingdom; Higher Education Funding Council for England; National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign; Kavli Institute of Cosmological Physics at the University of Chicago; Center for Cosmology and Astro-Particle Physics at the Ohio State University; Mitchell Institute for Fundamental Physics and Astronomy at Texas AM University; Financiadora de Estudos e Projetos; Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico; Ministerio da Ciencia, Tecnologia e Inovacao; Deutsche Forschungsgemeinschaft; Collaborating Institutions in the Dark Energy Survey; Argonne National Laboratory; University of California at Santa Cruz; University of Cambridge; Centro de Investigaciones Energeticas; Medioambientales y Tecnologicas-Madrid; University of Chicago; University College London; DES-Brazil Consortium; University of Edinburgh; Eidgenossische Technische Hochschule (ETH) Zurich; Fermi National Accelerator Laboratory; University of Illinois at Urbana-Champaign; Institut de Ciencies de l'Espai (IEEC/CSIC); Institut de Fisica d'Altes Energies; Lawrence Berkeley National Laboratory; Ludwig-Maximilians Universitat Munchen; associated Excellence Cluster Universe; University of Michigan; National Optical Astronomy Observatory; University of Nottingham; Ohio State University; University of Pennsylvania; University of Portsmouth; SLAC National Accelerator Laboratory; Stanford University; University of Sussex; Texas AM University; OzDES Membership Consortium; MINECO [AYA2012-39559, ESP2013-48274, FPA2013-47986]; Centro de Excelencia Severo Ochoa [SEV-2012-0234]; European Research Council under the European Union; ERC [240672, 291329, 306478]en
dc.language.isoenen
dc.publisherOXFORD UNIV PRESSen
dc.relation.urlhttps://academic.oup.com/mnras/article-lookup/doi/10.1093/mnras/stx594en
dc.rights© 2017 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Societyen
dc.subjectmethods: observationalen
dc.subjectmethods: statisticalen
dc.subjectgalaxies: abundancesen
dc.subjectgalaxies: clusters: generalen
dc.subjectlarge-scale structure of Universeen
dc.titleOptical-SZE scaling relations for DES optically selected clusters within the SPT-SZ Surveyen
dc.typeArticleen
dc.contributor.departmentUniv Arizona, Dept Physen
dc.identifier.journalMonthly Notices of the Royal Astronomical Societyen
dc.description.collectioninformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.en
dc.eprint.versionFinal published versionen
refterms.dateFOA2018-06-12T11:38:41Z
html.description.abstractWe study the Sunyaev-Zel'dovich effect (SZE) signature in South Pole Telescope (SPT) data for an ensemble of 719 optically identified galaxy clusters selected from 124.6 deg(2) of the Dark Energy Survey (DES) science verification data, detecting a clear stacked SZE signal down to richness lambda similar to 20. The SZE signature is measured using matched-filtered maps of the 2500 deg(2) SPT-SZ survey at the positions of the DES clusters, and the degeneracy between SZE observable and matched-filter size is broken by adopting as priors SZE and optical mass-observable relations that are either calibrated using SPT-selected clusters or through the Arnaud et al. (A10) X-ray analysis. We measure the SPT signal-to-noise zeta - lambda relation and two integrated Compton-y Y500-lambda relations for the DES-selected clusters and compare these to model expectations that account for the SZE-optical centre offset distribution. For clusters with lambda > 80, the two SPT-calibrated scaling relations are consistent with the measurements, while for the A10-calibrated relation the measured SZE signal is smaller by a factor of 0.61 +/- 0.12 compared to the prediction. For clusters at 20 < lambda < 80, the measured SZE signal is smaller by a factor of similar to 0.20-0.80 (between 2.3 sigma and 10 sigma significance) compared to the prediction, with the SPT-calibrated scaling relations and larger lambda clusters showing generally better agreement. We quantify the required corrections to achieve consistency, showing that there is a richness-dependent bias that can be explained by some combination of (1) contamination of the observables and (2) biases in the estimated halo masses. We also discuss particular physical effects associated with these biases, such as contamination of. from line-of-sight projections or of the SZE observables from point sources, larger offsets in the SZE-optical centring or larger intrinsic scatter in the lambda-mass relation at lower richnesses.


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