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Improved upper limit on degree-scale CMB B-mode polarization power from the 670 square-degree POLARBEAR survey

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DOIResolve DOI: https://doi.org/10.3847/1538-4357/ac6809
AuthorSearch for: ORCID identifier: https://orcid.org/0000-0002-0400-7555; Search for: ORCID identifier: https://orcid.org/0000-0002-3850-9553; Search for: ORCID identifier: https://orcid.org/0000-0002-1571-663X; Search for: ORCID identifier: https://orcid.org/0000-0002-3407-5305; Search for: ORCID identifier: https://orcid.org/0000-0002-8211-1630; Search for: ORCID identifier: https://orcid.org/0000-0002-1623-5651; Search for: 1ORCID identifier: https://orcid.org/0000-0002-8487-3153; Search for: ORCID identifier: https://orcid.org/0000-0002-7764-378X; Search for: ORCID identifier: https://orcid.org/0000-0002-3266-857X; Search for: ORCID identifier: https://orcid.org/0000-0001-5068-1295; Search for: ORCID identifier: https://orcid.org/0000-0002-5166-5614; Search for: ORCID identifier: https://orcid.org/0000-0002-1419-0031; Search for: ORCID identifier: https://orcid.org/0000-0002-3255-4695; Search for: ORCID identifier: https://orcid.org/0000-0001-7438-5896; Search for: ORCID identifier: https://orcid.org/0000-0002-1211-7850; Search for: ORCID identifier: https://orcid.org/0000-0001-7225-6679; Search for: ORCID identifier: https://orcid.org/0000-0003-2606-9340; Search for: ORCID identifier: https://orcid.org/0000-0003-1443-1082; Search for: ORCID identifier: https://orcid.org/0000-0001-6830-8309; Search for: ; Search for: ORCID identifier: https://orcid.org/0000-0003-1887-5860; Search for: ; Search for: ORCID identifier: https://orcid.org/0000-0001-5893-7697; Search for: ORCID identifier: https://orcid.org/0000-0003-3917-086X; Search for: ; Search for: ORCID identifier: https://orcid.org/0000-0003-3118-5514; Search for: ORCID identifier: https://orcid.org/0000-0003-3510-7134; Search for: ORCID identifier: https://orcid.org/0000-0002-5501-8449; Search for: ; Search for: ORCID identifier: https://orcid.org/0000-0003-3106-3218; Search for: ORCID identifier: https://orcid.org/0000-0001-5536-9241; Search for: ORCID identifier: https://orcid.org/0000-0003-1200-9179; Search for: ; Search for: ORCID identifier: https://orcid.org/0000-0003-0041-6447; Search for: ORCID identifier: https://orcid.org/0000-0001-9002-0686; Search for: ORCID identifier: https://orcid.org/0000-0003-2176-8089; Search for: ORCID identifier: https://orcid.org/0000-0003-4394-4645; Search for: ORCID identifier: https://orcid.org/0000-0003-0738-3369; Search for: ORCID identifier: https://orcid.org/0000-0001-9204-3611; Search for: ORCID identifier: https://orcid.org/0000-0001-9807-3758; Search for: ORCID identifier: https://orcid.org/0000-0003-2226-9169; Search for: ; Search for: ; Search for: ORCID identifier: https://orcid.org/0000-0001-6830-1537; Search for: ORCID identifier: https://orcid.org/0000-0002-9777-3813; Search for: ORCID identifier: https://orcid.org/0000-0001-8101-468X; Search for: ; Search for: ORCID identifier: https://orcid.org/0000-0001-9461-7519; Search for: ; Search for: ; Search for: ; Search for: ORCID identifier: https://orcid.org/0000-0003-0221-2130; Search for: ORCID identifier: https://orcid.org/0000-0002-5878-4237
Affiliation
  1. National Research Council of Canada. Herzberg Astronomy and Astrophysics
FormatText, Article
Subjectcosmic microwave background radiation; observational cosmology; cosmological parameters; cosmic inflation
Abstract
We report an improved measurement of the degree-scale cosmic microwave background B-mode angular-power spectrum over 670 deg² sky area at 150 GHz with Polarbear. In the original analysis of the data, errors in the angle measurement of the continuously rotating half-wave plate, a polarization modulator, caused significant data loss. By introducing an angle-correction algorithm, the data volume is increased by a factor of 1.8. We report a new analysis using the larger data set. We find the measured B-mode spectrum is consistent with the ΛCDM model with Galactic dust foregrounds. We estimate the contamination of the foreground by cross-correlating our data and Planck 143, 217, and 353 GHz measurements, where its spectrum is modeled as a power law in angular scale and a modified blackbody in frequency. We place an upper limit on the tensor-to-scalar ratio r < 0.33 at 95% confidence level after marginalizing over the foreground parameters.
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PublisherIOP
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  • The Astrophysical Journal 931, no. 2, 101 (27 May 2022).
LanguageEnglish
Peer reviewedYes
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Record identifier4af2ae84-25e4-429c-b94a-74f246dc9d28
Record created2023-12-15
Record modified2023-12-15
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