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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

We explore the 2013 Planck likelihood function with a high-precision multi-dimensional minimizer (Minuit). This allows a refinement of the ACDM 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 Sigma m(v) <= 0.26 eV (95% confidence) from the CMB+lensing+BAO data combination.

Planck intermediate results: XVI. Profile likelihoods for cosmological parameters / Planck, Collaboration; P. A. R., Ade; 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 Levy; J. P., Bernard; M., Bersanelli; P., Bielewicz; J., Bobin; A., Bonaldi; J. R., Bond; F. R., Bouchet; C., Burigana; J. F., Cardoso; Catalano, Andrea; A., Chamballu; H. C., Chiang; P. R., Christensen; D. L., Clements; S., Colombi; L. P. L., Colombo; F., Couchot; F., Cuttaia; L., Danese; R. D., Davies; R. J., Davis; DE BERNARDIS, Paolo; A., De Rosa; G., De Zotti; J., Delabrouille; C., Dickinson; J. M., Diego; H., Dole; S., Donzelli; O., Dore; M., Douspis; X., Dupac; T. A., Ensslin; H. K., Eriksen; F., Finelli; O., Forni; M., Frailis; E., Franceschi; S., Galeotta; Silvia, Galli; K., Ganga; M., Giard; Y., Giraud Heraud; J., Gonzalez Nuevo; K. M., Gorski; A., Gregorio; A., Gruppuso; F. K., Hansen; D. L., Harrison; S., Henrot Versille; C., Hernandez 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., Keihanen; R., Keskitalo; T. S., Kisner; R., Kneissl; J., Knoche; L., Knox; M., Kunz; H., Kurki Suonio; G., Lagache; A., Lahteenmaki; J. M., Lamarre; A., Lasenby; C. R., Lawrence; R., Leonardi; A., Liddle; M., Liguori; P. B., Lilje; M., Linden Vornle; M., Linden Vørnle; M., Lopez Caniego; P. M., Lubin; J. F., Macias Perez; B., Maffei; D., Maino; N., Mandolesi; M., Maris; P. G., Martin; E., Martinez Gonzalez; Masi, Silvia; M., Massardi; S., Matarrese; P., Mazzotta; Melchiorri, Alessandro; L., Mendes; A., Mennella; M., Migliaccio; S., Mitra; M. A., Miville Deschenes; A., Moneti; L., Montier; G., Morgante; D., Munshi; J. A., Murphy; P., Naselsky; Nati, Federico; P., Natoli; F., Noviello; D., Novikov; I., Novikov; C. A., Oxborrow; Pagano, Luca; F., Pajot; D., Paoletti; F., Pasian; O., Perdereau; L., Perotto; F., Perrotta; V., Pettorino; Piacentini, Francesco; M., Piat; E., Pierpaoli; D., Pietrobon; S., Plaszczynski; E., Pointecouteau; Polenta, Gianluca; L., Popa; G. W., Pratt; J. L., Puget; J. P., Rachen; R., Rebolo; M., Reinecke; M., Remazeilles; C., Renault; Ricciardi, Sara; T., Riller; I., Ristorcelli; G., Rocha; C., Rosset; G., Roudier; B. R., D'Orfeuil; B., Rouille D'Orfeuil; J. A., Rubino Martin; B., Rusholme; M., Sandri; M., Savelainen; Savini, Giorgio; L. D., Spencer; M., Spinelli; J. L., Starck; F., Sureau; D., Sutton; A. S., Suur Uski; J. F., Sygnet; J. A., Tauber; L., Terenzi; L., Toffolatti; M., Tomasi; M., Tristram; M., Tucci; G., Umana; L., Valenziano; J., Valiviita; B., Van Tent; P., Vielva; F., Villa; L. A., Wade; B. D., Wandelt; M., White; D., Yvon; A., Zacchei; A., Zonca. - In: ASTRONOMY & ASTROPHYSICS. - ISSN 0004-6361. - STAMPA. - 566:(2014), p. A54. [10.1051/0004-6361/201323003]

Planck intermediate results: XVI. Profile likelihoods for cosmological parameters

CATALANO, Andrea;DE BERNARDIS, Paolo;MASI, Silvia;MELCHIORRI, Alessandro;NATI, FEDERICO;PAGANO, LUCA;PIACENTINI, Francesco;POLENTA, GIANLUCA;RICCIARDI, Sara;SAVINI, Giorgio;
2014

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
2014
We explore the 2013 Planck likelihood function with a high-precision multi-dimensional minimizer (Minuit). This allows a refinement of the ACDM 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 Sigma m(v) <= 0.26 eV (95% confidence) from the CMB+lensing+BAO data combination.
cosmology: theory; cosmology: observations; cosmic background radiation; cosmological parameters; methods: statistical
01 Pubblicazione su rivista::01a Articolo in rivista
Planck intermediate results: XVI. Profile likelihoods for cosmological parameters / Planck, Collaboration; P. A. R., Ade; 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 Levy; J. P., Bernard; M., Bersanelli; P., Bielewicz; J., Bobin; A., Bonaldi; J. R., Bond; F. R., Bouchet; C., Burigana; J. F., Cardoso; Catalano, Andrea; A., Chamballu; H. C., Chiang; P. R., Christensen; D. L., Clements; S., Colombi; L. P. L., Colombo; F., Couchot; F., Cuttaia; L., Danese; R. D., Davies; R. J., Davis; DE BERNARDIS, Paolo; A., De Rosa; G., De Zotti; J., Delabrouille; C., Dickinson; J. M., Diego; H., Dole; S., Donzelli; O., Dore; M., Douspis; X., Dupac; T. A., Ensslin; H. K., Eriksen; F., Finelli; O., Forni; M., Frailis; E., Franceschi; S., Galeotta; Silvia, Galli; K., Ganga; M., Giard; Y., Giraud Heraud; J., Gonzalez Nuevo; K. M., Gorski; A., Gregorio; A., Gruppuso; F. K., Hansen; D. L., Harrison; S., Henrot Versille; C., Hernandez 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., Keihanen; R., Keskitalo; T. S., Kisner; R., Kneissl; J., Knoche; L., Knox; M., Kunz; H., Kurki Suonio; G., Lagache; A., Lahteenmaki; J. M., Lamarre; A., Lasenby; C. R., Lawrence; R., Leonardi; A., Liddle; M., Liguori; P. B., Lilje; M., Linden Vornle; M., Linden Vørnle; M., Lopez Caniego; P. M., Lubin; J. F., Macias Perez; B., Maffei; D., Maino; N., Mandolesi; M., Maris; P. G., Martin; E., Martinez Gonzalez; Masi, Silvia; M., Massardi; S., Matarrese; P., Mazzotta; Melchiorri, Alessandro; L., Mendes; A., Mennella; M., Migliaccio; S., Mitra; M. A., Miville Deschenes; A., Moneti; L., Montier; G., Morgante; D., Munshi; J. A., Murphy; P., Naselsky; Nati, Federico; P., Natoli; F., Noviello; D., Novikov; I., Novikov; C. A., Oxborrow; Pagano, Luca; F., Pajot; D., Paoletti; F., Pasian; O., Perdereau; L., Perotto; F., Perrotta; V., Pettorino; Piacentini, Francesco; M., Piat; E., Pierpaoli; D., Pietrobon; S., Plaszczynski; E., Pointecouteau; Polenta, Gianluca; L., Popa; G. W., Pratt; J. L., Puget; J. P., Rachen; R., Rebolo; M., Reinecke; M., Remazeilles; C., Renault; Ricciardi, Sara; T., Riller; I., Ristorcelli; G., Rocha; C., Rosset; G., Roudier; B. R., D'Orfeuil; B., Rouille D'Orfeuil; J. A., Rubino Martin; B., Rusholme; M., Sandri; M., Savelainen; Savini, Giorgio; L. D., Spencer; M., Spinelli; J. L., Starck; F., Sureau; D., Sutton; A. S., Suur Uski; J. F., Sygnet; J. A., Tauber; L., Terenzi; L., Toffolatti; M., Tomasi; M., Tristram; M., Tucci; G., Umana; L., Valenziano; J., Valiviita; B., Van Tent; P., Vielva; F., Villa; L. A., Wade; B. D., Wandelt; M., White; D., Yvon; A., Zacchei; A., Zonca. - In: ASTRONOMY & ASTROPHYSICS. - ISSN 0004-6361. - STAMPA. - 566:(2014), p. A54. [10.1051/0004-6361/201323003]
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11573/587786
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