Planck intermediate results: LI. Features in the cosmic microwave background temperature power spectrum and shifts in cosmological parameters

dc.contributorAalto Universityen
dc.contributor.authorAghanim, N.en_US
dc.contributor.authorAkrami, Y.en_US
dc.contributor.authorAshdown, M.en_US
dc.contributor.authorAumont, J.en_US
dc.contributor.authorBaccigalupi, C.en_US
dc.contributor.authorBallardini, M.en_US
dc.contributor.authorBanday, A. J.en_US
dc.contributor.authorBarreiro, R. B.en_US
dc.contributor.authorBartolo, N.en_US
dc.contributor.authorBasak, S.en_US
dc.contributor.authorBenabed, K.en_US
dc.contributor.authorBersanelli, M.en_US
dc.contributor.authorBielewicz, P.en_US
dc.contributor.authorBonaldi, A.en_US
dc.contributor.authorBonavera, L.en_US
dc.contributor.authorBond, J. R.en_US
dc.contributor.authorBorrill, J.en_US
dc.contributor.authorBouchet, F. R.en_US
dc.contributor.authorBurigana, C.en_US
dc.contributor.authorCalabrese, E.en_US
dc.contributor.authorCardoso, J. F.en_US
dc.contributor.authorChallinor, A.en_US
dc.contributor.authorChiang, H. C.en_US
dc.contributor.authorColombo, L. P.L.en_US
dc.contributor.authorCombet, C.en_US
dc.contributor.authorCrill, B. P.en_US
dc.contributor.authorCurto, A.en_US
dc.contributor.authorCuttaia, F.en_US
dc.contributor.authorDe Bernardis, P.en_US
dc.contributor.authorDe Rosa, A.en_US
dc.contributor.authorDe Zotti, G.en_US
dc.contributor.authorDelabrouille, J.en_US
dc.contributor.authorDi Valentino, E.en_US
dc.contributor.authorDickinson, C.en_US
dc.contributor.authorDiego, J. M.en_US
dc.contributor.authorDoré, O.en_US
dc.contributor.authorDucout, A.en_US
dc.contributor.authorDupac, X.en_US
dc.contributor.authorDusini, S.en_US
dc.contributor.authorEfstathiou, G.en_US
dc.contributor.authorElsner, F.en_US
dc.contributor.authorEnßlin, T. A.en_US
dc.contributor.authorEriksen, H. K.en_US
dc.contributor.authorFantaye, Y.en_US
dc.contributor.authorFinelli, F.en_US
dc.contributor.authorForastieri, F.en_US
dc.contributor.authorFrailis, M.en_US
dc.contributor.authorFranceschi, E.en_US
dc.contributor.authorFrolov, A.en_US
dc.contributor.authorGaleotta, S.en_US
dc.contributor.authorGalli, S.en_US
dc.contributor.authorGanga, K.en_US
dc.contributor.authorGénova-Santos, R. T.en_US
dc.contributor.authorGerbino, M.en_US
dc.contributor.authorGonzález-Nuevo, J.en_US
dc.contributor.authorGórski, K. M.en_US
dc.contributor.authorGratton, S.en_US
dc.contributor.authorGruppuso, A.en_US
dc.contributor.authorGudmundsson, J. E.en_US
dc.contributor.authorHerranz, D.en_US
dc.contributor.authorHivon, E.en_US
dc.contributor.authorHuang, Z.en_US
dc.contributor.authorJaffe, A. H.en_US
dc.contributor.authorJones, W. C.en_US
dc.contributor.authorKeihänen, E.en_US
dc.contributor.authorKeskitalo, R.en_US
dc.contributor.authorKiiveri, K.en_US
dc.contributor.authorKim, J.en_US
dc.contributor.authorKisner, T. S.en_US
dc.contributor.authorKnox, L.en_US
dc.contributor.authorKrachmalnicoff, N.en_US
dc.contributor.authorKunz, M.en_US
dc.contributor.authorKurki-Suonio, H.en_US
dc.contributor.authorLagache, G.en_US
dc.contributor.authorLamarre, J. M.en_US
dc.contributor.authorLasenby, A.en_US
dc.contributor.authorLattanzi, M.en_US
dc.contributor.authorLawrence, C. R.en_US
dc.contributor.authorLe Jeune, M.en_US
dc.contributor.authorLevrier, F.en_US
dc.contributor.authorLewis, A.en_US
dc.contributor.authorLiguori, M.en_US
dc.contributor.authorLilje, P. B.en_US
dc.contributor.authorLilley, M.en_US
dc.contributor.authorLindholm, V.en_US
dc.contributor.authorLópez-Caniego, M.en_US
dc.contributor.authorLubin, P. M.en_US
dc.contributor.authorMa, Y. Z.en_US
dc.contributor.authorMacías-Pérez, J. F.en_US
dc.contributor.authorMaggio, G.en_US
dc.contributor.authorMaino, D.en_US
dc.contributor.authorMandolesi, N.en_US
dc.contributor.authorMangilli, A.en_US
dc.contributor.authorMaris, M.en_US
dc.contributor.authorMartin, P. G.en_US
dc.contributor.authorMartínez-González, E.en_US
dc.contributor.authorMatarrese, S.en_US
dc.contributor.authorMauri, N.en_US
dc.contributor.authorMcEwen, J. D.en_US
dc.contributor.authorMeinhold, P. R.en_US
dc.contributor.authorMennella, A.en_US
dc.contributor.authorMigliaccio, M.en_US
dc.contributor.authorMillea, M.en_US
dc.contributor.authorMiville-Deschênes, M. A.en_US
dc.contributor.authorMolinari, D.en_US
dc.contributor.authorMoneti, A.en_US
dc.contributor.authorMontier, L.en_US
dc.contributor.authorMorgante, G.en_US
dc.contributor.authorMoss, A.en_US
dc.contributor.authorNarimani, A.en_US
dc.contributor.authorNatoli, P.en_US
dc.contributor.authorOxborrow, C. A.en_US
dc.contributor.authorPagano, L.en_US
dc.contributor.authorPaoletti, D.en_US
dc.contributor.authorPartridge, B.en_US
dc.contributor.authorPatanchon, G.en_US
dc.contributor.authorPatrizii, L.en_US
dc.contributor.authorPettorino, V.en_US
dc.contributor.authorPiacentini, F.en_US
dc.contributor.authorPolastri, L.en_US
dc.contributor.authorPolenta, G.en_US
dc.contributor.authorPuget, J. L.en_US
dc.contributor.authorRachen, J. P.en_US
dc.contributor.authorRacine, B.en_US
dc.contributor.authorReinecke, M.en_US
dc.contributor.authorRemazeilles, M.en_US
dc.contributor.authorRenzi, A.en_US
dc.contributor.authorRocha, G.en_US
dc.contributor.authorRossetti, M.en_US
dc.contributor.authorRoudier, G.en_US
dc.contributor.authorRubiño-Martín, J. A.en_US
dc.contributor.authorRuiz-Granados, B.en_US
dc.contributor.authorSalvati, L.en_US
dc.contributor.authorSandri, M.en_US
dc.contributor.authorSavelainen, M.en_US
dc.contributor.authorScott, D.en_US
dc.contributor.authorSirignano, C.en_US
dc.contributor.authorSirri, G.en_US
dc.contributor.authorStanco, L.en_US
dc.contributor.authorSuur-Uski, A. S.en_US
dc.contributor.authorTauber, J. A.en_US
dc.contributor.authorTavagnacco, D.en_US
dc.contributor.authorTenti, M.en_US
dc.contributor.authorToffolatti, L.en_US
dc.contributor.authorTomasi, M.en_US
dc.contributor.authorTristram, M.en_US
dc.contributor.authorTrombetti, T.en_US
dc.contributor.authorValiviita, J.en_US
dc.contributor.authorVan Tent, F.en_US
dc.contributor.authorVielva, P.en_US
dc.contributor.authorVilla, F.en_US
dc.contributor.authorVittorio, N.en_US
dc.contributor.authorWandelt, B. D.en_US
dc.contributor.authorWehus, I. K.en_US
dc.contributor.authorWhite, Martin J.en_US
dc.contributor.authorZacchei, A.en_US
dc.contributor.authorZonca, A.en_US
dc.contributor.departmentDepartment of Applied Physicsen
dc.contributor.groupauthorTopological Quantum Fluidsen
dc.contributor.organizationUniversité Paris-Suden_US
dc.contributor.organizationLeiden Universityen_US
dc.contributor.organizationUniversity of Cambridgeen_US
dc.contributor.organizationInternational School for Advanced Studiesen_US
dc.contributor.organizationUniversitá di Bolognaen_US
dc.contributor.organizationUniversity of Padovaen_US
dc.contributor.organizationIndian Institute of Science Education and Research Thiruvananthapuramen_US
dc.contributor.organizationUniversity of Milanen_US
dc.contributor.organizationUniversity of Manchesteren_US
dc.contributor.organizationUniversity of Oviedoen_US
dc.contributor.organizationUniversity of Torontoen_US
dc.contributor.organizationLawrence Berkeley National Laboratoryen_US
dc.contributor.organizationUniversity of Ferraraen_US
dc.contributor.organizationCardiff Universityen_US
dc.contributor.organizationObservatoire de Parisen_US
dc.contributor.organizationUniversity of KwaZulu-Natalen_US
dc.contributor.organizationUniversity of Southern Californiaen_US
dc.contributor.organizationUniversité Grenoble Alpesen_US
dc.contributor.organizationCalifornia Institute of Technologyen_US
dc.contributor.organizationIstituto di Astrofisica Spaziale e Fisica Cosmica di Bolognaen_US
dc.contributor.organizationSapienza University of Romeen_US
dc.contributor.organizationAstronomical Observatory of Paduaen_US
dc.contributor.organizationImperial College Londonen_US
dc.contributor.organizationEuropean Space Astronomy Centreen_US
dc.contributor.organizationNational Institute for Nuclear Physicsen_US
dc.contributor.organizationMax Planck Institute for Astrophysicsen_US
dc.contributor.organizationUniversity of Osloen_US
dc.contributor.organizationAfrican Institute for Mathematical Sciencesen_US
dc.contributor.organizationOsservatorio Astronomico di Triesteen_US
dc.contributor.organizationSimon Fraser Universityen_US
dc.contributor.organizationUniversity of Chicagoen_US
dc.contributor.organizationUniversity of La Lagunaen_US
dc.contributor.organizationJet Propulsion Laboratoryen_US
dc.contributor.organizationPrinceton Universityen_US
dc.contributor.organizationSun Yat-sen Universityen_US
dc.contributor.organizationUniversity of Helsinkien_US
dc.contributor.organizationUniversity of California, Davisen_US
dc.contributor.organizationUniversity of Sussexen_US
dc.contributor.organizationUniversity of California, Santa Barbaraen_US
dc.contributor.organizationUniversity College Londonen_US
dc.contributor.organizationItalian Space Agencyen_US
dc.contributor.organizationUniversity of Nottinghamen_US
dc.contributor.organizationUniversity of British Columbiaen_US
dc.contributor.organizationTechnical University of Denmarken_US
dc.contributor.organizationHaverford Collegeen_US
dc.contributor.organizationHeidelberg University en_US
dc.contributor.organizationRadboud University Nijmegenen_US
dc.contributor.organizationUniversity of Granadaen_US
dc.contributor.organizationEuropean Space Research and Technology Centreen_US
dc.contributor.organizationUniversity of Triesteen_US
dc.contributor.organizationUniversity of Rome Tor Vergataen_US
dc.contributor.organizationUniversity of Illinois at Urbana-Champaignen_US
dc.contributor.organizationUniversity of Adelaideen_US
dc.contributor.organizationUniversity of California, San Diegoen_US
dc.contributor.organizationJodrell Bank Centre for Astrophysicsen_US
dc.description.abstractThe six parameters of the standard ΛCDM model have best-fit values derived from the Planck temperature power spectrum that are shifted somewhat from the best-fit values derived from WMAP data. These shifts are driven by features in the Planck temperature power spectrum at angular scales that had never before been measured to cosmic-variance level precision. We have investigated these shifts to determine whether they are within the range of expectation and to understand their origin in the data. Taking our parameter set to be the optical depth of the reionized intergalactic medium, the baryon density ωb, the matter density ωm, the angular size of the sound horizon the spectral index of the primordial power spectrum, ns, and Ase-2τ (where As is the amplitude of the primordial power spectrum), we have examined the change in best-fit values between a WMAP-like large angular-scale data set (with multipole moment < 800 in the Planck temperature power spectrum) and an all angular-scale data set (< 2500Planck temperature power spectrum), each with a prior on τ of 0.07 ± 0.02. We find that the shifts, in units of the 1σ expected dispersion for each parameter, are {value of 8.0. We find that this χ2 value is exceeded in 15% of our simulated data sets, and that a parameter deviates by more than 2.2σ in 9% of simulated data sets, meaning that the shifts are not unusually large. Comparing < 800 instead to > 800, or splitting at a different multipole, yields similar results. We examined the < 800 model residuals in the > 800 power spectrum data and find that the features there that drive these shifts are a set of oscillations across a broad range of angular scales. Although they partly appear similar to the effects of enhanced gravitational lensing, the shifts in ΛCDM parameters that arise in response to these features correspond to model spectrum changes that are predominantly due to non-lensing effects; the only exception is, which, at fixed Ase-2τ, affects the > 800 temperature power spectrum solely through the associated change in As and the impact of that on the lensing potential power spectrum. We also ask, "what is it about the power spectrum at < 800 that leads to somewhat different best-fit parameters than come from the full range?" We find that if we discard the data at < 30, where there is a roughly 2σ downward fluctuation in power relative to the model that best fits the full range, the < 800 best-fit parameters shift significantly towards the < 2500 best-fit parameters. In contrast, including < 30, this previously noted "low-deficit" drives ns up and impacts parameters correlated with ns, such as ωm and H0. As expected, the < 30 data have a much greater impact on the < 800 best fit than on the < 2500 best fit. So although the shifts are not very significant, we find that they can be understood through the combined effects of an oscillatory-like set of high-residuals and the deficit in low-power, excursions consistent with sample variance that happen to map onto changes in cosmological parameters. Finally, we examine agreement between PlanckTT data and two other CMB data sets, namely the Planck lensing reconstruction and the TT power spectrum measured by the South Pole Telescope, again finding a lack of convincing evidence of any significant deviations in parameters, suggesting that current CMB data sets give an internally consistent picture of the ΛCDM model.en
dc.description.versionPeer revieweden
dc.identifier.citationAghanim, N, Akrami, Y, Ashdown, M, Aumont, J, Baccigalupi, C, Ballardini, M, Banday, A J, Barreiro, R B, Bartolo, N, Basak, S, Benabed, K, Bersanelli, M, Bielewicz, P, Bonaldi, A, Bonavera, L, Bond, J R, Borrill, J, Bouchet, F R, Burigana, C, Calabrese, E, Cardoso, J F, Challinor, A, Chiang, H C, Colombo, L P L, Combet, C, Crill, B P, Curto, A, Cuttaia, F, De Bernardis, P, De Rosa, A, De Zotti, G, Delabrouille, J, Di Valentino, E, Dickinson, C, Diego, J M, Doré, O, Ducout, A, Dupac, X, Dusini, S, Efstathiou, G, Elsner, F, Enßlin, T A, Eriksen, H K, Fantaye, Y, Finelli, F, Forastieri, F, Frailis, M, Franceschi, E, Frolov, A, Galeotta, S, Galli, S, Ganga, K, Génova-Santos, R T, Gerbino, M, González-Nuevo, J, Górski, K M, Gratton, S, Gruppuso, A, Gudmundsson, J E, Herranz, D, Hivon, E, Huang, Z, Jaffe, A H, Jones, W C, Keihänen, E, Keskitalo, R, Kiiveri, K, Kim, J, Kisner, T S, Knox, L, Krachmalnicoff, N, Kunz, M, Kurki-Suonio, H, Lagache, G, Lamarre, J M, Lasenby, A, Lattanzi, M, Lawrence, C R, Le Jeune, M, Levrier, F, Lewis, A, Liguori, M, Lilje, P B, Lilley, M, Lindholm, V, López-Caniego, M, Lubin, P M, Ma, Y Z, Macías-Pérez, J F, Maggio, G, Maino, D, Mandolesi, N, Mangilli, A, Maris, M, Martin, P G, Martínez-González, E, Matarrese, S, Mauri, N, McEwen, J D, Meinhold, P R, Mennella, A, Migliaccio, M, Millea, M, Miville-Deschênes, M A, Molinari, D, Moneti, A, Montier, L, Morgante, G, Moss, A, Narimani, A, Natoli, P, Oxborrow, C A, Pagano, L, Paoletti, D, Partridge, B, Patanchon, G, Patrizii, L, Pettorino, V, Piacentini, F, Polastri, L, Polenta, G, Puget, J L, Rachen, J P, Racine, B, Reinecke, M, Remazeilles, M, Renzi, A, Rocha, G, Rossetti, M, Roudier, G, Rubiño-Martín, J A, Ruiz-Granados, B, Salvati, L, Sandri, M, Savelainen, M, Scott, D, Sirignano, C, Sirri, G, Stanco, L, Suur-Uski, A S, Tauber, J A, Tavagnacco, D, Tenti, M, Toffolatti, L, Tomasi, M, Tristram, M, Trombetti, T, Valiviita, J, Van Tent, F, Vielva, P, Villa, F, Vittorio, N, Wandelt, B D, Wehus, I K, White, M J, Zacchei, A & Zonca, A 2017, ' Planck intermediate results : LI. Features in the cosmic microwave background temperature power spectrum and shifts in cosmological parameters ', Astronomy and Astrophysics, vol. 607, A95 .
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dc.relation.ispartofseriesAstronomy and Astrophysicsen
dc.relation.ispartofseriesVolume 607en
dc.subject.keywordCosmic background radiationen_US
dc.subject.keywordCosmological parametersen_US
dc.subject.keywordCosmology: observationsen_US
dc.subject.keywordCosmology: theoryen_US
dc.titlePlanck intermediate results: LI. Features in the cosmic microwave background temperature power spectrum and shifts in cosmological parametersen
dc.typeA1 Alkuperäisartikkeli tieteellisessä aikakauslehdessäfi