- Record: found
- Abstract: found
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N. Aghanim ,
Y. Akrami ,
M. Ashdown ,
J. Aumont ,
C. Baccigalupi ,
M. Ballardini ,
A. J. Banday ,
R. B. Barreiro ,
N. Bartolo ,
S. Basak ,
R. Battye ,
K. Benabed ,
J.-P. Bernard ,
M. Bersanelli ,
P. Bielewicz ,
J. J. Bock ,
J. R. Bond ,
J. Borrill ,
F. R. Bouchet ,
F. Boulanger ,
M. Bucher ,
C. Burigana ,
R. C. Butler ,
E. Calabrese ,
J.-F. Cardoso ,
J. Carron ,
A. Challinor ,
H. C. Chiang ,
J. Chluba ,
L. P. L. Colombo ,
C. Combet ,
D. Contreras ,
B. P. Crill ,
F. Cuttaia ,
P. de Bernardis ,
G. de Zotti ,
J. Delabrouille ,
J.-M. Delouis ,
E. Di Valentino ,
J. M. Diego ,
O. Doré ,
M. Douspis ,
A. Ducout ,
X. Dupac ,
S. Dusini ,
G. Efstathiou ,
F. Elsner ,
T. A. Enßlin ,
H. K. Eriksen ,
Y. Fantaye ,
M. Farhang ,
J. Fergusson ,
R. Fernandez-Cobos ,
F. Finelli ,
F. Forastieri ,
M. Frailis ,
A. A. Fraisse ,
E. Franceschi ,
A. Frolov ,
S. Galeotta ,
S. Galli ,
K. Ganga ,
R. T. Génova-Santos ,
M. Gerbino ,
T. Ghosh ,
J. González-Nuevo ,
K. M. Górski ,
S. Gratton ,
A. Gruppuso ,
J. E. Gudmundsson ,
J. Hamann ,
W. Handley ,
F. K. Hansen ,
D. Herranz ,
S. R. Hildebrandt ,
E. Hivon ,
Z. Huang ,
A. H. Jaffe ,
W. C. Jones ,
A. Karakci ,
E. Keihänen ,
R. Keskitalo ,
K. Kiiveri ,
J. Kim ,
T. S. Kisner ,
L. Knox ,
N. Krachmalnicoff ,
M. Kunz ,
H. Kurki-Suonio ,
G. Lagache ,
J.-M. Lamarre ,
A. Lasenby ,
M. Lattanzi ,
C. R. Lawrence ,
M. Le Jeune ,
P. Lemos ,
J. Lesgourgues ,
F. Levrier ,
A. Lewis ,
M. Liguori ,
P. B. Lilje ,
M. Lilley ,
V. Lindholm ,
M. López-Caniego ,
P. M. Lubin ,
Y.-Z. Ma ,
J. F. Macías-Pérez ,
G. Maggio ,
D. Maino ,
N. Mandolesi ,
A. Mangilli ,
A. Marcos-Caballero ,
M. Maris ,
P. G. Martin ,
M. Martinelli ,
E. Martínez-González ,
S. Matarrese ,
N. Mauri ,
J. D. McEwen ,
P. R. Meinhold ,
A. Melchiorri ,
A. Mennella ,
M. Migliaccio ,
M. Millea ,
S. Mitra ,
M.-A. Miville-Deschênes ,
D. Molinari ,
L. Montier ,
G. Morgante ,
A. Moss ,
P. Natoli ,
H. U. Nørgaard-Nielsen ,
L. Pagano ,
D. Paoletti ,
B. Partridge ,
G. Patanchon ,
H. V. Peiris ,
F. Perrotta ,
V. Pettorino ,
F. Piacentini ,
L. Polastri ,
G. Polenta ,
J.-L. Puget ,
J. P. Rachen ,
M. Reinecke ,
M. Remazeilles ,
A. Renzi ,
G. Rocha ,
C. Rosset ,
G. Roudier ,
J. A. Rubiño-Martín ,
B. Ruiz-Granados ,
L. Salvati ,
M. Sandri ,
M. Savelainen ,
D. Scott ,
E. P. S. Shellard ,
C. Sirignano ,
G. Sirri ,
L. D. Spencer ,
R. Sunyaev ,
A.-S. Suur-Uski ,
J. A. Tauber ,
D. Tavagnacco ,
M. Tenti ,
L. Toffolatti ,
M. Tomasi ,
T. Trombetti ,
L. Valenziano ,
J. Valiviita ,
B. Van Tent ,
L. Vibert ,
P. Vielva ,
F. Villa ,
N. Vittorio ,
B. D. Wandelt ,
I. K. Wehus ,
M. White ,
S. D. M. White ,
A. Zacchei ,
A. Zonca ,
Planck Collaboration

September 11 2020

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We present cosmological parameter results from the final full-mission
*Planck* measurements of the cosmic microwave background (CMB) anisotropies, combining information
from the temperature and polarization maps and the lensing reconstruction. Compared
to the 2015 results, improved measurements of large-scale polarization allow the reionization
optical depth to be measured with higher precision, leading to significant gains in
the precision of other correlated parameters. Improved modelling of the small-scale
polarization leads to more robust constraints on many parameters, with residual modelling
uncertainties estimated to affect them only at the 0.5
*σ* level. We find good consistency with the standard spatially-flat 6-parameter ΛCDM
cosmology having a power-law spectrum of adiabatic scalar perturbations (denoted “base
ΛCDM” in this paper), from polarization, temperature, and lensing, separately and
in combination. A combined analysis gives dark matter density Ω
_{c}
*h*
^{2} = 0.120 ± 0.001, baryon density Ω
_{b}
*h*
^{2} = 0.0224 ± 0.0001, scalar spectral index
*n*
_{s} = 0.965 ± 0.004, and optical depth
*τ* = 0.054 ± 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
*θ*
_{*} = 1.0411 ± 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-ΛCDM cosmology, the inferred (model-dependent) late-Universe parameters
are: Hubble constant
*H*
_{0} = (67.4 ± 0.5) km s
^{−1} Mpc
^{−1}; matter density parameter Ω
_{m} = 0.315 ± 0.007; and matter fluctuation amplitude
*σ*
_{8} = 0.811 ± 0.006. We find no compelling evidence for extensions to the base-ΛCDM model.
Combining with baryon acoustic oscillation (BAO) measurements (and considering single-parameter
extensions) we constrain the effective extra relativistic degrees of freedom to be
*N*
_{eff} = 2.99 ± 0.17, in agreement with the Standard Model prediction
*N*
_{eff} = 3.046, and find that the neutrino mass is tightly constrained to ∑
*m*
_{
ν
} < 0.12 eV. The CMB spectra continue to prefer higher lensing amplitudes than predicted
in base ΛCDM at over 2
*σ*, which pulls some parameters that affect the lensing amplitude away from the ΛCDM
model; however, this is not supported by the lensing reconstruction or (in models
that also change the background geometry) BAO data. The joint constraint with BAO
measurements on spatial curvature is consistent with a flat universe, Ω
_{
K
} = 0.001 ± 0.002. Also combining with Type Ia supernovae (SNe), the dark-energy equation
of state parameter is measured to be
*w*
_{0} = −1.03 ± 0.03, consistent with a cosmological constant. We find no evidence for
deviations from a purely power-law primordial spectrum, and combining with data from
BAO, BICEP2, and Keck Array data, we place a limit on the tensor-to-scalar ratio
*r*
_{0.002} < 0.06. Standard big-bang nucleosynthesis predictions for the helium and deuterium
abundances for the base-ΛCDM cosmology are in excellent agreement with observations.
The
*Planck* base-ΛCDM results are in good agreement with BAO, SNe, and some galaxy lensing observations,
but in slight tension with the Dark Energy Survey’s combined-probe results including
galaxy clustering (which prefers lower fluctuation amplitudes or matter density parameters),
and in significant, 3.6
*σ*, tension with local measurements of the Hubble constant (which prefer a higher value).
Simple model extensions that can partially resolve these tensions are not favoured
by the
*Planck* data.

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N. Aghanim, Y. Akrami, M Ashdown … (2020)

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Eduardo Banados, Bram Venemans, Chiara Mazzucchelli … (2017)

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N. Aghanim, Y. Akrami, M Ashdown … (2020)