Improved Constraints on Primordial Gravitational Waves using Planck, WMAP, and BICEP/Keck Observations through the 2018 Observing Season

P A R Ade¹, Z Ahmed², M Amiri³, D Barkats⁴, R Basu Thakur⁵, C A Bischoff⁶, D Beck^{2 7}, J J Bock^{5 8}, H Boenish⁴, E Bullock⁹, V Buza¹⁰, J R Cheshire⁹, J Connors⁴, J Cornelison⁴, M Crumrine¹¹, A Cukierman^{2 7}, E V Denison¹², M Dierickx⁴, L Duband¹³, M Eiben⁴, S Fatigoni³, J P Filippini^{14 15}, S Fliescher¹¹, N Goeckner-Wald⁷, D C Goldfinger⁴, J Grayson⁷, P Grimes⁴, G Hall¹¹, G Halal⁷, M Halpern³, E Hand⁶, S Harrison⁴, S Henderson², S R Hildebrandt^{5 8}, G C Hilton¹², J Hubmayr¹², H Hui⁵, K D Irwin^{2 7 12}, J Kang^{5 7}, K S Karkare^{4 10}, E Karpel⁷, S Kefeli⁵, S A Kernasovskiy⁷, J M Kovac^{4 16}, C L Kuo^{2 7}, K Lau¹¹, E M Leitch¹⁰, A Lennox¹⁴, K G Megerian⁸, L Minutolo⁵, L Moncelsi⁵, Y Nakato⁷, T Namikawa¹⁷, H T Nguyen⁸, R O'Brient^{5 8}, R W Ogburn^{2 7}, S Palladino⁶, T Prouve¹³, C Pryke^{9 11}, B Racine^{4 18}, C D Reintsema¹², S Richter⁴, A Schillaci⁵, R Schwarz¹¹, B L Schmitt⁴, C D Sheehy¹⁹, A Soliman⁵, T St Germaine^{4 16}, B Steinbach⁵, R V Sudiwala¹, G P Teply⁵, K L Thompson^{2 7}, J E Tolan⁷, C Tucker¹, A D Turner⁸, C Umiltà^{6 14}, C Vergès⁴, A G Vieregg^{10 20}, A Wandui⁵, A C Weber⁸, D V Wiebe³, J Willmert¹¹, C L Wong^{4 16}, W L K Wu², H Yang⁷, K W Yoon^{2 7}, E Young^{2 7}, C Yu⁷, L Zeng⁴, C Zhang⁵, S Zhang⁵; BICEP/<i>Keck</i> Collaboration

Affiliations

¹ School of Physics and Astronomy, Cardiff University, Cardiff CF24 3AA, United Kingdom.
² Kavli Institute for Particle Astrophysics and Cosmology, SLAC National Accelerator Laboratory, 2575 Sand Hill Rd, Menlo Park, California 94025, USA.
³ Department of Physics and Astronomy, University of British Columbia, Vancouver, British Columbia V6T 1Z1, Canada.
⁴ Center for Astrophysics, Harvard & Smithsonian, Cambridge, Massachusetts 02138, USA.
⁵ Department of Physics, California Institute of Technology, Pasadena, California 91125, USA.
⁶ Department of Physics, University of Cincinnati, Cincinnati, Ohio 45221, USA.
⁷ Department of Physics, Stanford University, Stanford, California 94305, USA.
⁸ Jet Propulsion Laboratory, Pasadena, California 91109, USA.
⁹ Minnesota Institute for Astrophysics, University of Minnesota, Minneapolis, Minnesota 55455, USA.
¹⁰ Kavli Institute for Cosmological Physics, University of Chicago, Chicago, Illinois 60637, USA.
¹¹ School of Physics and Astronomy, University of Minnesota, Minneapolis, Minnesota 55455, USA.
¹² National Institute of Standards and Technology, Boulder, Colorado 80305, USA.
¹³ Service des Basses Températures, Commissariat à l'Energie Atomique, 38054 Grenoble, France.
¹⁴ Department of Physics, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA.
¹⁵ Department of Astronomy, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA.
¹⁶ Department of Physics, Harvard University, Cambridge, Massachusetts 02138, USA.
¹⁷ Kavli Institute for the Physics and Mathematics of the Universe (WPI), UTIAS, The University of Tokyo, Kashiwa, Chiba 277-8583, Japan.
¹⁸ Aix-Marseille Université, CNRS/IN2P3, CPPM, Marseille 13288, France.
¹⁹ Physics Department, Brookhaven National Laboratory, Upton, New York 11973, USA.
²⁰ Department of Physics, Enrico Fermi Institute, University of Chicago, Chicago, Illinois 60637, USA.

PMID:34678017
DOI: 10.1103/PhysRevLett.127.151301

Improved Constraints on Primordial Gravitational Waves using Planck, WMAP, and BICEP/Keck Observations through the 2018 Observing Season

P A R Ade et al. Phys Rev Lett.2021.

.2021 Oct 8;127(15):151301.

doi: 10.1103/PhysRevLett.127.151301.

Authors

Affiliations

¹ School of Physics and Astronomy, Cardiff University, Cardiff CF24 3AA, United Kingdom.
² Kavli Institute for Particle Astrophysics and Cosmology, SLAC National Accelerator Laboratory, 2575 Sand Hill Rd, Menlo Park, California 94025, USA.
³ Department of Physics and Astronomy, University of British Columbia, Vancouver, British Columbia V6T 1Z1, Canada.
⁴ Center for Astrophysics, Harvard & Smithsonian, Cambridge, Massachusetts 02138, USA.
⁵ Department of Physics, California Institute of Technology, Pasadena, California 91125, USA.
⁶ Department of Physics, University of Cincinnati, Cincinnati, Ohio 45221, USA.
⁷ Department of Physics, Stanford University, Stanford, California 94305, USA.
⁸ Jet Propulsion Laboratory, Pasadena, California 91109, USA.
⁹ Minnesota Institute for Astrophysics, University of Minnesota, Minneapolis, Minnesota 55455, USA.
¹⁰ Kavli Institute for Cosmological Physics, University of Chicago, Chicago, Illinois 60637, USA.
¹¹ School of Physics and Astronomy, University of Minnesota, Minneapolis, Minnesota 55455, USA.
¹² National Institute of Standards and Technology, Boulder, Colorado 80305, USA.
¹³ Service des Basses Températures, Commissariat à l'Energie Atomique, 38054 Grenoble, France.
¹⁴ Department of Physics, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA.
¹⁵ Department of Astronomy, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA.
¹⁶ Department of Physics, Harvard University, Cambridge, Massachusetts 02138, USA.
¹⁷ Kavli Institute for the Physics and Mathematics of the Universe (WPI), UTIAS, The University of Tokyo, Kashiwa, Chiba 277-8583, Japan.
¹⁸ Aix-Marseille Université, CNRS/IN2P3, CPPM, Marseille 13288, France.
¹⁹ Physics Department, Brookhaven National Laboratory, Upton, New York 11973, USA.
²⁰ Department of Physics, Enrico Fermi Institute, University of Chicago, Chicago, Illinois 60637, USA.

PMID:34678017
DOI: 10.1103/PhysRevLett.127.151301

Abstract

We present results from an analysis of all data taken by the BICEP2, Keck Array, and BICEP3 CMB polarization experiments up to and including the 2018 observing season. We add additional Keck Array observations at 220 GHz and BICEP3 observations at 95 GHz to the previous 95/150/220 GHz dataset. The Q/U maps now reach depths of 2.8, 2.8, and 8.8 μK_{CMB} arcmin at 95, 150, and 220 GHz, respectively, over an effective area of ≈600 square degrees at 95 GHz and ≈400 square degrees at 150 and 220 GHz. The 220 GHz maps now achieve a signal-to-noise ratio on polarized dust emission exceeding that of Planck at 353 GHz. We take auto- and cross-spectra between these maps and publicly available WMAP and Planck maps at frequencies from 23 to 353 GHz and evaluate the joint likelihood of the spectra versus a multicomponent model of lensed ΛCDM+r+dust+synchrotron+noise. The foreground model has seven parameters, and no longer requires a prior on the frequency spectral index of the dust emission taken from measurements on other regions of the sky. This model is an adequate description of the data at the current noise levels. The likelihood analysis yields the constraint r_{0.05}<0.036 at 95% confidence. Running maximum likelihood search on simulations we obtain unbiased results and find that σ(r)=0.009. These are the strongest constraints to date on primordial gravitational waves.

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Improved Constraints on Primordial Gravitational Waves using Planck, WMAP, and BICEP/Keck Observations through the 2018 Observing Season

Affiliations

Improved Constraints on Primordial Gravitational Waves using Planck, WMAP, and BICEP/Keck Observations through the 2018 Observing Season

Authors

Affiliations

Abstract

LinkOut - more resources

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