Journal article
A Measurement of the Cosmic Microwave Background B-mode Polarization Power Spectrum at Subdegree Scales from Two Years of polarbear Data
PAR Ade, M Aguilar, Y Akiba, K Arnold, C Baccigalupi, D Barron, D Beck, F Bianchini, D Boettger, J Borrill, S Chapman, Y Chinone, K Crowley, A Cukierman, R Dünner, M Dobbs, A Ducout, T Elleflot, J Errard, G Fabbian Show all
Astrophysical Journal | IOP Publishing Ltd | Published : 2017
Abstract
We report an improved measurement of the cosmic microwave background B-mode polarization power spectrum with the Polarbear experiment at 150 GHz. By adding new data collected during the second season of observations (2013-2014) to re-analyzed data from the first season (2012-2013), we have reduced twofold the band-power uncertainties. The band powers are reported over angular multipoles 500 ≤ ℓ ≤ 2100, where the dominant B-mode signal is expected to be due to the gravitational lensing of E-modes. We reject the null hypothesis of no B-mode polarization at a confidence of 3.1σ including both statistical and systematic uncertainties. We test the consistency of the measured B-modes with the Λ Co..
View full abstractRelated Projects (2)
Grants
Awarded by Comisión Nacional de Investigación Científica y Tecnológica
Funding Acknowledgements
J.P. acknowledges support from the Science and Technology Facilities Council (grant number ST/L000652/1) and from the European Research Council under the European Union's Seventh Framework Programme (FP/2007-2013)/ERC Grant Agreement No. [616170]. The POLARBEAR project is funded by the National Science Foundation under grants No. AST-0618398 and No. AST-1212230. 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). This research used resources of the Central Computing System, owned and operated by the Computing Research Center at KEK, the HPCI system (Project ID: hp150132), and the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility supported by the Office of Science of the U.S. Department of Energy under contract No. DE-AC02-05CH11231. In Japan, this work was supported by MEXT KAKENHI grant Nos. JP15H05891 and 21111002, and JSPS KAKENHI grant Nos. JP26220709, JP24111715, and JP26800125. This work was supported by World Premier International Research Center Initiative (WPI), MEXT, Japan. This work was supported by JSPS Core-to-Core Program. In Italy, this work was supported by the RADIOFORE-GROUNDS grant of the European Union's Horizon 2020 research and innovation programme (COMPET-05-2015, grant agreement number 687312) as well as by the INDARK INFN Initiative. The McGill authors acknowledge funding from the Natural Sciences and Engineering Research Council of Canada and the Canadian Institute for Advanced Research. J.P. acknowledges support from the Science and Technology Facilities Council (grant number ST/L000652/1) and from the European Research Council under the European Union's Seventh Framework Programme (FP/2007-2013)/ERC Grant Agreement No. [616170]. G.F. acknowledges support from the CNES postdoctoral program. D.B. acknowledges support from NSF grant AST-1501422. D.B. acknowledges support from FONDECYT postdoctoral grant number 3150504. C.F. acknowledges support from grants HST-AR-13886.001-A, IGPP LANL 368641, NASA NNX16AF39G, and the Ax Foundation for Cosmology at UC Irvine. C.R. acknowledges support from an Australian Research Council's Future Fellowship (FT150100074). M.A. acknowledges support from CONICYT UC Berkeley-Chile Seed Grant (CLAS fund) Number 77047, Fondecyt Project 1130777, the DFI Postgraduate Scholarship Program, and the DFI Postgraduate Competitive Fund for Support in the Attendance to Scientific Events. R.D. acknowledges support from CONICYT grants FONDECYT 1141113, QUIMAL 160009, and Anillo ACT-1417. S.T. was supported by a Grant-in-Aid for JSPS Research Fellow.