Статья

<i>Planck</i>2018 results

N. AghanimY. AkramiDpartement de Physique, cole normale suprieure, PSL Research University, CNRS, 24 rue Lhomond, 75005 Paris, FranceM. AshdownAstrophysics Group, Cavendish Laboratory, University of Cambridge, J J Thomson Avenue, Cambridge CB3 0HE, UKJ. AumontC. BaccigalupiM. BallardiniDepartment of Physics & Astronomy, University of the Western Cape, Cape Town 7535, South AfricaA. J. BandayCNRS, IRAP, 9 Av. Colonel Roche, BP 44346, 31028 Toulouse Cedex 4, FranceR. B. BarreiroN. BartoloDipartimento di Fisica e Astronomia G. Galilei, Universit degli Studi di Padova, Via Marzolo 8, 35131 Padova, ItalyS. BasakK. BenabedJ.-P. BernardCNRS, IRAP, 9 Av. Colonel Roche, BP 44346, 31028 Toulouse Cedex 4, FranceM. BersanelliDipartimento di Fisica, Universit degli Studi di Milano, Via Celoria, 16, Milano, ItalyP. BielewiczJ. J. BockCalifornia Institute of Technology, Pasadena, California, USAJ. R. BondCITA, University of Toronto, 60 St. George St., Toronto, ON M5S 3H8, CanadaJ. BorrillComputational Cosmology Center, Lawrence Berkeley National Laboratory, Berkeley, CA, USAF. R. BouchetF. BoulangerM. BucherC. BuriganaDipartimento di Fisica e Scienze della Terra, Universit di Ferrara, Via Saragat 1, 44122 Ferrara, ItalyE. CalabreseJ.-F. CardosoJ. CarronDepartment of Physics and Astronomy, University of Sussex, Brighton BN1 9QH, UKA. ChallinorCentre for Theoretical Cosmology, DAMTP, University of Cambridge, Wilberforce Road, Cambridge CB3 0WA, UKH. C. ChiangL. P. L. ColomboDipartimento di Fisica, Universit degli Studi di Milano, Via Celoria, 16, Milano, ItalyC. CombetLaboratoire de Physique Subatomique et Cosmologie, Universit Grenoble-Alpes, CNRS/IN2P3, 53 rue des Martyrs,B. P. CrillCalifornia Institute of Technology, Pasadena, California, USAF. CuttaiaP. de BernardisDipartimento di Fisica, Universit La Sapienza, P.le A. Moro 2, Roma, ItalyG. de ZottiJ. DelabrouilleAPC, AstroParticule et Cosmologie, Universit Paris Diderot,E. Di ValentinoJodrell Bank Centre for Astrophysics, Alan Turing Building, School of Physics and Astronomy, The University of Manchester, Oxford Road,, Manchester M13 9PL, UKJ. M. DiegoO. DoréM. DouspisA. DucoutKavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU, WPI), UTIAS, The University of Tokyo, Chiba 277-8583, JapanX. DupacG. EfstathiouKavli Institute for Cosmology Cambridge, Madingley Road, Cambridge CB3 0HA, UKF. ElsnerT. A. EnßlinH. K. EriksenY. FantayeAfrican Institute for Mathematical Sciences, 6-8 Melrose Road, Muizenberg, Cape Town, South AfricaR. Fernandez-CobosF. FinelliF. ForastieriDipartimento di Fisica e Scienze della Terra, Universit di Ferrara, Via Saragat 1, 44122 Ferrara, ItalyM. FrailisA. A. FraisseDepartment of Physics, Princeton University, Princeton, NJ, USAE. FranceschiA. FrolovS. GaleottaS. GalliK. GangaAPC, AstroParticule et Cosmologie, Universit Paris Diderot,R. T. Génova-SantosM. GerbinoT. GhoshCahill Center for Astronomy and Astrophysics, California Institute of Technology, Pasadena, CA 91125, USAJ. González-NuevoK. M. GórskiS. GrattonKavli Institute for Cosmology Cambridge, Madingley Road, Cambridge CB3 0HA, UKA. GruppusoJ. E. GudmundssonDepartment of Physics, Princeton University, Princeton, NJ, USAJ. HamannW. HandleyAstrophysics Group, Cavendish Laboratory, University of Cambridge, J J Thomson Avenue, Cambridge CB3 0HE, UKF. K. HansenD. HerranzE. HivonZ. HuangA. H. JaffeW. C. JonesDepartment of Physics, Princeton University, Princeton, NJ, USAA. KarakciE. KeihänenR. KeskitaloComputational Cosmology Center, Lawrence Berkeley National Laboratory, Berkeley, CA, USAK. KiiveriDepartment of Physics, University of Helsinki, Gustaf Hllstrmin katu 2a, Helsinki, FinlandJ. KimL. KnoxDepartment of Physics, University of California, One Shields Avenue, Davis, CA, USAN. KrachmalnicoffM. KunzAfrican Institute for Mathematical Sciences, 6-8 Melrose Road, Muizenberg, Cape Town, South AfricaH. Kurki-SuonioDepartment of Physics, University of Helsinki, Gustaf Hllstrmin katu 2a, Helsinki, FinlandG. LagacheAix Marseille Univ, CNRS, CNES, LAM, Marseille, FranceJ.-M. LamarreA. LasenbyAstrophysics Group, Cavendish Laboratory, University of Cambridge, J J Thomson Avenue, Cambridge CB3 0HE, UKM. LattanziDipartimento di Fisica e Scienze della Terra, Universit di Ferrara, Via Saragat 1, 44122 Ferrara, ItalyC. R. LawrenceJet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena CA, USAM. Le JeuneAPC, AstroParticule et Cosmologie, Universit Paris Diderot,F. LevrierA. LewisDepartment of Physics and Astronomy, University of Sussex, Brighton BN1 9QH, UKM. LiguoriDipartimento di Fisica e Astronomia G. Galilei, Universit degli Studi di Padova, Via Marzolo 8, 35131 Padova, ItalyP. B. LiljeV. LindholmDepartment of Physics, University of Helsinki, Gustaf Hllstrmin katu 2a, Helsinki, FinlandM. López-CaniegoP. M. LubinDepartment of Physics, University of California, Santa Barbara, CA, USAY.-Z. MaJ. F. Macías-PérezG. MaggioD. MainoDipartimento di Fisica, Universit degli Studi di Milano, Via Celoria, 16, Milano, ItalyN. MandolesiDipartimento di Fisica e Scienze della Terra, Universit di Ferrara, Via Saragat 1, 44122 Ferrara, ItalyA. MangilliCNRS, IRAP, 9 Av. Colonel Roche, BP 44346, 31028 Toulouse Cedex 4, FranceA. Marcos-CaballeroM. Maris

2019en

ABI

Аннотация

We present measurements of the cosmic microwave background (CMB) lensing potential using the final Planck 2018 temperature and polarization data. Using polarization maps filtered to account for the noise anisotropy, we increase the significance of the detection of lensing in the polarization maps from 5 σ to 9 σ . Combined with temperature, lensing is detected at 40 σ . We present an extensive set of tests of the robustness of the lensing-potential power spectrum, and construct a minimum-variance estimator likelihood over lensing multipoles 8 ≤ L ≤ 400 (extending the range to lower L compared to 2015), which we use to constrain cosmological parameters. We find good consistency between lensing constraints and the results from the Planck CMB power spectra within the ΛCDM model. Combined with baryon density and other weak priors, the lensing analysis alone constrains σ 8 Ω m 0.25 = 0.589 ± 0.020 (1 σ errors). Also combining with baryon acoustic oscillation data, we find tight individual parameter constraints, σ 8 = 0.811 ± 0.019, H 0 = 67.9 −1.3 +1.2 km s −1 Mpc −1 , and Ω m = 0.303 −0.018 +0.016 . Combining with Planck CMB power spectrum data, we measure σ 8 to better than 1% precision, finding σ 8 = 0.811 ± 0.006. CMB lensing reconstruction data are complementary to galaxy lensing data at lower redshift, having a different degeneracy direction in σ 8 − Ω m space; we find consistency with the lensing results from the Dark Energy Survey, and give combined lensing-only parameter constraints that are tighter than joint results using galaxy clustering. Using the Planck cosmic infrared background (CIB) maps as an additional tracer of high-redshift matter, we make a combined Planck -only estimate of the lensing potential over 60% of the sky with considerably more small-scale signal. We additionally demonstrate delensing of the Planck power spectra using the joint and individual lensing potential estimates, detecting a maximum removal of 40% of the lensing-induced power in all spectra. The improvement in the sharpening of the acoustic peaks by including both CIB and the quadratic lensing reconstruction is detected at high significance.

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Идентификаторы

DOI: 10.1051/0004-6361/201833886

Цитирования и источники

Цитирований: 5Использованных источников: 0

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