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Cited by 1,197Cosmology and Gravitation TheoriesDark Matter and Cosmic PhenomenaGalaxies: Formation, Evolution, Phenomena

Planck 2018 results: V. CMB power spectra and likelihoods

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Planck Collaboration, Aghanim, N., Akrami, Y., Ashdown, M., Aumont, J., Baccigalupi, C., Ballardini, M., Banday, A. J. +160 more·2020·Astronomy & Astrophysics
DOI 10.1051/0004-6361/201936386
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Abstract

We describe the legacy Planck cosmic microwave background (CMB) likelihoods derived from the 2018 data release. The overall approach is similar in spirit to the one retained for the 2013 and 2015 data release, with a hybrid method using different approximations at low ( ℓ < 30) and high ( ℓ ≥ 30) multipoles, implementing several methodological and data-analysis refinements compared to previous releases. With more realistic simulations, and better correction and modelling of systematic effects, we can now make full use of the CMB polarization observed in the High Frequency Instrument (HFI) channels. The low-multipole EE cross-spectra from the 100 GHz and 143 GHz data give a constraint on the ΛCDM reionization optical-depth parameter τ to better than 15% (in combination with the TT low- ℓ data and the high- ℓ temperature and polarization data), tightening constraints on all parameters with posterior distributions correlated with τ . We also update the weaker constraint on τ from the joint TEB likelihood using the Low Frequency Instrument (LFI) channels, which was used in 2015 as part of our baseline analysis. At higher multipoles, the CMB temperature spectrum and likelihood are very similar to previous releases. A better model of the temperature-to-polarization leakage and corrections for the effective calibrations of the polarization channels (i.e., the polarization efficiencies) allow us to make full use of polarization spectra, improving the ΛCDM constraints on the parameters θ MC , ω c , ω b , and H 0 by more than 30%, and n s by more than 20% compared to TT-only constraints. Extensive tests on the robustness of the modelling of the polarization data demonstrate good consistency, with some residual modelling uncertainties. At high multipoles, we are now limited mainly by the accuracy of the polarization efficiency modelling. Using our various tests, simulations, and comparison between different high-multipole likelihood implementations, we estimate the consistency of the results to be better than the 0.5 σ level on the ΛCDM parameters, as well as classical single-parameter extensions for the joint likelihood (to be compared to the 0.3 σ levels we achieved in 2015 for the temperature data alone on ΛCDM only). Minor curiosities already present in the previous releases remain, such as the differences between the best-fit ΛCDM parameters for the ℓ < 800 and ℓ > 800 ranges of the power spectrum, or the preference for more smoothing of the power-spectrum peaks than predicted in ΛCDM fits. These are shown to be driven by the temperature power spectrum and are not significantly modified by the inclusion of the polarization data. Overall, the legacy Planck CMB likelihoods provide a robust tool for constraining the cosmological model and represent a reference for future CMB observations.

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  • Fixing the parameter A_lens=1.2, similar to its best fit obtained by Planck, could be a way to resolve the internal disagreement of the two multipole regions, directly indicating a systematic error present in the data.

    “fixing the parameter A lens = 1.2, similar to its best fit obtained by Planck, could be a way to resolve this internal disagreement of the two multipole regions, directly indicating a systematic error present in the data.”

    From Challenges of the Standard Cosmological Model (2022) · cites this paper as [12]

    Section 3.9.2 reports that allowing A_L to vary reduces parameter shifts between the ℓ < 800 and ℓ > 800 regions, but it does not test fixing A_L at 1.2. More importantly, the section says the shifts are consistent with statistical fluctuations and do not provide sufficient evidence of a systematic origin, contrary to the claim that they directly indicate a systematic error. No page number was supplied in our copy. (LLM, conf=0.88)

    Experimental — accuracy not yet measured

  • The S8 tension is at the level of 3.1σ with KiDS-100, which gives S8=0.766+0.020-0.014, and 2.5σ with DES-Y3, which gives S8=0.759+0.025-0.025, while Planck prefers a higher value S8=0.834+0.016-0.016.

    “This tension is becoming statistically significant and is now at the level of 3.1σ with KiDS-100 [77], that gives S 8 = 0.766 +0.020 -0.014 , and 2.5σ with DES-Y3 [78], that gives S 8 = 0.759 +0.025 -0.025 , while Planck prefers a higher value for S 8 = 0.834 +0.016 -0.016 .”

    From Challenges of the Standard Cosmological Model (2022) · cites this paper as [12]

    Our copy discusses Planck cosmological-parameter constraints (section 3.3.3) and internal parameter shifts (section 3.9.2), but the passages found do not give S8 = 0.834 ± 0.016 or compare Planck with KiDS-1000 and DES-Y3. Searches for that value, S8, and the named surveys found no decisive passage; the copy is also truncated. (LLM, conf=0.70)

    Experimental — accuracy not yet measured

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Authors
Planck Collaboration, Aghanim, N., Akrami, Y., Ashdown, M., Aumont, J., Baccigalupi, C., Ballardini, M., Banday, A. J., Barreiro, R. B., Bartolo, N., Basak, S., Benabed, K., Bernard, J.-P., Bersanelli, M., Bielewicz, P., Bock, J. J., Bond, J. R., Borrill, J., Bouchet, F. R., Boulanger, F., Bucher, M., Burigana, C., Butler, R. C., Calabrese, E., Cardoso, J.-F., Carron, J., Casaponsa, B., Challinor, A., Chiang, H. C., Colombo, L. P. L., Combet, C., Crill, B. P., Cuttaia, F., de Bernardis, P., de Rosa, A., de Zotti, G., Delabrouille, J., Delouis, J.-M., Di Valentino, E., Diego, J. M., Doré, O., Douspis, M., Ducout, A., Dupac, X., Dusini, S., Efstathiou, G., Elsner, F., Enßlin, T. A., Eriksen, H. K., Fantaye, Y., Fernandez-Cobos, R., Finelli, F., Frailis, M., Fraisse, A. A., Franceschi, E., Frolov, A., Galeotta, S., Galli, S., Ganga, K., Génova-Santos, R. T., Gerbino, M., Ghosh, T., Giraud-Héraud, Y., González-Nuevo, J., Górski, K. M., Gratton, S., Gruppuso, A., Gudmundsson, J. E., Hamann, J., Handley, W., Hansen, F. K., Herranz, D., Hivon, E., Huang, Z., Jaffe, A. H., Jones, W. C., Keihänen, E., Keskitalo, R., Kiiveri, K., Kim, J., Kisner, T. S., Krachmalnicoff, N., Kunz, M., Kurki-Suonio, H., Lagache, G., Lamarre, J.-M., Lasenby, A., Lattanzi, M., Lawrence, C. R., Le Jeune, M., Levrier, F., Lewis, A., Liguori, M., Lilje, P. B., Lilley, M., Lindholm, V., López-Caniego, M., Lubin, P. M., Ma, Y.-Z., Macías-Pérez, J. F., Maggio, G., Maino, D., Mandolesi, N., Mangilli, A., Marcos-Caballero, A., Maris, M., Martin, P. G., Martínez-González, E., Matarrese, S., Mauri, N., McEwen, J. D., Meinhold, P. R., Melchiorri, A., Mennella, A., Migliaccio, M., Millea, M., Miville-Deschênes, M.-A., Molinari, D., Moneti, A., Montier, L., Morgante, G., Moss, A., Natoli, P., Nørgaard-Nielsen, H. U., Pagano, L., Paoletti, D., Partridge, B., Patanchon, G., Peiris, H. V., Perrotta, F., Pettorino, V., Piacentini, F., Polenta, G., Puget, J.-L., Rachen, J. P., Reinecke, M., Remazeilles, M., Renzi, A., Rocha, G., Rosset, C., Roudier, G., Rubiño-Martín, J. A., Ruiz-Granados, B., Salvati, L., Sandri, M., Savelainen, M., Scott, D., Shellard, E. P. S., Sirignano, C., Sirri, G., Spencer, L. D., Sunyaev, R., Suur-Uski, A.-S., Tauber, J. A., Tavagnacco, D., Tenti, M., Toffolatti, L., Tomasi, M., Trombetti, T., Valiviita, J., Van Tent, B., Vielva, P., Villa, F., Vittorio, N., Wandelt, B. D., Wehus, I. K., Zacchei, A., & Zonca, A.
Affiliations
  • Université Paris-Sud (FR)
  • Leiden University (NL)
  • University of Cambridge (GB)
  • Centre National de la Recherche Scientifique (FR)
  • California Institute of Technology (US)
  • University of Toronto (CA)
  • Lawrence Berkeley National Laboratory (US)
  • Princeton University (US)
  • African Institute for Mathematical Sciences (ZA)
  • Argonne National Laboratory (US)
  • University of Sussex (GB)
  • Universidad de Cantabria (ES)
  • University of Milan (IT)
  • University of Rome Tor Vergata (IT)
  • Osservatorio di Astrofisica e Scienza dello Spazio (IT)
  • University of Nottingham (GB)
  • University of Ferrara (IT)
  • DTU Space (DK)
  • Haverford College (US)
  • University College London (GB)
  • Scuola Internazionale Superiore di Studi Avanzati (IT)
  • Radboud University Nijmegen (NL)
  • Max Planck Institute for Astrophysics (DE)
  • University of Manchester (GB)
  • Istituto Nazionale di Fisica Nucleare, Sezione di Padova (IT)
  • Universidad de La Laguna (ES)
  • Trieste Astronomical Observatory (IT)
  • University of British Columbia (CA)
  • University of Padua (IT)
  • Istituto Nazionale di Fisica Nucleare, Sezione di Bologna (IT)
  • Cardiff University (GB)
  • Russian Academy of Sciences (RU)
  • University of Helsinki (FI)
  • European Space Agency (FR)
  • University of Trieste (IT)
  • Istituto Nazionale di Fisica Nucleare, Centro Nazionale Analisi Fotogrammi (IT)
  • Universidad de Oviedo (ES)
  • Istituto Nazionale di Fisica Nucleare, Sezione di Ferrara (IT)
  • University of Oslo (NO)
  • San Diego Supercomputer Center (US)
ORCID
Venue
Astronomy & Astrophysics
Publisher
EDP Sciences
Published
2020-09
Volume
641
Pages
A5
ISSN
  • 0004-6361 (ISSN-L)
  • 1432-0746
DOI
10.1051/0004-6361/201936386
OpenAlex
W3103282112
Cited by
1,197
References
3
Citations by year
2026: 148 · 2025: 234 · 2024: 191 · 2023: 165 · 2022: 170 · 2021: 169 · 2020: 102 · 2019: 13 · 2018: 3 · 2017: 1
FWCI
68.16
Type
journal article
Language
en
Open access
Licence
Locations
  • Astronomy and Astrophysics (publishedVersion, cc-by)
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  • CaltechAUTHORS (California Institute of Technology) (submittedVersion, cc-by)
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  • IRIS Research product catalog (Sapienza University of Rome) (submittedVersion, cc-by-nc-nd)
  • OSTI OAI (U.S. Department of Energy Office of Scientific and Technical Information) (submittedVersion)
  • Technical University of Denmark, DTU Orbit (Technical University of Denmark, DTU) (submittedVersion, cc-by)
  • MPG.PuRe (Max Planck Society) (submittedVersion)
  • UCrea (University of Cantabria) (submittedVersion, cc-by)
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  • Radboud Repository (Radboud University) (submittedVersion, other-oa)
  • arXiv (Cornell University)
Funders
  • National Aeronautics and Space Administration
  • California Institute of Technology
  • Helsingin Yliopisto
  • UK Space Agency
  • European Space Agency
  • Haverford College
  • Imperial College London
  • Science Foundation Ireland
  • Agence Nationale de la Recherche (ANR-16-IDEX-0008)
  • Universiteit Leiden
  • Partnership for Advanced Computing in Europe AISBL
  • Centre National d’Etudes Spatiales (IN2P3)
  • Tekes
  • Max-Planck-Gesellschaft
  • China Scholarship Council
  • Centre National de la Recherche Scientifique
  • Istituto Nazionale di Astrofisica
  • Universitetet i Oslo
  • Ministério da Ciência, Tecnologia e Ensino Superior
  • Universidad de Cantabria
  • Université Paris-Saclay
  • Istituto Nazionale di Fisica Nucleare
  • Gran Sasso Science Institute
  • Instituto de Física de Cantabria
  • Instituto de Astrofísica de Canarias
  • Jet Propulsion Laboratory
  • Science and Technology Facilities Council (IN2P3)
  • Fundação para a Ciência e a Tecnologia
  • Institut National de Physique Nucléaire et de Physique des Particules
  • Argonne National Laboratory
Topics
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Cosmology and Gravitation Theories
  • Physical Sciences › Physics and Astronomy › Nuclear and High Energy Physics › Dark Matter and Cosmic Phenomena
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Galaxies: Formation, Evolution, Phenomena
Keywords
cosmic microwave background, Planck 2018, reionization optical depth, CMB polarization, angular power spectrum, Hubble constant, primordial power spectrum, cosmological parameters, systematic effects

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