Planck intermediate results LI. Features in the cosmic microwave background temperature power spectrum and shifts in cosmological parameters
Aghanim, N.52; Akrami, Y.54,56; Ashdown, M.6,63; Aumont, J.52; Baccigalupi, C.78; Ballardini, M.29,44,47; Banday, A. J.9,91; Barreiro, R. B.58; Bartolo, N.28,59; Basak, S.84; Benabed, K.53,90; Bersanelli, M.32,45; Bielewicz, P.9,75,78; Bonaldi, A.61; Bonavera, L.16; Bond, J. R.8; Borrill, J.12,88; Bouchet, F. R.53,86; Burigana, C.30,44,47; Calabrese, E.81; Cardoso, J. -F.1,53,66,67; Challinor, A.11,55,63; Chiang, H. C.7,23; Colombo, L. P. L.20,60; Combet, C.68; Crill, B. P.10,60; Curto, A.6,58,63; Cuttaia, F.44; de Bernardis, P.31; de Rosa, A.44; de Zotti, G.42,78; Delabrouille, J.1; Di Valentino, E.53,86; Dickinson, C.61; Diego, J. M.58; Dore, O.10,60; Ducout, A.51,53; Dupac, X.35; Dusini, S.59; Efstathiou, G.55,63; Elsner, F.73; Ensslin, T. A.73; Eriksen, H. K.56; Fantaye, Y.2,18; Finelli, F.44,47; Forastieri, F.30,48; Frailis, M.43; Franceschi, E.44; Frolov, A.85; Galeotta, S.43; Galli, S.62; Ganga, K.1; Genova-Santos, R. T.15,57; Gerbino, M.31,76,89; Gonzalez-Nuevo, J.16,58; Gorski, K. M.60,93; Gratton, S.55,63; Gruppuso, A.44,47; Gudmundsson, J. E.23,89; Herranz, D.58; Hivon, E.53,90; Huang, Z.82; Jaffe, A. H.51; Jones, W. C.23; Keihanen, E.22; Keskitalo, R.12; Kiiveri, K.22,41; Kim, J.73; Kisner, T. S.71; Knox, L.25; Krachmalnicoff, N.78; Kunz, M.2,14,52; Kurki-Suonio, H.22,41; Lagache, G.5,52; Lamarre, J. -M.65; Lasenby, A.6,63; Lattanzi, M.30,48; Lawrence, C. R.60; Le Jeune, M.1; Levrier, F.65; Lewis, A.21; Liguori, M.28,59; Lilje, P. B.56; Lilley, M.53,86; Lindholm, V.22,41; Lopez-Caniego, M.35; Lubin, P. M.26; Ma, Y. -Z.61,77,80; Macias-Perez, J. F.68; Maggio, G.43; Maino, D.32,45; Mandolesi, N.30,44; Mangilli, A.52,64; Maris, M.43; Martin, P. G.8; Martinez-Gonzalez, E.58; Matarrese, S.28,37,59; Mauri, N.47; McEwen, J. D.74; Meinhold, P. R.26; Mennella, A.32,45; Migliaccio, M.3,49; Millea, M.25,53,87; Miville-Deschenes, M. -A.8,52; Molinari, D.30,44,48; Moneti, A.53; Montier, L.9,91; Morgante, G.44; Moss, A.83; Narimani, A.19; Natoli, P.3,30,48; Oxborrow, C. A.13; Pagano, L.52; Paoletti, D.44,47; Partridge, B.40; Patanchon, G.1; Patrizii, L.47; Pettorino, V.38,39; Piacentini, F.31; Polastri, L.30,48; Polenta, G.4; Puget, J. -L.52; Rachen, J. P.17; Racine, B.56; Reinecke, M.73; Remazeilles, M.1,52,61; Renzi, A.50,78; Rocha, G.10,60; Rossetti, M.32,45; Roudier, G.1,60,65; Rubino-Martin, J. A.15,57; Ruiz-Granados, B.92; Salvati, L.52; Sandri, M.44; Savelainen, M.22,41,72; Scott, D.19; Sirignano, C.28,59; Sirri, G.47; Stanco, L.59; Suur-Uski, A. -S.22,41; Tauber, J. A.36; Tavagnacco, D.33,43; Tenti, M.46; Toffolati, L.16,44,58; Tomasi, M.32,45; Tristram, M.64; Trombetti, T.30,44,47; Valiviita, J.22,41; Van Tent, F.69,70; Vielva, P.58; Villa, F.44; Vittorio, N.34; Wandelt, B. D.27,53,90; Wehus, I. K.56,60; White, M.24; Zacchei, A.43; Zonca, A.79
Corresponding AuthorGalli, S.( ; Millea, M.(
AbstractThe six parameters of the standard Lambda CDM 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 tau, the baryon density omega(b), the matter density omega(m), the angular size of the sound horizon theta(*), the spectral index of the primordial power spectrum, n(s), and A(s)e(-2 pi) (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 < 2500 Planck temperature power spectrum), each with a prior on tau of 0.07 +/- 0.02. We find that the shifts, in units of the 1 sigma expected dispersion for each parameter, are {Delta tau, Delta A(s)e(-2 tau), Delta n(s), Delta omega(m), Delta omega(b), Delta theta(*)} = {-1.7, -2.2, 1.2, 2.0, 1.1, 0.9}, with a chi(2) value of 8.0. We find that this chi(2) value is exceeded in 15% of our simulated data sets, and that a parameter deviates by more than 2.2 sigma 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 Lambda CDM 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 tau, which, at fixed A(s)e(-2 tau), 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 2 sigma 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 omega(m) and H-0. 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 Planck TT 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 Lambda CDM model.
Keywordcosmology: observations cosmic background radiation cosmological parameters cosmology: theory
Indexed BySCI
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS IDWOS:000415859600004
Citation statistics
Cited Times:35[WOS]   [WOS Record]     [Related Records in WOS]
Document Type期刊论文
Corresponding AuthorGalli, S.; Millea, M.
Affiliation1.Univ Paris Diderot, CNRS IN2P3, APC Astroparticule & Cosmol, CEA lrfu Observ Paris,Sorbonne Paris Cite, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France
2.African Inst Math Sci, 6-8 Melrose Rd, ZA-7945 Cape Town, South Africa
3.Agenzia Spaziale Italiana Sci Data Ctr, Via Politecn Snc, I-00133 Rome, Italy
4.Agenzia Spaziale Italiana, Via Politecn Snc, I-00133 Rome, Italy
5.Aix Marseille Univ, CNRS, LAM, F-13013 Marseille, France
6.Univ Cambridge, Cavendish Lab, Astrophys Grp, J J Thomson Ave, Cambridge CB3 0HE, England
7.Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, Westville Campus,Private Bag X54001, ZA-4000 Durban, South Africa
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10.CALTECH, Pasadena, CA 91125 USA
11.Univ Cambridge, Ctr Theoret Cosmol, DAMTP, Wilberforce Rd, Cambridge CB3 0WA, England
12.Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA
13.Tech Univ Denmark, Natl Space Inst, DTU Space, Elektrovej 327, DK-2800 Lyngby, Denmark
14.Univ Geneva, Dept Phys Theor, 24 Quai E Ansermet, CH-1211 Geneva 4, Switzerland
15.Univ La Laguna, Dept Astrofis, Tenerife 38206, Spain
16.Univ Oviedo, Dept Fis, Avda Calvo Sotelo S-N, Oviedo 33007, Spain
17.Radboud Univ Nijmegen, Dept Astrophys, IMAPP, POB 9010, NL-6500 GL Nijmegen, Netherlands
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36.European Space Agcy, Estec, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands
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38.HGSFP, Philosophenweg 16, D-69120 Heidelberg, Germany
39.Heidelberg Univ, Theoret Phys Dept, Philosophenweg 16, D-69120 Heidelberg, Germany
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71.Lawrence Berkeley Natl Lab, Berkeley, CA USA
72.Aalto Univ, Dept Appl Phys, Low Temp Lab, Espoo 00076, Finland
73.Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany
74.Univ Coll London, Mullard Space Sci Lab, Surrey RH5 6NT, England
75.Polish Acad Sci, Nicolaus Copernicus Astron Ctr, Bartycka 18, PL-00716 Warsaw, Poland
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87.Sorbonne Univ, Inst Lagrange Paris, 98bis Blvd Arago, F-75014 Paris, France
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93.Univ Warsaw Observ, Aleje Ujazdowskie 4, PL-00478 Warsaw, Poland
Recommended Citation
GB/T 7714
Aghanim, N.,Akrami, Y.,Ashdown, M.,et al. Planck intermediate results LI. Features in the cosmic microwave background temperature power spectrum and shifts in cosmological parameters[J]. ASTRONOMY & ASTROPHYSICS,2017,607:27.
APA Aghanim, N..,Akrami, Y..,Ashdown, M..,Aumont, J..,Baccigalupi, C..,...&Zonca, A..(2017).Planck intermediate results LI. Features in the cosmic microwave background temperature power spectrum and shifts in cosmological parameters.ASTRONOMY & ASTROPHYSICS,607,27.
MLA Aghanim, N.,et al."Planck intermediate results LI. Features in the cosmic microwave background temperature power spectrum and shifts in cosmological parameters".ASTRONOMY & ASTROPHYSICS 607(2017):27.
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