Ade, P.A.R. and Aghanim, N. and Arnaud, M. and Ashdown, M. and Aumont, J. and Baccigalupi, C. and Banday, A.J. and Barreiro, R.B. and Bartlett, J.G. and Battaner, E. and Benabed, K. and Benoit-Lévy, A. and Bernard, J.-P. and Bersanelli, M. and Bielewicz, P. and Bobin, J. and Bonaldi, A. and Bond, J.R. and Bouchet, F.R. and Burigana, C. and Cardoso, J.-F. and Catalano, A. and Chamballu, A. and Chiang, H.C. and Christensen, P.R. and Clements, D.L. and Colombi, S. and Colombo, L.P.L. and Couchot, F. and Cuttaia, F. and Danese, L. and Davies, R.D. and Davis, R.J. and De Bernardis, P. and de Rosa, A. and de Zotti, G. and Delabrouille, J. and Dickinson, C. and Diego, J.M. and Dole, H. and Donzelli, S. and Dore, O. and Douspis, M. and Dupac, X. and Enßlin, T.A. and Eriksen, H.K. and Finelli, F. and Forni, O. and Frailis, M. and Franceschi, E. and Galeotta, S. and Galli, S. and Ganga, K. and Giard, M. and Giraud-Héraud, Y. and Gonzalez-Nuevo, J. and Gorski, K.M. and Gregorio, A. and Gruppuso, A. and Hansen, F.K. and Harrison, D. and Henrot-Versille, S. and Hernandez-Monteagudo, C. and Herranz, D. and Hildebrandt, S.R. and Hivon, E. and Hobson, M. and Holmes, W.A. and Hornstrup, A. and Hovest, W. and Huffenberger, K.M. and Jaffe, A.H. and Jaffe, T.R. and Jones, W.C. and Juvela, M. and Keihanen, E. and Keskitalo, R. and Kisner, T.S. and Kneissl, R. and Knoche, J. and Knox, L. and Kunz, M. and Kurki-Suonio, H. and Lagache, G. and Lahteenmaki, A. and Lamarre, J.-M. and Lasenby, A. and Lawrence, C.R. and Leonardi, R. and Liddle, A. and Liguori, M. and Lilje, P.B. and Linden-Vornle, M. and Lopez-Caniego, M. and Lubin, P.M. and Macias-Perez, J.F. and Maffei, B. and Maino, D. and Mandolesi, N. and Maris, M. and Martin, P.G. and Martinez-Gonzalez, E. and Masi, S. and Massardi, M. and Matarrese, S. and Mazzotta, P. and Melchiorri, A. and Mendes, L. and Mennella, A. and Migliaccio, M. and Mitra, S. and Miville-Deschenes, M.-A. and Moneti, A. and Montier, L. and Morgante, G. and Munshi, D. and Murphy, J.Anthony and Naselsky, P. and Nati, F. and Natoli, P. and Noviello, F. and Novikov, D. and Novikov, I. and Oxborrow, C.A. and Pagano, L. and Pajot, F. and Paoletti, D. and Pasian, F. and Perdereau, O. and Perotto, L. and Perrotta, F. and Pettorino, V. and Piacentini, F. and Piat, M. and Pierpaoli, E. and Pietrobon, D. and Plaszczynski, S. and Pointecouteau, E. and Polenta, G. and Popa, L. and Pratt, G.W. and Puget, J.-L. and Rachen, J.P. and Rebolo, R. and Reinecke, M. and Remazeilles, M. and Renault, C. and Ricciardi, S. and Riller, T. and Ristorcelli, I. and Rocha, G. and Rosset, C. and Roudier, G. and Rouillé d’Orfeuil, B. and Rubino-Martin, J.A. and Rusholme, B. and Sandri, M. and Savelainen, M. and Savini, G. and Spencer, L. and Spinelli, S. and Starck, J.-L. and Sureau, F. and Sutton, D. and Suur-Uski, A.-S. and Sygnet, J.-F. and Tauber, J.A. and Terenzi, L. and Toffolatti, L. and Tomasi, M. and Tristram, M. and Tucci, M. and Umana, G. and Valenziano, L. and Valiviita, J. and Van Tent, B. and Vielva, P. and Villa, F. and Wade, L.A. and Wandelt, B.D. and White, M. and Yvon, D. and Zacchei, A. and Zonca, A. (2014) Planck intermediate results XVI. Profile likelihoods for cosmological parameters. Astronomy & Astrophysics, 566 (A54). ISSN 0004-6361

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Abstract

We explore the 2013 Planck likelihood function with a high-precision multi-dimensional minimizer (Minuit). This allows a refinement of the ΛCDM best-fit solution with respect to previously-released results, and the construction of frequentist confidence intervals using profile likelihoods. The agreement with the cosmological results from the Bayesian framework is excellent, demonstrating the robustness of the Planck results to the statistical methodology. We investigate the inclusion of neutrino masses, where more significant differences may appear due to the non-Gaussian nature of the posterior mass distribution. By applying the Feldman-Cousins prescription, we again obtain results very similar to those of the Bayesian methodology. However, the profile-likelihood analysis of the cosmic microwave background (CMB) combination (Planck+WP+highL) reveals a minimum well within the unphysical negative-mass region. We show that inclusion of the Planck CMB-lensing information regularizes this issue, and provide a robust frequentist upper limit ∑ mν ≤ 0.26 eV (95% confidence) from the CMB+lensing+BAO data combination.

Item Type:	Article
Keywords:	Planck Collaboration; cosmic background radiation; cosmology: observations; cosmology: theory; cosmological parameters; methods: statistical;
Academic Unit:	Faculty of Science and Engineering > Experimental Physics
Item ID:	14166
Identification Number:	https://doi.org/10.1051/0004-6361/201323003
Depositing User:	Dr. Anthony Murphy
Date Deposited:	11 Mar 2021 15:11
Journal or Publication Title:	Astronomy & Astrophysics
Publisher:	EDP Sciences
Refereed:	Yes
URI:	Publisher
Use Licence:	This item is available under a Creative Commons Attribution Non Commercial Share Alike Licence (CC BY-NC-SA). Details of this licence are available here

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