A. A. Fraisse, A. Challinor, A. Ducout, A. Frolov, A. Gruppuso, A. H. Jaffe, A. J. Banday, A. Karakci, A. Lasenby, A. Lewis, A. Mangilli, A. Marcos-Caballero, A. Melchiorri, A. Mennella, A. Moss, A. Renzi, A.-S. Suur-Uski, A. Zacchei, A. Zonca, B. D. Wandelt, B. Partridge, B. P. Crill, B. Ruiz-Granados, B. Van Tent, C. Baccigalupi, C. Burigana, C. Combet, C. R. Lawrence, C. Rosset, C. Sirignano, D. Contreras, D. Herranz, D. Maino, D. Molinari, D. Paoletti, D. Scott, D. Tavagnacco, E. Calabrese, E. Di Valentino, E. Franceschi, E. Hivon, E. Keih\"anen, E. Mart\'inez-Gonz\'alez, E. P. S. Shellard, F. Boulanger, F. Cuttaia, F. Elsner, F. Finelli, F. Forastieri, F. K. Hansen, F. Levrier, F. Perrotta, F. Piacentini, F. R. Bouchet, F. Villa, G. de Zotti, G. Efstathiou, G. Lagache, G. Maggio, G. Morgante, G. Patanchon, G. Polenta, G. Rocha, G. Roudier, G. Sirri, H. C. Chiang, H. K. Eriksen, H. Kurki-Suonio, H. U. N{\o}rgaard-Nielsen, H. V. Peiris, I. K. Wehus, J. A. Rubi\~no-Mart\'in, J. A. Tauber, J. Aumont, J. Borrill, J. Carron, J. Chluba, J. Delabrouille, J. D. McEwen, J. E. Gudmundsson, J.-F. Cardoso, J. Fergusson, J. F. Mac\'ias-P\'erez, J. Gonz\'alez-Nuevo, J. Hamann, J. J. Bock, J. Kim, J. Lesgourgues, J.-L. Puget, J.-M. Delouis, J. M. Diego, J.-M. Lamarre, J.-P. Bernard, J. P. Rachen, J. R. Bond, J. Valiviita, K. Benabed, K. Ganga, K. Kiiveri, K. M. G\'orski, L. D. Spencer, L. Knox, L. Montier, L. Pagano, L. P. L. Colombo, L. Polastri, L. Salvati, L. Toffolatti, L. Valenziano, L. Vibert, M.-A. Miville-Desch\^enes, M. Ashdown, M. Ballardini, M. Bersanelli, M. Bucher, M. Douspis, M. Farhang, M. Frailis, M. Gerbino, M. Kunz, M. Lattanzi, M. Le Jeune, M. Liguori, M. Lilley, M. L\'opez-Caniego, M. Maris, M. Martinelli, M. Migliaccio, M. Millea, M. Reinecke, M. Remazeilles, M. Sandri, M. Savelainen, M. Tenti, M. Tomasi, M. White, N. Bartolo, N. Krachmalnicoff, N. Mandolesi, N. Mauri, N. Vittorio, O. Dor\'e, P. Bielewicz, P. B. Lilje, P. De Bernardis, P. G. Martin, Planck Collaboration: N. Aghanim, P. Lemos, P. M. Lubin, P. Natoli, P. R. Meinhold, P. Vielva, R. Battye, R. B. Barreiro, R. C. Butler, R. Fernandez-Cobos, R. Keskitalo, R. Sunyaev, R. T. G\'enova-Santos, S. Basak, S. D. M. White, S. Dusini, S. Galeotta, S. Galli, S. Gratton, S. Matarrese, S. Mitra, S. R. Hildebrandt, T. A. En{\ss}lin, T. Ghosh, T. S. Kisner, T. Trombetti, V. Lindholm, V. Pettorino, W. C. Jones, W. Handley, X. Dupac, Y. Akrami, Y. Fantaye, Y.-Z. Ma, Z. Huang
Planck's final CMB measurements fix the standard flat six-parameter Lambda CDM parameters to high precision and find no compelling evidence for extensions.
The bundle contains the canonical record plus signed events. A mirror can host it anywhere and recompute the same
current state with the deterministic merge algorithm.
Claims
C1strongest claim
A combined analysis gives dark matter density Ω_c h² = 0.120±0.001, baryon density Ω_b h² = 0.0224±0.0001, scalar spectral index n_s = 0.965±0.004, and optical depth τ = 0.054±0.007. We find no compelling evidence for extensions to the base-ΛCDM model.
C2weakest assumption
The analysis assumes that the observed CMB power spectra are generated by the base spatially-flat 6-parameter ΛCDM model plus standard foregrounds, with no large unmodeled systematics or new physics that would alter the likelihood surface.
C3one line summary
Final Planck CMB data confirms the flat 6-parameter ΛCDM model with Ω_c h² = 0.120 ± 0.001, Ω_b h² = 0.0224 ± 0.0001, n_s = 0.965 ± 0.004, τ = 0.054 ± 0.007, H_0 = 67.4 ± 0.5 km/s/Mpc, and no strong evidence for extensions.
References
299 extracted · 299 resolved · 63 Pith anchors
[1] Astrophysical and Dark Matter Interpretations of Extended Gamma-Ray Emission from the Galactic Center
2014
· arXiv:1402.4090
[2] GW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral
2017
· arXiv:1710.05832
[3] A gravitational-wave standard siren measurement of the Hubble constant
2017
· arXiv:1710.05835
[4] Atmospheric neutrino oscillation analysis with external constraints in Super-Kamiokande I-IV
2018
· arXiv:1710.09126
[5] Constraints on Oscillation Parameters from $\nu_e$ Appearance and $\nu_\mu$ Disappearance in NOvA
2017
· arXiv:1703.03328