Journal article
A Measurement of the Degree-scale CMB B-mode Angular Power Spectrum with POLARBEAR
S Adachi, MAO Aguilar Faundez, K Arnold, C Baccigalupi, D Barron, D Beck, S Beckman, F Bianchini, D Boettger, J Borrill, J Carron, S Chapman, K Cheung, Y Chinone, K Crowley, A Cukierman, M Dobbs, H El Bouhargani, T Elleflot, J Errard Show all
Astrophysical Journal | American Astronomical Society | Published : 2020
Abstract
The American Astronomical Society. All rights reserved. We present a measurement of the B-mode polarization power spectrum of the cosmic microwave background (CMB) using data taken from 2014 July to 2016 December with the Polarbear experiment. The CMB power spectra are measured using observations at 150 GHz with an instantaneous array sensitivity of NETarray=23μ K√s on a 670 square degree patch of sky centered at (R.A., decl.) = (+0h12m0s, -59°18′). A continuously rotating half-wave plate is used to modulate polarization and to suppress low-frequency noise. We achieve 32 μK arcmin effective polarization map noise with a knee in sensitivity of ℓ = 90, where the inflationary gravitational-wave..
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Grants
Awarded by National Science Foundation
Awarded by Moore Foundation
Awarded by Simons Foundation
Awarded by Templeton Foundation
Awarded by JSPS KAKENHI
Awarded by European Research Council under the European Union's Seventh Framework Programme (FP/2007-2013)/ERC grant
Awarded by UK STFC
Awarded by CONICYT UC Berkeley-Chile Seed grant (CLAS fund)
Awarded by Fondecyt
Awarded by Australian Research Council's Future Fellowship
Awarded by U.S. Department of Energy, Office of Science, Office of High Energy Physics
Awarded by Office of Science of the U.S. Department of Energy
Funding Acknowledgements
The POLARBEAR project is funded by the National Science Foundation under grants AST-0618398 and AST-1212230. The analysis presented here was also supported by Moore Foundation grant number 4633, the Simons Foundation grant number 034079, and the Templeton Foundation grant number 58724. The James Ax Observatory operates in the Parque Astronomico Atacama in Northern Chile under the auspices of the Comision Nacional de Investigacion Cientifica y Tecnologica de Chile (CONICYT). A. K. acknowledges support by JSPS Leading Initiative for Excellent Young Researchers (LEADER) and by JSPS KAKENHI grants No. JP16K21744 and 18H05539. C.B., N.K., and D.P. acknowledge support from the ASI-COSMOS Network (cosmosnet.it) and from the INDARK INFN Initiative (web.infn.it/CSN4/IS/Linea5/InDark). G.F. acknowledges the support of the European Research Council under the European Union's Seventh Framework Programme (FP/2007-2013)/ERC grant Agreement No. [616170] and of the UK STFC grant ST/P000525/1. H.N. acknowledges JSPS KAKENHI grant JP26800125. J.C. is supported by the European Research Council under the European Union's Seventh Framework Programme (FP/2007-2013)/ERC grant Agreement No. [616170]. M.A. acknowledges support from CONICYT UC Berkeley-Chile Seed grant (CLAS fund) Number 77047, and Fondecyt projects 1130777 and 1171811, the DFI postgraduate scholarship program, and the DFI Postgraduate Competitive Fund for Support in the Attendance to Scientific Events. M.D. acknowledges funding from the Natural Sciences and Engineering Research Council of Canada and Canadian Institute for Advanced Research. M.H. acknowledges the support from the JSPS KAKENHI grants No. JP26220709 and JP15H05891. N.K. acknowledges the support from JSPS Coreto-Core Program, A. Advanced Research Networks. O.T. acknowledges a SPIRITS grant from the Kyoto University, and JSPS KAKENHI JP26105519. S.T. was supported by a Grant-inAid for JSPS Research Fellow JP14J01662 and JP18J02133. Y.C. acknowledges support from JSPS KAKENHI grants No. 18K13558, 18H04347, 19H00674. The APC group acknowledges travel support from the Labex Univearths grant. The Melbourne group acknowledges support from the University of Melbourne and an Australian Research Council's Future Fellowship (FT150100074). This work was supported by the World Premier International Research Center Initiative (WPI), MEXT, Japan. This research used resources of the Central Computing System, owned and operated by the Computing Research Center at KEK. Support from the Ax Center for Experimental Cosmology at UC San Diego is gratefully acknowledged. Work at LBNL is supported in part by the U.S. Department of Energy, Office of Science, Office of High Energy Physics, under contract No. DE-AC02-05CH11231. This research used resources of the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. We acknowledge many useful conversations with Nathan Whitehorn. We also acknowledge the use of the emcee package (Foreman-Mackey et al. 2013). Some of the results in this paper have been derived using the HEALPix (Gorski et al. 2005) package.