Data di Pubblicazione:
2014
Abstract:
We explore the 2013 Planck likelihood function with a high-precision
multi-dimensional minimizer (Minuit). This allows a refinement of the
LambdaCDM 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 ∑ mnu <= 0.26 eV (95%
confidence) from the CMB+lensing+BAO data combination.
multi-dimensional minimizer (Minuit). This allows a refinement of the
LambdaCDM 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 ∑ mnu <= 0.26 eV (95%
confidence) from the CMB+lensing+BAO data combination.
Tipologia CRIS:
1.1 Articolo in rivista
Keywords:
cosmic background radiation; cosmology: observations; cosmology: theory; cosmological parameters; methods: statistical
Elenco autori:
P., Collaboration; P. A., R.; N., Aghanim; M., Arnaud; M., Ashdown; J., Aumont; C., Baccigalupi; A. J., Banday; R. B., Barreiro; J. G., Bartlett; E., Battaner; K., Benabed; A., Benoit L�vy; J., Bernard; M., Bersanelli; P., Bielewicz; J., Bobin; A., Bonaldi; J. R., Bond; F. R., Bouchet; C., Burigana; J., Cardoso; A., Catalano; A., Chamballu; H. C., Chiang; P. R., Christensen; D. L., Clements; S., Colombi; L. P., L.; F., Couchot; F., Cuttaia; L., Danese; R. D., Davies; R. J., Davis; P. d., Bernardis; A. d., Rosa; G. d., Zotti; J., Delabrouille; C., Dickinson; J. M., Diego; H., Dole; S., Donzelli; O., Dor�; M., Douspis; X., Dupac; T. A., En�lin; H. K., Eriksen; F., Finelli; O., Forni; M., Frailis; E., Franceschi; S., Galeotta; S., Galli; K., Ganga; M., Giard; Y., Giraud H�raud; J., Gonz�lez Nuevo; K. M., G�rski; A., Gregorio; A., Gruppuso; F. K., Hansen; D. L., Harrison; S., Henrot Versill�; C., Hern�ndez Monteagudo; D., Herranz; S. R., Hildebrandt; E., Hivon; M., Hobson; W. A., Holmes; A., Hornstrup; W., Hovest; K. M., Huffenberger; A. H., Jaffe; T. R., Jaffe; W. C., Jones; M., Juvela; E., Keih�nen; R., Keskitalo; T. S., Kisner; R., Kneissl; J., Knoche; L., Knox; M., Kunz; H., Kurki Suonio; G., Lagache; A., L�hteenm�ki; J., Lamarre; A., Lasenby; C. R., Lawrence; R., Leonardi; A., Liddle; M., Liguori; P. B., Lilje; M., Linden V�rnle; M., L�pez Caniego; P. M., Lubin; J. F., Mac�as P�rez; B., Maffei; D., Maino; N., Mandolesi; M., Maris; P. G., Martin; E., Mart�nez Gonz�lez; S., Masi; M., Massardi; S., Matarrese; P., Mazzotta; A., Melchiorri; L., Mendes; A., Mennella; M., Migliaccio; S., Mitra; M., Miville Desch�nes; A., Moneti; L., Montier; G., Morgante; D., Munshi; J. A., Murphy; P., Naselsky; F., Nati; P., Natoli; F., Noviello; D., Novikov; I., Novikov; C. A., Oxborrow; L., Pagano; F., Pajot; D., Paoletti; F., Pasian; O., Perdereau; L., Perotto; F., Perrotta; V., Pettorino; F., Piacentini; M., Piat; E., Pierpaoli; D., Pietrobon; S., Plaszczynski*; E., Pointecouteau; G., Polenta; L., Popa; G. W., Pratt; J., Puget; J. P., Rachen; R., Rebolo; M., Reinecke; M., Remazeilles; C., Renault; S., Ricciardi; T., Riller; I., Ristorcelli; G., Rocha; C., Rosset; G., Roudier; B. R., D'Orfeuil; Mart�n, J. A. Rubi�o.; B., Rusholme; M., Sandri; M., Savelainen; G., Savini; L. D., Spencer; M., Spinelli; J., Starck; F., Sureau; D., Sutton; A., Suur Uski; J., Sygnet; J. A., Tauber; Terenzi, Luca; L., Toffolatti; M., Tomasi; M., Tristram; M., Tucci; G., Umana; L., Valenziano; J., Valiviita; B. V., Tent; P., Vielva; F., Villa; L. A., Wade; B. D., Wandelt; M., White; D., Yvon; A., Zacchei; A., Zonca
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