期刊
ASTROPHYSICAL JOURNAL
卷 811, 期 2, 页码 -出版社
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/811/2/126
关键词
cosmic background radiation; cosmology: observations; gravitational waves; inflation; polarization
资金
- National Science Foundation (Harvard) [ANT-1145172]
- Keck Foundation (Caltech)
- NASA APRA program [06-ARPA206-0040, 10-SAT10-0017]
- NASA SAT program [06-ARPA206-0040, 10-SAT10-0017]
- Canada Foundation for Innovation
- National Science Foundation (Minnesota) [ANT-1145143]
- National Science Foundation (Stanford) [ANT-1145248]
- Direct For Mathematical & Physical Scien
- Division Of Physics [1125897] Funding Source: National Science Foundation
- Directorate For Geosciences
- Office of Polar Programs (OPP) [1145172] Funding Source: National Science Foundation
- Directorate For Geosciences
- Office of Polar Programs (OPP) [1145143] Funding Source: National Science Foundation
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [1255358] Funding Source: National Science Foundation
- STFC [ST/K000926/1] Funding Source: UKRI
The Keck Array is a system of cosmic microwave background polarimeters, each similar to the BICEP2 experiment. In this paper we report results from the 2012 to 2013 observing seasons, during which the Keck Array consisted of five receivers all operating in the same (150 GHz) frequency band and observing field as BICEP2. We again find an excess of B-mode power over the lensed-.CDM expectation of >5 sigma in the range 30 < l < 150 and confirm that this is not due to systematics using jackknife tests and simulations based on detailed calibration measurements. In map difference and spectral difference tests these new data are shown to be consistent with BICEP2. Finally, we combine the maps from the two experiments to produce final Q and U maps which have a depth of 57 nK deg (3.4 mu K arcmin) over an effective area of 400 deg(2) for an equivalent survey weight of 250,000 mu K-2. The final BB band powers have noise uncertainty a factor of 2.3 times better than the previous results, and a significance of detection of excess power of >6 sigma.
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