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Bicep2/Keck Array V: measurements ofb-mode polarization at degree angular scales and 150 ghz by the Keck Array

Ade, Peter A. R., Ahmed, Z., Aikin, R. W., Alexander, K. D., Barkats, D., Benton, S. J., Bischoff, C. A., Bock, J. J., Brevik, J. A., Buder, I., Bullock, E., Buza, V., Connors, J., Crill, B. P., Dowell, C. D., Dvorkin, C., Duband, L., Filippini, J. P., Fliescher, S., Golwala, S. R., Halpern, M., Harrison, S., Hasselfield, M., Hildebrandt, S. R., Hilton, G. C., Hristov, V. V., Hui, H., Irwin, K. D., Karkare, K. S., Kaufman, J. P., Keating, B. G., Kefeli, S., Kernasovskiy, S. A., Kovac, J. M., Kuo, C. L., Leitch, E. M., Lueker, M., Mason, P., Megerian, K. G., Netterfield, C. B., Nguyen, H. T., O'Brient, R., Ogburn IV, R. W., Orlando, A., Pryke, C., Reintsema, C. D., Richter, S., Schwarz, R., Sheehy, C. D., Staniszewski, Z. K., Sudiwala, Rashmikant, Teply, G. P., Thompson, K. L., Tolan, J. E., Turner, A. D., Vieregg, A. G., Weber, A. C., Willmert, J., Wong, C. L. and Yoon, K. W. 2015. Bicep2/Keck Array V: measurements ofb-mode polarization at degree angular scales and 150 ghz by the Keck Array. The Astrophysical Journal 811 (2) , 126. 10.1088/0004-637X/811/2/126

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Abstract

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-ΛCDM expectation of >5σ 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 μK arcmin) over an effective area of 400 deg2 for an equivalent survey weight of 250,000 μK−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 >6σ.

Item Type: Article
Date Type: Published Online
Status: Published
Schools: Physics and Astronomy
Subjects: Q Science > QB Astronomy
Publisher: IOP Science
ISSN: 1538-4357
Last Modified: 15 Mar 2019 15:11
URI: http://orca-mwe.cf.ac.uk/id/eprint/89755

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