A1 Vertaisarvioitu alkuperäisartikkeli tieteellisessä lehdessä
Planck 2013 results. XV. CMB power spectra and likelihood
Tekijät: Ade PAR, Aghanim N, Armitage-Caplan C, Arnaud M, Ashdown M, Atrio-Barandela F, Aumont J, Baccigalupi C, Banday AJ, Barreiro RB, Bartlett JG, Battaner E, Benabed K, Benoit A, Benoit-Levy A, Bemard JP, Bersanelli M, Bielewicz P, Bobin J, Bock JJ, Bonaldi A, Bonavera L, Bond JR, Borrill J, Bouchet FR, Boulanger F, Bridges M, Bucher M, Burigana C, Butler RC, Calabrese E, Cardoso JF, Catalano A, Challinor A, Chamballu A, Chiang HC, Chiang LY, Christensen PR, Church S, Clements DL, Colombi S, Colombo LPL, Combet C, Couchot F, Coulais A, Crill BP, Curto A, Cuttaia F, Danese L, Davies RD, Davis RJ, de Bemardis P, de Rosa A, de Zotti G, Delabrouille J, Delouis JM, Desert FX, Dickinson C, Diego JM, Dole H, Donzelli S, Dore O, Douspis M, Dunkley J, Dupac X, Efstathiou G, Elsner F, Ensslin TA, Eriksen HK, Finelli F, Forni O, Frailis M, Fraisse AA, Franceschi E, Gaier TC, Galeotta S, Galli S, Ganga K, Giard M, Giardino G, Giraud-Heraud Y, Gjerlow E, Gonzalez-Nuevo J, Gorski KM, Gratton S, Gregorio A, Gruppuso A, Gudmundsson JE, Hansen FK, Hanson D, Harrison D, Helou G, Henrot-Versille S, Hernandez-Monteagudo C, Herranz D, Hildebrandt SR, Hivon E, Hobson M, Holmes WA, Homtrup A, Hovest W, Huffenberger KM, Hurier G, Jaffe AH, Jaffe TR, Jewell J, Jones WC, Juvela M, Keihanen E, Kesldtalo R, Kiiveri K, Kisner TS, Krieiss R, Knoche J, Knox L, Kunz M, Kurki-Suonio H, Lagache G, Lahteenmaki A, Lamarre JM, Lasenby A, Lattanzi M, Laureijs RJ, Lawrence CR, Le Jeune M, Leach S, Leahy JP, Leonardi R, Leon-Tavares J, Lesgourgues J, Liguori M, Lilje PB, Linden-Vornle M, Lindholm V, Lopez-Caniego M, Lubin PM, Macias-Perez JF, Maffei B, Maino D, Mandolesi N, Marinucci D, Maris M, Marshall DJ, Martin PG, Martinez-Gonzalez E, Masi S, Massardi M, Matarrese S, Matthai F, Mazzotta P, Meinhold PR, Melchiorri A, Mendes L, Menegoni E, Mennella A, Migliaccio M, Millea M, Mitra S, Miville-Deschenes MA, Molinari D, Moneti A, Montier L, Morgante G, Mortlock D, Moss A, Munshi D, Murphy JA, Naselsky P, Nati F, Natoli P, Netterfield CB, Norgaard-Nielsen HU, Noviello F, Novikov D, Novikov I, O'Dwyer IJ, Orieux F, Osborne S, Oxborrow CA, Paci F, Pagano L, Pajot F, Paladini R, Paoletti D, Partridge B, Pasian F, Patanchon G, Paykari P, Perdereaun O, Perotto L, Perrotta F, Piacentini F, Piat M, Pierpaoli E, Pietrobon D, Plaszczynski S, Pointecouteau E, Polenta G, Ponthieu N, Popa L, Poutanen T, Pratt GW, Prezeau G, Prunet S, Puget JL, Rachen JP, Rahlin A, Rebolo R, Reinecke M, Remazeilles M, Renault C, Ricciardi S, Riller T, Ringeval C, Ristorcelli I, Rocha G, Rosset C, Roudier G, Rowan-Robinson M, Rubino-Martin JA, Rusholme B, Sandri M, Sanselme L, Santos D, Savini G, Scott D, Seiffert MD, Shellard EPS, Spencer LD, Starck JL, Stolyarov V, Stompor R, Sudiwala R, Sureau F, Sutton D, Suur-Uski AS, Sygnet JF, Tauber JA, Tavagnacco D, Terenzi L, Toffolatti L, Tomasi M, Tristram M, Tucci M, Tuovinen J, Turler M, Valenziano L, Valiviita J, Van Tent B, Varis J, Vielva P, Villa F, Vittorio N, Wade LA, Wandelt BD, Wehus IK, White M, White SDM, Yvon D, Zacchei A, Zonca A
Kustantaja: EDP SCIENCES S A
Julkaisuvuosi: 2014
Lehti: Astronomy and Astrophysics
Tietokannassa oleva lehden nimi: ASTRONOMY & ASTROPHYSICS
Lehden akronyymi: ASTRON ASTROPHYS
Artikkelin numero: ARTN A15
Vuosikerta: 571
Sivujen määrä: 60
ISSN: 0004-6361
DOI: https://doi.org/10.1051/0004-6361/201321573
This paper presents the Planck 2013 likelihood, a complete statistical description of the two-point correlation function of the CMB temperature fluctuations that accounts for all known relevant uncertainties, both instrumental and astrophysical in nature. We use this likelihood to derive our best estimate of the CMB angular power spectrum from Planck over three decades in multipole moment, t, covering 2 2500. The main source of uncertainty at S 1500 is cosmic variance. Uncertainties in small-scale foreground modelling and instrumental noise dominate the error budget at higher Es. For < 50, our likelihood exploits all Planck frequency channels from 30 to 353 GHz, separating the cosmological CMB signal from diffuse Galactic foregrounds through a physically motivated Bayesian component separation technique. At 50, we employ a correlated Gaussian likelihood approximation based on a fine-grained set of angular cross-spectra derived from multiple detector combinations between the 100, 143, and 217 GHz frequency channels, marginalising over power spectrum foreground templates. We validate our likelihood through an extensive suite of consistency tests, and assess the impact of residual foreground and instrumental uncertainties on the final cosmological parameters. We find good internal agreement among the high- cross-spectra with residuals below a few fiK2 at S 1000, in agreement with estimated calibration uncertainties. We compare our results with foreground-cleaned CMB maps derived from all Planck frequencies, as well as with cross-spectra derived from the 70 GHz Planck map, and find broad agreement in terms of spectrum residuals and cosmological parameters. We further show that the best-fit ACDM cosmology is in excellent agreement with preliminary Planck EE and T E polarisation spectra. We find that the standard ACDM cosmology is well constrained by Planck from the measurements at C 1500. One specific example is the spectral index of scalar perturbations, for which we report a 5.4o- deviation from scale invariance, ns = 1. Increasing the multipole range beyond = 1500 does not increase our accuracy for the ACDM parameters, but instead allows us to study extensions beyond the standard model. We find no indication of significant departures from the ACDM framework. Finally, we report a tension between the Planck best-fit ACDM model and the low- spectrum in the form of a power deficit of 5-10% at 40, with a statistical significance of 2.5-3o-. Without a theoretically motivated model for this power deficit, we do not elaborate further on its cosmological implications, but note that this is our most puzzling finding in an otherwise remarkably consistent data set.
