Improved Constraints on Primordial Gravitational Waves using Planck, WMAP, and BICEP/Keck Observations through the 2018 Observing Season
- Creators
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Ade, P. A. R.
- Ahmed, Z.
- Amiri, M.
- Barkats, D.
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Basu Thakur, R.
- Bischoff, C. A.
- Beck, D.
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Bock, J. J.
- Boenish, H.
- Bullock, E.
- Buza, V.
- Cheshire, J. R.
- Connors, J.
- Cornelison, J.
- Crumrine, M.
- Cukierman, A.
- Denison, E. V.
- Dierickx, M.
- Duband, L.
- Eiben, M.
- Fatigoni, S.
- Filippini, J. P.
- Fliescher, S.
- Goeckner-Wald, N.
- Goldfinger, D. C.
- Grayson, J.
- Grimes, P.
- Hall, G.
- Halal, G.
- Halpern, M.
- Hand, E.
- Harrison, S.
- Henderson, S.
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Hildebrandt, S. R.
- Hilton, G. C.
- Hubmayr, J.
- Hui, H.
- Irwin, K. D.
- Kang, J.
- Karkare, K. S.
- Karpel, E.
- Kefeli, S.
- Kernasovskiy, S. A.
- Kovac, J. M.
- Kuo, C. L.
- Lau, K.
- Leitch, E. M.
- Lennox, A.
- Megerian, K. G.
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Minutolo, L.
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Moncelsi, L.
- Nakato, Y.
- Namikawa, T.
- Nguyen, H. T.
- O'Brient, R.
- Ogburn, R. W.
- Palladino, S.
- Prouve, T.
- Pryke, C.
- Racine, B.
- Reintsema, C. D.
- Richter, S.
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Schillaci, A.
- Schwarz, R.
- Schmitt, B. L.
- Sheehy, C. D.
- Soliman, A.
- Germaine, T. St.
- Steinbach, B.
- Sudiwala, R. V.
- Teply, G. P.
- Thompson, K. L.
- Tolan, J. E.
- Tucker, C.
- Turner, A. D.
- Umiltà, C.
- Vergès, C.
- Vieregg, A. G.
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Wandui, A.
- Weber, A. C.
- Wiebe, D. V.
- Willmert, J.
- Wong, C. L.
- Wu, W. L. K.
- Yang, H.
- Yoon, K. W.
- Young, E.
- Yu, C.
- Zeng, L.
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Zhang, C.
- Zhang, S.
- BICEP Collaboration
- Keck Collaboration
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.
Additional Information
© 2021 American Physical Society. Received 21 June 2021; accepted 12 August 2021; published 4 October 2021. The BICEP/Keck projects have been made possible through a series of grants from the National Science Foundation including Grants No. 0742818, No. 0742592, No. 1044978, No. 1110087, No. 1145172, No. 1145143, No. 1145248, No. 1639040, No. 1638957, No. 1638978, and No. 1638970, and by the Keck Foundation. The development of antenna-coupled detector technology was supported by the JPL Research and Technology Development Fund, and by NASA Grants No. 06-ARPA206-0040, No. 10-SAT10-0017, No. 12-SAT12-0031, No. 14-SAT14-0009, and No. 16-SAT-16-0002. The development and testing of focal planes were supported by the Gordon and Betty Moore Foundation at Caltech. Readout electronics were supported by a Canada Foundation for Innovation grant to UBC. Support for quasioptical filtering was provided by UK STFC Grant No. ST/N000706/1. The computations in this Letter were run on the Odyssey/Cannon cluster supported by the FAS Science Division Research Computing Group at Harvard University. The analysis effort at Stanford and S. L. A. C. is partially supported by the U.S. DOE Office of Science. We thank the staff of the U.S. Antarctic Program and in particular the South Pole Station without whose help this research would not have been possible. Most special thanks go to our heroic winter-overs Robert Schwarz, Steffen Richter, Sam Harrison, Grantland Hall, and Hans Boenish. We thank all those who have contributed past efforts to the BICEP/Keck series of experiments, including the BICEP1 team. We also thank the Planck and WMAP teams for the use of their data, and are grateful to the Planck team for helpful discussions.Attached Files
Published - PhysRevLett.127.151301.pdf
Submitted - 2110.00483.pdf
Supplemental Material - prl_supp.pdf
Files
Additional details
- Alternative title
- BICEP/Keck XIII: Improved Constraints on Primordial Gravitational Waves using Planck, WMAP, and BICEP/Keck Observations through the 2018 Observing Season
- Eprint ID
- 111176
- Resolver ID
- CaltechAUTHORS:20211004-183512532
- OPP-0742818
- NSF
- OPP-0742592
- NSF
- OPP-1044978
- NSF
- PLR-1110087
- NSF
- OPP-1145172
- NSF
- OPP-1145143
- NSF
- OPP-1145248
- NSF
- OPP-1639040
- NSF
- OPP-1638957
- NSF
- OPP-1638978
- NSF
- OPP-1638970
- NSF
- W. M. Keck Foundation
- JPL Research and Technology Development Fund
- 06-ARPA206-0040
- NASA
- 10-SAT10-0017
- NASA
- 12-SAT12-0031
- NASA
- 14-SAT14-0009
- NASA
- 16-SAT-16-0002
- NASA
- Gordon and Betty Moore Foundation
- Canada Foundation for Innovation
- ST/N000706/1
- Science and Technology Facilities Council (STFC)
- Harvard University
- Department of Energy (DOE)
- Created
-
2021-10-04Created from EPrint's datestamp field
- Updated
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2023-03-16Created from EPrint's last_modified field
- Caltech groups
- Astronomy Department