Journal article

A Measurement of the CMB E-mode Angular Power Spectrum at Subdegree Scales from 670 Square Degrees of POLARBEAR Data

S Adachi, MAO Aguilar Faundez, K Arnold, C Baccigalupi, D Barron, D Beck, F Bianchini, S Chapman, K Cheung, Y Chinone, K Crowley, M Dobbs, H El Bouhargani, T Elleflot, J Errard, G Fabbian, C Feng, T Fujino, N Galitzki, N Goeckner-Wald Show all

ASTROPHYSICAL JOURNAL | IOP PUBLISHING LTD | Published : 2020

Abstract

We report a measurement of the E-mode polarization power spectrum of the cosmic microwave background (CMB) using 150 GHz data taken from 2014 July to 2016 December with the Polarbear experiment. We reach an effective polarization map noise level of $32\,\mu {\rm{K}}$-$\mathrm{arcmin}$ across an observation area of 670 square degrees. We measure the EE power spectrum over the angular multipole range $500\leqslant {\ell }\lt 3000$, tracing the third to seventh acoustic peaks with high sensitivity. The statistical uncertainty on E-mode bandpowers is ~2.3 $\mu {{\rm{K}}}^{2}$ at ${\ell }\sim 1000$, with a systematic uncertainty of 0.5 $\mu {{\rm{K}}}^{..

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University of Melbourne Researchers

Grants

Awarded by National Science Foundation


Awarded by Moore Foundation


Awarded by Simons Foundation


Awarded by Templeton Foundation


Awarded by Australian Research Council's Future Fellowship


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 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 No. 4633, the Simons Foundation grant No. 034079, and the Templeton Foundation grant No. 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).The Melbourne group acknowledges support from the University of Melbourne and an Australian Research Council's Future Fellowship (FT150100074). A.K. acknowledges the support by JSPS Leading Initiative for Excellent Young Researchers (LEADER) and by the 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. M.A. acknowledges support from CONICYT UC Berkeley-Chile Seed Grant (CLAS fund) Number 77047, Fondecyt project 1130777 and 1171811, DFI postgraduate scholarship program and 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 Core-to-Core Program, A. Advanced Research Networks. O.T. acknowledges the SPIRITS grant in the Kyoto University, and JSPS KAKENHI JP26105519. S.T. was supported by Grant-in-Aid for JSPS Research Fellow JP14J01662 and JP18J02133. Y. C. acknowledges the support from the JSPS KAKENHI grants No. 18K13558, 18H04347, and 19H00674. The APC group acknowledges the travel support from the Labex Univearths grant. 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.