Planck 2018 results. VI. Cosmological parameters
Authors
Collaboration, Planck
Aghanim, N
Akrami, Y
Ashdown, Mark
Aumont, J
Baccigalupi, C
Ballardini, M
Banday, AJ
Barreiro, RB
Bartolo, N
Basak, S
Battye, R
Benabed, K
Bernard, J-P
Bersanelli, M
Bielewicz, P
Bock, JJ
Bond, JR
Borrill, J
Bouchet, FR
Boulanger, F
Bucher, M
Burigana, C
Butler, RC
Calabrese, E
Cardoso, J-F
Carron, J
Chiang, HC
Chluba, J
Colombo, LPL
Combet, C
Contreras, D
Crill, BP
Cuttaia, F
Bernardis, P de
Zotti, G de
Delabrouille, J
Delouis, J-M
Valentino, E Di
Diego, JM
Doré, O
Douspis, M
Ducout, A
Dupac, X
Dusini, S
Efstathiou, George
Elsner, F
Enßlin, TA
Eriksen, HK
Fantaye, Y
Farhang, M
Fernandez-Cobos, R
Finelli, F
Forastieri, F
Frailis, M
Fraisse, AA
Franceschi, E
Frolov, A
Galeotta, S
Galli, S
Ganga, K
Génova-Santos, RT
Gerbino, M
Ghosh, T
González-Nuevo, J
Górski, KM
Gratton, Steven
Gruppuso, A
Gudmundsson, JE
Hamann, J
Hansen, FK
Herranz, D
Hildebrandt, SR
Hivon, E
Huang, Z
Jaffe, AH
Jones, WC
Karakci, A
Keihänen, E
Keskitalo, R
Kiiveri, K
Kim, J
Kisner, TS
Knox, L
Krachmalnicoff, N
Kunz, M
Kurki-Suonio, H
Lagache, G
Lamarre, J-M
Lattanzi, M
Lawrence, CR
Jeune, M Le
Lemos, P
Lesgourgues, J
Levrier, F
Lewis, A
Liguori, M
Lilje, PB
Lilley, M
Lindholm, V
López-Caniego, M
Lubin, PM
Ma, Y-Z
Macías-Pérez, JF
Maggio, G
Maino, D
Mandolesi, N
Mangilli, A
Marcos-Caballero, A
Maris, M
Martin, PG
Martinelli, M
Martínez-González, E
Matarrese, S
Mauri, N
McEwen, JD
Meinhold, PR
Melchiorri, A
Mennella, A
Migliaccio, M
Millea, M
Mitra, S
Miville-Deschênes, M-A
Molinari, D
Montier, L
Morgante, G
Moss, A
Natoli, P
Nørgaard-Nielsen, HU
Pagano, L
Paoletti, D
Partridge, B
Patanchon, G
Peiris, HV
Perrotta, F
Pettorino, V
Piacentini, F
Polastri, L
Polenta, G
Puget, J-L
Rachen, JP
Reinecke, M
Remazeilles, M
Renzi, A
Rocha, G
Rosset, C
Roudier, G
Rubiño-Martín, JA
Ruiz-Granados, B
Salvati, L
Sandri, M
Savelainen, M
Scott, D
Shellard, Edward
Sirignano, C
Sirri, G
Spencer, LD
Sunyaev, R
Suur-Uski, A-S
Tauber, JA
Tavagnacco, D
Tenti, M
Toffolatti, L
Tomasi, M
Trombetti, T
Valenziano, L
Valiviita, J
Tent, B Van
Vibert, L
Vielva, P
Villa, F
Vittorio, N
Wandelt, BD
Wehus, IK
White, M
White, SDM
Zacchei, A
Zonca, A
Publication Date
2020-09-11Journal Title
Astronomy and Astrophysics
ISSN
0004-6361
Publisher
EDP Sciences
Volume
641
Pages
A6-A6
Language
English
Type
Article
This Version
VoR
Metadata
Show full item recordCitation
Collaboration, P., Aghanim, N., Akrami, Y., Ashdown, M., Aumont, J., Baccigalupi, C., Ballardini, M., et al. (2020). Planck 2018 results. VI. Cosmological parameters. Astronomy and Astrophysics, 641 A6-A6. https://doi.org/10.1051/0004-6361/201833910
Abstract
We present cosmological parameter results from the final full-mission Planck measurements of the CMB anisotropies. We find good consistency with the standard spatially-flat 6-parameter $\Lambda$CDM cosmology having a power-law spectrum of adiabatic scalar perturbations (denoted "base $\Lambda$CDM" in this paper), from polarization, temperature, and lensing, separately and in combination. A combined analysis gives dark matter density $\Omega_c h^2 = 0.120\pm 0.001$, baryon density $\Omega_b h^2 = 0.0224\pm 0.0001$, scalar spectral index $n_s = 0.965\pm 0.004$, and optical depth $\tau = 0.054\pm 0.007$ (in this abstract we quote $68\,\%$ confidence regions on measured parameters and $95\,\%$ on upper limits). The angular acoustic scale is measured to $0.03\,\%$ precision, with $100\theta_*=1.0411\pm 0.0003$. These results are only weakly dependent on the cosmological model and remain stable, with somewhat increased errors, in many commonly considered extensions. Assuming the base-$\Lambda$CDM cosmology, the inferred late-Universe parameters are: Hubble constant $H_0 = (67.4\pm 0.5)$km/s/Mpc; matter density parameter $\Omega_m = 0.315\pm 0.007$; and matter fluctuation amplitude $\sigma_8 = 0.811\pm 0.006$. We find no compelling evidence for extensions to the base-$\Lambda$CDM model. Combining with BAO we constrain the effective extra relativistic degrees of freedom to be $N_{\rm eff} = 2.99\pm 0.17$, and the neutrino mass is tightly constrained to $\sum m_\nu< 0.12$eV. The CMB spectra continue to prefer higher lensing amplitudes than predicted in base -$\Lambda$CDM at over $2\,\sigma$, which pulls some parameters that affect the lensing amplitude away from the base-$\Lambda$CDM model; however, this is not supported by the lensing reconstruction or (in models that also change the background geometry) BAO data. (Abridged)
Sponsorship
Science and Technology Facilities Council (ST/L000636/1)
Science and Technology Facilities Council (ST/M007065/1)
Science and Technology Facilities Council (ST/P000673/1)
Science and Technology Facilities Council (ST/N000927/1)
Embargo Lift Date
2100-01-01
Identifiers
External DOI: https://doi.org/10.1051/0004-6361/201833910
This record's URL: https://www.repository.cam.ac.uk/handle/1810/310335
Rights
Licence:
http://www.rioxx.net/licenses/all-rights-reserved
Statistics
Total file downloads (since January 2020). For more information on metrics see the
IRUS guide.