2024-03-28T22:47:35Zhttp://digital.csic.es/dspace-oai/requestoai:digital.csic.es:10261/1706242022-02-07T13:01:50Zcom_10261_37com_10261_4col_10261_290
00925njm 22002777a 4500
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Aghanim, N.
author
Akrami, Y.
author
Ashdown, Mark
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Aumont, J.
author
Baccigalupi, C.
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Ballardini, M.
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Banday, A. J.
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Barreiro, R. Belén
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Bartolo, Nicola
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Basak, S.
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Benabed, K.
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Vittorio, N.
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Wandelt, B. D.
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Enßlin, T. A.
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Wehus, I. K.
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White, Martin
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Zacchei, A.
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Zonca, A.
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Borrill, J.
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Bouchet, F. R.
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Boulanger, F.
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Kim, J.
author
Bracco, Andrea
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Burigana, C.
author
Calabrese, E.
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Eriksen, H. K.
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Cardoso, J. F.
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Challinor, A.
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Chiang, H. C.
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Colombo, L.P.L.
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Combet, C.
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Crill, B. P.
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Kisner, T. S.
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Curto, Andrés
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Cuttaia, F.
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Bernardis, P. de
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Rosa, A. de
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Fantaye, Y.
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Zotti, G. de
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Delabrouille, J.
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Valentino, E. di
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Dickinson, C.
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Diego, José María
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Mennella, A.
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Doré, O.
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Ducout, A.
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Dupac, X.
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Dusini, S.
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Finelli, F.
author
Forastieri, F.
author
Frailis, M.
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Franceschi, E.
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Frolov, A.
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McEwen, J. D.
author
Knox, L.
author
Galeotta, S.
author
Galli, S.
author
Ganga, K.
author
Génova-Santos, R.
author
Gerbino, M.
author
González-Nuevo, J.
author
Górski, K. M.
author
Gratton, S.
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Gruppuso, A.
author
Gudmundsson, J.E.
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Krachmalnicof, N.
author
Meinhold, P. R.
author
Herranz, D.
author
Hivon, E.
author
Huang, Z.
author
Jaffe, A. H.
author
Jones, W. C.
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Keihänen, E.
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Keskitalo, R.
author
Kiiveri, K.
author
Kunz, M.
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Kurki-Suonio, H.
author
Lagache, Guilaine
author
Lamarre, J.-M.
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Lasenby, Anthony N.
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Renzi, A.
author
Lattanzi, M.
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Lawrence, C. R.
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Jeune, M. le
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Migliaccio, M.
author
Levrier, F.
author
Lewis, A.
author
Liguori, Michele
author
Lilje, P. B.
author
Lilley, M.
author
Lindholm, V.
author
Rocha, G.
author
López-Caniego, M.
author
Lubin, P. M.
author
Ma, Y.-Z
author
Macías-Pérez, J. F.
author
Millea, M.
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Maggio, G.
author
Maino, D.
author
Mandolesi, N.
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Mangilli, A.
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Maris, M.
author
Bonaldi, A.
author
Martin, P. G.
author
Martínez-González, Enrique
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Matarrese, S.
author
Mauri, N.
author
Miville-Deschênes, M. A.
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Molinari, D.
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Moneti, A.
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Montier, L.
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Morgante, G.
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Bersanelli, M.
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Rossetti, M.
author
Moss, A.
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Narimani, A.
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Natoli, P.
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Oxborrow, C. A.
author
Pagano, L.
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Paoletti, D.
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Partridge, B.
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Patanchon, G.
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Patrizii, L.
author
Pettorino, V.
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Roudier, G.
author
Bielewicz, P.
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Piacentini, F.
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Polastri, L.
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Polenta, G.
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Puget, J.-L.
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Rachen, J. P.
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Racine, B.
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Reinecke, M.
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Remazeilles, Mathieu
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Rubiño-Martín, J. A.
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Ruiz-Granados, Beatriz
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Salvati, L.
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Sandri, M.
author
Savelainen, M.
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Efstathiou, G.
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Scott, D.
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Sirignano, C.
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Sirri, G.
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Bonavera, Laura
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Stanco, L.
author
Suur-Uski, A.-S.
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Tauber, J. A.
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Tavagnacco, D.
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Tenti, M.
author
Toffolatti, L.
author
Elsner, F.
author
Tomasi, M.
author
Tristram, M.
author
Trombetti, T.
author
Valiviita, J.
author
Bond, J. R.
author
Tent, F. van
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Vielva, P.
author
Villa, F.
author
2017
The 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 τ, the baryon density ωb, the matter density ωm, the angular size of the sound horizon θ∗, 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 ℓ < 800 in the Planck temperature power spectrum) and an all angular-scale data set (ℓ < 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 { Δτ,ΔAse− 2τ,Δns,Δωm,Δωb,Δθ∗ } = { −1.7,−2.2,1.2,−2.0,1.1,0.9 }, with a χ2 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 ℓ < 800 instead to ℓ> 800, or splitting at a different multipole, yields similar results. We examined the ℓ < 800 model residuals in the ℓ> 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 τ, which, at fixed Ase− 2τ, affects the ℓ> 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 ℓ < 800 that leads to somewhat different best-fit parameters than come from the full ℓ range?” We find that if we discard the data at ℓ < 30, where there is a roughly 2σ downward fluctuation in power relative to the model that best fits the full ℓ range, the ℓ < 800 best-fit parameters shift significantly towards the ℓ < 2500 best-fit parameters. In contrast, including ℓ < 30, this previously noted “low-ℓ deficit” drives ns up and impacts parameters correlated with ns, such as ωm and H0. As expected, the ℓ < 30 data have a much greater impact on the ℓ < 800 best fit than on the ℓ < 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-ℓ residuals and the deficit in low-ℓ 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.
Astronomy and Astrophysics 607: A95 (2017)
http://hdl.handle.net/10261/170624
10.1051/0004-6361/201629504
http://dx.doi.org/10.13039/501100003339
http://dx.doi.org/10.13039/100000104
http://dx.doi.org/10.13039/501100004462
http://dx.doi.org/10.13039/501100005184
http://dx.doi.org/10.13039/501100003981
http://dx.doi.org/10.13039/501100002830
http://dx.doi.org/10.13039/501100004794
http://dx.doi.org/10.13039/501100000844
http://dx.doi.org/10.13039/501100000271
http://dx.doi.org/10.13039/501100006111
http://dx.doi.org/10.13039/501100001602
http://dx.doi.org/10.13039/501100000016
http://dx.doi.org/10.13039/501100002347
http://dx.doi.org/10.13039/501100001659
http://dx.doi.org/10.13039/501100000780
http://dx.doi.org/10.13039/501100001871
http://dx.doi.org/10.13039/501100000781
http://dx.doi.org/10.13039/501100002341
http://dx.doi.org/10.13039/100000015
http://dx.doi.org/10.13039/501100010198
Cosmology: theory
Cosmic background radiation
Cosmological parameters
Cosmology: observations
Planck intermediate results LI. Features in the cosmic microwave background temperature power spectrum and shifts in cosmological parameters