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dc.date.accessioned2017-08-10T11:59:05Z
dc.date.available2017-08-10T11:59:05Z
dc.date.created2015-08-17T09:32:03Z
dc.date.issued2015
dc.identifier.citationRadovich, M. Formicola, I. Meneghetti, M. Bartalucci, I. Bourdin, H. Mazzotta, P. Moscardini, L. Ettori, S. Arnaud, M. Pratt, G. W. Aghanim, N. Dahle, Håkon Douspis, M. Pointecouteau, E. Grado, A. . A weak lensing analysis of the PLCK G100.2-30.4 cluster. Astronomy and Astrophysics. 2015, 579
dc.identifier.urihttp://hdl.handle.net/10852/56930
dc.description.abstractWe present a mass estimate of the Planck-discovered cluster PLCK G100.2-30.4, derived from a weak lensing analysis of deep Subaru griz images. We perform a careful selection of the background galaxies using the multi-band imaging data, and undertake the weak lensing analysis on the deep (1 h) r −band image. The shape measurement is based on the Kaiser-Squires-Broadhurst algorithm; we adopt the PSFex software to model the point spread function (PSF) across the field and correct for this in the shape measurement. The weak lensing analysis is validated through extensive image simulations. We compare the resulting weak lensing mass profile and total mass estimate to those obtained from our re-analysis of XMM-Newton observations, derived under the hypothesis of hydrostatic equilibrium. The total integrated mass profiles agree remarkably well, within 1σ across their common radial range. A mass M500 ~ 7 × 1014M⊙ is derived for the cluster from our weak lensing analysis. Comparing this value to that obtained from our reanalysis of XMM-Newton data, we obtain a bias factor of (1−b) = 0.8 ± 0.1. This is compatible within 1σ with the value of (1-b) obtained in Planck 2015 from the calibration of the bias factor using newly available weak lensing reconstructed masses. Reproduced with permission from Astronomy & Astrophysics, © ESOen_US
dc.languageEN
dc.publisherEDP Sciences
dc.titleA weak lensing analysis of the PLCK G100.2-30.4 clusteren_US
dc.typeJournal articleen_US
dc.creator.authorRadovich, M.
dc.creator.authorFormicola, I.
dc.creator.authorMeneghetti, M.
dc.creator.authorBartalucci, I.
dc.creator.authorBourdin, H.
dc.creator.authorMazzotta, P.
dc.creator.authorMoscardini, L.
dc.creator.authorEttori, S.
dc.creator.authorArnaud, M.
dc.creator.authorPratt, G. W.
dc.creator.authorAghanim, N.
dc.creator.authorDahle, Håkon
dc.creator.authorDouspis, M.
dc.creator.authorPointecouteau, E.
dc.creator.authorGrado, A.
cristin.unitcode185,15,3,0
cristin.unitnameInstitutt for teoretisk astrofysikk
cristin.ispublishedtrue
cristin.fulltextoriginal
cristin.qualitycode2
dc.identifier.cristin1258260
dc.identifier.bibliographiccitationinfo:ofi/fmt:kev:mtx:ctx&ctx_ver=Z39.88-2004&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.jtitle=Astronomy and Astrophysics&rft.volume=579&rft.spage=&rft.date=2015
dc.identifier.jtitleAstronomy and Astrophysics
dc.identifier.volume579
dc.identifier.pagecount11
dc.identifier.doihttp://dx.doi.org/10.1051/0004-6361/201425600
dc.identifier.urnURN:NBN:no-59675
dc.type.documentTidsskriftartikkelen_US
dc.type.peerreviewedPeer reviewed
dc.source.issn0004-6361
dc.identifier.fulltextFulltext https://www.duo.uio.no/bitstream/handle/10852/56930/1/aa25600-14.pdf
dc.type.versionPublishedVersion
cristin.articleidA7


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