Data di Pubblicazione:
2016
Abstract:
The Planck full mission cosmic microwave background (CMB) temperature and E-mode polarization maps are analysed to obtain constraints on
primordial non-Gaussianity (NG). Using three classes of optimal bispectrum estimators – separable template-fitting (KSW), binned, and modal –
we obtain consistent values for the primordial local, equilateral, and orthogonal bispectrum amplitudes, quoting as our final result from temperature
alone f local = 2.5 ± 5.7, f equil = −16 ± 70, and f ortho = −34 ± 33 (68% CL, statistical). Combining temperature and polarization data we obtain NL NL NL
f local = 0.8 ± 5.0, f equil = −4 ± 43, and f ortho = −26 ± 21 (68% CL, statistical). The results are based on comprehensive cross-validation NL NL NL
of these estimators on Gaussian and non-Gaussian simulations, are stable across component separation techniques, pass an extensive suite of
tests, and are consistent with estimators based on measuring the Minkowski functionals of the CMB. The effect of time-domain de-glitching
systematics on the bispectrum is negligible. In spite of these test outcomes we conservatively label the results including polarization data as
preliminary, owing to a known mismatch of the noise model in simulations and the data. Beyond estimates of individual shape amplitudes, we
present model-independent, three-dimensional reconstructions of the Planck CMB bispectrum and derive constraints on early universe scenarios
that generate primordial NG, including general single-field models of inflation, axion inflation, initial state modifications, models producing parity-
violating tensor bispectra, and directionally dependent vector models. We present a wide survey of scale-dependent feature and resonance models,
accounting for the “look elsewhere” effect in estimating the statistical significance of features. We also look for isocurvature NG, and find no
signal, but we obtain constraints that improve significantly with the inclusion of polarization. The primordial trispectrum amplitude in the local
model is constrained to be glocal = (−9.0 ± 7.7) × 104 (68% CL statistical), and we perform an analysis of trispectrum shapes beyond the local case. NL
The global picture that emerges is one of consistency with the premises of the ΛCDM cosmology, namely that the structure we observe today was sourced by adiabatic, passive, Gaussian, and primordial seed perturbations.
primordial non-Gaussianity (NG). Using three classes of optimal bispectrum estimators – separable template-fitting (KSW), binned, and modal –
we obtain consistent values for the primordial local, equilateral, and orthogonal bispectrum amplitudes, quoting as our final result from temperature
alone f local = 2.5 ± 5.7, f equil = −16 ± 70, and f ortho = −34 ± 33 (68% CL, statistical). Combining temperature and polarization data we obtain NL NL NL
f local = 0.8 ± 5.0, f equil = −4 ± 43, and f ortho = −26 ± 21 (68% CL, statistical). The results are based on comprehensive cross-validation NL NL NL
of these estimators on Gaussian and non-Gaussian simulations, are stable across component separation techniques, pass an extensive suite of
tests, and are consistent with estimators based on measuring the Minkowski functionals of the CMB. The effect of time-domain de-glitching
systematics on the bispectrum is negligible. In spite of these test outcomes we conservatively label the results including polarization data as
preliminary, owing to a known mismatch of the noise model in simulations and the data. Beyond estimates of individual shape amplitudes, we
present model-independent, three-dimensional reconstructions of the Planck CMB bispectrum and derive constraints on early universe scenarios
that generate primordial NG, including general single-field models of inflation, axion inflation, initial state modifications, models producing parity-
violating tensor bispectra, and directionally dependent vector models. We present a wide survey of scale-dependent feature and resonance models,
accounting for the “look elsewhere” effect in estimating the statistical significance of features. We also look for isocurvature NG, and find no
signal, but we obtain constraints that improve significantly with the inclusion of polarization. The primordial trispectrum amplitude in the local
model is constrained to be glocal = (−9.0 ± 7.7) × 104 (68% CL statistical), and we perform an analysis of trispectrum shapes beyond the local case. NL
The global picture that emerges is one of consistency with the premises of the ΛCDM cosmology, namely that the structure we observe today was sourced by adiabatic, passive, Gaussian, and primordial seed perturbations.
Tipologia CRIS:
01.01 - Articolo in rivista
Keywords:
Cosmic background radiation; Cosmology: observations; Cosmology: theory; Early Universe; Inflation; Methods: data analysis; Astronomy and Astrophysics; Space and Planetary Science
Elenco autori:
Ade, P. A. R.; Aghanim, N.; Arnaud, M.; Arroja, F.; Ashdown, M.; Aumont, J.; Baccigalupi, C.; Ballardini, M.; Banday, A. J.; Barreiro, R. B.; Bartolo, Nicola; Basak, S.; Battaner, E.; Benabed, K.; Benoît, A.; Benoit Lévy, A.; Bernard, J. P.; Bersanelli, M.; Bielewicz, P.; Bock, J. J.; Bonaldi, A.; Bonavera, L.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Boulanger, F.; Bucher, M.; Burigana, C.; Butler, R. C.; Calabrese, E.; Cardoso, J. F.; Catalano, A.; Challinor, A.; Chamballu, A.; Chiang, H. C.; Christensen, P. R.; Church, S.; Clements, D. L.; Colombi, S.; Colombo, L. P. L.; Combet, C.; Couchot, F.; Coulais, A.; Crill, B. P.; Curto, A.; Cuttaia, F.; Danese, L.; Davies, R. D.; Davis, R. J.; De Bernardis, P.; De Rosa, A.; De Zotti, G.; Delabrouille, J.; Désert, F. X.; Diego, J. M.; Dole, H.; Donzelli, S.; Doré, O.; Douspis, M.; Ducout, A.; Dupac, X.; Efstathiou, G.; Elsner, F.; Enßlin, T. A.; Eriksen, H. K.; Fergusson, J.; Finelli, F.; Forni, O.; Frailis, M.; Fraisse, A. A.; Franceschi, E.; Frejsel, A.; Galeotta, S.; Galli, S.; Ganga, K.; Gauthier, C.; Ghosh, T.; Giard, M.; Giraud Héraud, Y.; Gjerløw, E.; González Nuevo, J.; Górski, K. M.; Gratton, S.; Gregorio, A.; Gruppuso, A.; Gudmundsson, J. E.; Hamann, J.; Hansen, F. K.; Hanson, D.; Harrison, D. L.; Heavens, A.; Helou, G.; Henrot Versillé, S.; Hernández Monteagudo, C.; Herranz, D.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.; Hornstrup, A.; Hovest, W.; Huang, Z.; Huffenberger, K. M.; Hurier, G.; Jaffe, A. H.; Jaffe, T. R.; Jones, W. C.; Juvela, M.; Keihänen, E.; Keskitalo, R.; Kim, J.; Kisner, T. S.; Knoche, J.; Kunz, M.; Kurki Suonio, H.; Lacasa, F.; Lagache, G.; Lähteenmäki, A.; Lamarre, J. M.; Lasenby, A.; Lattanzi, M.; Lawrence, C. R.; Leonardi, R.; Lesgourgues, J.; Levrier, F.; Lewis, A.; Liguori, Michele; Lilje, P. B.; Linden Vørnle, M.; López Caniego, M.; Lubin, P. M.; Maciás Pérez, J. F.; Maggio, G.; Maino, D.; Mandolesi, N.; Mangilli, A.; Marinucci, D.; Maris, M.; Martin, P. G.; Martínez González, E.; Masi, S.; Matarrese, Sabino; Mcgehee, P.; Meinhold, P. R.; Melchiorri, A.; Mendes, L.; Mennella, A.; Migliaccio, M.; Mitra, S.; Miville Deschênes, M. A.; Moneti, A.; Montier, L.; Morgante, G.; Mortlock, D.; Moss, A.; Münchmeyer, M.; Munshi, D.; Murphy, J. A.; Naselsky, P.; Nati, F.; Natoli, P.; Netterfield, C. B.; Nørgaard Nielsen, H. U.; Noviello, F.; Novikov, D.; Novikov, I.; Oxborrow, C. A.; Paci, F.; Pagano, L.; Pajot, F.; Paoletti, D.; Pasian, F.; Patanchon, G.; Peiris, H. V.; Perdereau, O.; Perotto, L.; Perrotta, F.; Pettorino, V.; Piacentini, F.; Piat, M.; Pierpaoli, E.; Pietrobon, D.; Plaszczynski, S.; Pointecouteau, E.; Polenta, G.; Popa, L.; Pratt, G. W.; Prézeau, G.; Prunet, S.; Puget, J. L.; Rachen, J. P.; Racine, B.; Rebolo, R.; Reinecke, M.; Remazeilles, M.; Renault, C.; Renzi, A.; Ristorcelli, I.; Rocha, G.; Rosset, C.; Rossetti, M.; Roudier, G.; Rubinõ Martín, J. A.; Rusholme, B.; Sandri, M.; Santos, D.; Savelainen, M.; Savini, G.; Scott, D.; Seiffert, M. D.; Shellard, E. P. S.; Shiraishi, M.; Smith, K.; Spencer, L. D.; Stolyarov, V.; Stompor, R.; Sudiwala, R.; Sunyaev, R.; Sutter, P.; Sutton, D.; Suur Uski, A. S.; Sygnet, J. F.; Tauber, J. A.; Terenzi, L.; Toffolatti, L.; Tomasi, M.; Tristram, M.; Troja, A.; Tucci, M.; Tuovinen, J.; Valenziano, L.; Valiviita, J.; Van Tent, B.; Vielva, P.; Villa, F.; Wade, L. A.; Wandelt, B. D.; Wehus, I. K.; Yvon, D.; Zacchei, A.; Zonca, A.
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