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dc.date.accessioned2023-09-16T15:03:10Z
dc.date.available2023-09-16T15:03:10Z
dc.date.created2023-09-05T10:07:05Z
dc.date.issued2023
dc.identifier.citationAndersen, Kristian Joten Aurvik, Ragnhild Banerji, Ranajoy Basyrov, Artem Bersanelli, M. Bertocco, S. Brilenkov, Maksym Carbone, M. Colombo, L.P.L. Eriksen, Hans Kristian Kamfjord Eskilt, Johannes Røsok Foss, Marie Kristine Franceschet, C. Fuskeland, Unni Galeotta, S. Galloway, Mathew Gerakakis, S. Gjerløw, Eirik Hensley, B. Herman, Daniel Christopher Iacobellis, M. Ieronymaki, M. Ihle, Håvard Tveit Jewell, J.B. Karakci, Ata Keihänen, Elina Keskitalo, R. Lunde, Jonas Gahr Sturtzel Maggio, G. Maino, D. Maris, M. Mennella, A. Paradiso, S. Partridge, B. Reinecke, M. San, Metin Stutzer, Nils-Ole Suur-Uski, A.-S. Svalheim, Trygve Leithe Tavagnacco, D. Thommesen, Harald Watts, Duncan Wehus, Ingunn Kathrine Zacchei, A. . BeyondPlanck: I. Global Bayesian analysis of the Planck Low Frequency Instrument data. Astronomy and Astrophysics (A & A). 2023, 675
dc.identifier.urihttp://hdl.handle.net/10852/105071
dc.description.abstractWe describe the B EYOND P LANCK project in terms of our motivation, methodology, and main products, and provide a guide to a set of companion papers that describe each result in more detail. Building directly on experience from ESA’s Planck mission, we implemented a complete end-to-end Bayesian analysis framework for the Planck Low Frequency Instrument (LFI) observations. The primary product is a full joint posterior distribution P ( ω  ∣  d ), where ω represents the set of all free instrumental (gain, correlated noise, bandpass, etc.), astrophysical (synchrotron, free-free, thermal dust emission, etc.), and cosmological (cosmic microwave background – CMB – map, power spectrum, etc.) parameters. Some notable advantages of this approach compared to a traditional pipeline procedure are seamless end-to-end propagation of uncertainties; accurate modeling of both astrophysical and instrumental effects in the most natural basis for each uncertain quantity; optimized computational costs with little or no need for intermediate human interaction between various analysis steps; and a complete overview of the entire analysis process within one single framework. As a practical demonstration of this framework, we focus in particular on low- ℓ CMB polarization reconstruction with Planck LFI. In this process, we identify several important new effects that have not been accounted for in previous pipelines, including gain over-smoothing and time-variable and non-1/ f correlated noise in the 30 and 44 GHz channels. Modeling and mitigating both previously known and newly discovered systematic effects, we find that all results are consistent with the ΛCDM model, and we constrained the reionization optical depth to τ  = 0.066 ± 0.013, with a low-resolution CMB-based χ 2 probability to exceed of 32%. This uncertainty is about 30% larger than the official pipelines, arising from taking a more complete instrumental model into account. The marginal CMB solar dipole amplitude is 3362.7 ± 1.4 μK, where the error bar was derived directly from the posterior distribution without the need of any ad hoc instrumental corrections. We are currently not aware of any significant unmodeled systematic effects remaining in the Planck LFI data, and, for the first time, the 44 GHz channel is fully exploited in the current analysis. We argue that this framework can play a central role in the analysis of many current and future high-sensitivity CMB experiments, including LiteBIRD, and it will serve as the computational foundation of the emerging community-wide C OSMOGLOBE effort, which aims to combine state-of-the-art radio, microwave, and submillimeter data sets into one global astrophysical model.
dc.languageEN
dc.rightsAttribution 4.0 International
dc.rights.urihttps://creativecommons.org/licenses/by/4.0/
dc.titleBeyondPlanck: I. Global Bayesian analysis of the Planck Low Frequency Instrument data
dc.title.alternativeENEngelskEnglishBeyondPlanck: I. Global Bayesian analysis of the Planck Low Frequency Instrument data
dc.typeJournal article
dc.creator.authorAndersen, Kristian Joten
dc.creator.authorAurvik, Ragnhild
dc.creator.authorBanerji, Ranajoy
dc.creator.authorBasyrov, Artem
dc.creator.authorBersanelli, M.
dc.creator.authorBertocco, S.
dc.creator.authorBrilenkov, Maksym
dc.creator.authorCarbone, M.
dc.creator.authorColombo, L.P.L.
dc.creator.authorEriksen, Hans Kristian Kamfjord
dc.creator.authorEskilt, Johannes Røsok
dc.creator.authorFoss, Marie Kristine
dc.creator.authorFranceschet, C.
dc.creator.authorFuskeland, Unni
dc.creator.authorGaleotta, S.
dc.creator.authorGalloway, Mathew
dc.creator.authorGerakakis, S.
dc.creator.authorGjerløw, Eirik
dc.creator.authorHensley, B.
dc.creator.authorHerman, Daniel Christopher
dc.creator.authorIacobellis, M.
dc.creator.authorIeronymaki, M.
dc.creator.authorIhle, Håvard Tveit
dc.creator.authorJewell, J.B.
dc.creator.authorKarakci, Ata
dc.creator.authorKeihänen, Elina
dc.creator.authorKeskitalo, R.
dc.creator.authorLunde, Jonas Gahr Sturtzel
dc.creator.authorMaggio, G.
dc.creator.authorMaino, D.
dc.creator.authorMaris, M.
dc.creator.authorMennella, A.
dc.creator.authorParadiso, S.
dc.creator.authorPartridge, B.
dc.creator.authorReinecke, M.
dc.creator.authorSan, Metin
dc.creator.authorStutzer, Nils-Ole
dc.creator.authorSuur-Uski, A.-S.
dc.creator.authorSvalheim, Trygve Leithe
dc.creator.authorTavagnacco, D.
dc.creator.authorThommesen, Harald
dc.creator.authorWatts, Duncan
dc.creator.authorWehus, Ingunn Kathrine
dc.creator.authorZacchei, A.
cristin.unitcode185,15,3,0
cristin.unitnameInstitutt for teoretisk astrofysikk
cristin.ispublishedtrue
cristin.fulltextoriginal
cristin.qualitycode2
dc.identifier.cristin2172378
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 (A & A)&rft.volume=675&rft.spage=&rft.date=2023
dc.identifier.jtitleAstronomy and Astrophysics (A & A)
dc.identifier.volume675
dc.identifier.pagecount61
dc.identifier.doihttps://doi.org/10.1051/0004-6361/202244953
dc.subject.nviVDP::Astrofysikk, astronomi: 438
dc.type.documentTidsskriftartikkel
dc.type.peerreviewedPeer reviewed
dc.source.issn0004-6361
dc.type.versionPublishedVersion
cristin.articleidA1


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