Improved Upper Limit on Degree-scale CMB B-mode Polarization Power from the 670 Square-degree POLARBEAR Survey

S. Adachi; T. Adkins; M. A.O. Aguilar Faúndez; K. S. Arnold; C. Baccigalupi; D. Barron; S. Chapman; K. Cheung; Y. Chinone; K. T. Crowley; T. Elleflot; J. Errard; G. Fabbian; C. Feng; T. Fujino; N. Galitzki; N. W. Halverson; M. Hasegawa; M. Hazumi; H. Hirose; L. Howe; J. Ito; O. Jeong; D. Kaneko; N. Katayama; B. Keating; T. Kisner; N. Krachmalnicoff; A. Kusaka; A. T. Lee; E. Linder; A. I. Lonappan; L. N. Lowry; F. Matsuda; T. Matsumura; Y. Minami; M. Murata; H. Nishino; Y. Nishinomiya; D. Poletti; C. L. Reichardt; C. Ross; Y. Segawa; P. Siritanasak; R. Stompor; A. Suzuki; O. Tajima; S. Takakura; S. Takatori; D. Tanabe; G. Teply; K. Yamada; Y. Zhou

doi:10.3847/1538-4357/ac6809

Improved Upper Limit on Degree-scale CMB B-mode Polarization Power from the 670 Square-degree POLARBEAR Survey

S. Adachi, T. Adkins, M. A.O. Aguilar Faúndez, K. S. Arnold, C. Baccigalupi, D. Barron, S. Chapman, K. Cheung, Y. Chinone, K. T. Crowley, T. Elleflot, J. Errard, G. Fabbian, C. Feng, T. Fujino, N. Galitzki, N. W. Halverson, M. Hasegawa, M. Hazumi, H. HiroseL. Howe, J. Ito, O. Jeong, D. Kaneko, N. Katayama, B. Keating, T. Kisner, N. Krachmalnicoff, A. Kusaka, A. T. Lee, E. Linder, A. I. Lonappan, L. N. Lowry, F. Matsuda, T. Matsumura, Y. Minami, M. Murata, H. Nishino, Y. Nishinomiya, D. Poletti, C. L. Reichardt, C. Ross, Y. Segawa, P. Siritanasak, R. Stompor, A. Suzuki, O. Tajima, S. Takakura, S. Takatori, D. Tanabe, G. Teply, K. Yamada, Y. Zhou

Research output: Contribution to journal › Article › peer-review

3 Citations (Scopus)

Abstract

We report an improved measurement of the degree-scale cosmic microwave background B-mode angular-power spectrum over 670 deg2 sky area at 150 GHz with Polarbear. In the original analysis of the data, errors in the angle measurement of the continuously rotating half-wave plate, a polarization modulator, caused significant data loss. By introducing an angle-correction algorithm, the data volume is increased by a factor of 1.8. We report a new analysis using the larger data set. We find the measured B-mode spectrum is consistent with the ΛCDM model with Galactic dust foregrounds. We estimate the contamination of the foreground by cross-correlating our data and Planck 143, 217, and 353 GHz measurements, where its spectrum is modeled as a power law in angular scale and a modified blackbody in frequency. We place an upper limit on the tensor-to-scalar ratio r < 0.33 at 95% confidence level after marginalizing over the foreground parameters.

Original language	English
Article number	101
Journal	Astrophysical Journal
Volume	931
Issue number	2
DOIs	https://doi.org/10.3847/1538-4357/ac6809
Publication status	Published - Jun 1 2022
Externally published	Yes

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.3847/1538-4357/ac6809

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Adachi, S., Adkins, T., Aguilar Faúndez, M. A. O., Arnold, K. S., Baccigalupi, C., Barron, D., Chapman, S., Cheung, K., Chinone, Y., Crowley, K. T., Elleflot, T., Errard, J., Fabbian, G., Feng, C., Fujino, T., Galitzki, N., Halverson, N. W., Hasegawa, M., Hazumi, M., ... Zhou, Y. (2022). Improved Upper Limit on Degree-scale CMB B-mode Polarization Power from the 670 Square-degree POLARBEAR Survey. Astrophysical Journal, 931(2), [101]. https://doi.org/10.3847/1538-4357/ac6809

Adachi, S, Adkins, T, Aguilar Faúndez, MAO, Arnold, KS, Baccigalupi, C, Barron, D, Chapman, S, Cheung, K, Chinone, Y, Crowley, KT, Elleflot, T, Errard, J, Fabbian, G, Feng, C, Fujino, T, Galitzki, N, Halverson, NW, Hasegawa, M, Hazumi, M, Hirose, H, Howe, L, Ito, J, Jeong, O, Kaneko, D, Katayama, N, Keating, B, Kisner, T, Krachmalnicoff, N, Kusaka, A, Lee, AT, Linder, E, Lonappan, AI, Lowry, LN, Matsuda, F, Matsumura, T, Minami, Y, Murata, M, Nishino, H, Nishinomiya, Y, Poletti, D, Reichardt, CL, Ross, C, Segawa, Y, Siritanasak, P, Stompor, R, Suzuki, A, Tajima, O, Takakura, S, Takatori, S, Tanabe, D, Teply, G, Yamada, K & Zhou, Y 2022, 'Improved Upper Limit on Degree-scale CMB B-mode Polarization Power from the 670 Square-degree POLARBEAR Survey', Astrophysical Journal, vol. 931, no. 2, 101. https://doi.org/10.3847/1538-4357/ac6809

@article{ea43c69de8684bd5bc39b23a017adacc,

title = "Improved Upper Limit on Degree-scale CMB B-mode Polarization Power from the 670 Square-degree POLARBEAR Survey",

abstract = "We report an improved measurement of the degree-scale cosmic microwave background B-mode angular-power spectrum over 670 deg2 sky area at 150 GHz with Polarbear. In the original analysis of the data, errors in the angle measurement of the continuously rotating half-wave plate, a polarization modulator, caused significant data loss. By introducing an angle-correction algorithm, the data volume is increased by a factor of 1.8. We report a new analysis using the larger data set. We find the measured B-mode spectrum is consistent with the ΛCDM model with Galactic dust foregrounds. We estimate the contamination of the foreground by cross-correlating our data and Planck 143, 217, and 353 GHz measurements, where its spectrum is modeled as a power law in angular scale and a modified blackbody in frequency. We place an upper limit on the tensor-to-scalar ratio r < 0.33 at 95% confidence level after marginalizing over the foreground parameters.",

author = "S. Adachi and T. Adkins and {Aguilar Fa{\'u}ndez}, {M. A.O.} and Arnold, {K. S.} and C. Baccigalupi and D. Barron and S. Chapman and K. Cheung and Y. Chinone and Crowley, {K. T.} and T. Elleflot and J. Errard and G. Fabbian and C. Feng and T. Fujino and N. Galitzki and Halverson, {N. W.} and M. Hasegawa and M. Hazumi and H. Hirose and L. Howe and J. Ito and O. Jeong and D. Kaneko and N. Katayama and B. Keating and T. Kisner and N. Krachmalnicoff and A. Kusaka and Lee, {A. T.} and E. Linder and Lonappan, {A. I.} and Lowry, {L. N.} and F. Matsuda and T. Matsumura and Y. Minami and M. Murata and H. Nishino and Y. Nishinomiya and D. Poletti and Reichardt, {C. L.} and C. Ross and Y. Segawa and P. Siritanasak and R. Stompor and A. Suzuki and O. Tajima and S. Takakura and S. Takatori and D. Tanabe and G. Teply and K. Yamada and Y. Zhou",

note = "Funding Information: The P olarbear 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 Astron{\'o}mico Atacama in Northern Chile under the auspices of the Comisi{\'o}n Nacional de Investigaci{\'o}n Cient{\'i}fica y Tecnol{\'o}gica de Chile (CONICYT). 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. In Japan, this work was supported by MEXT KAKENHI grant Nos. JP21111002, JP15H05891, JP18H05539, and JP18H04362, JSPS KAKENHI grant Nos. JP26220709, JP26800125, JP14J01662, JP16K21744, JP17K18785, JP18H01240, JP18J02133, JP18K13558, JP19H00674, JP19KK0079, JP20H01921, JP20K14481, JP20K14497, JP21K03585, and the JSPS Core-to-Core Program. This research used resources of the Central Computing System, owned and operated by the Computing Research Center at KEK. This work was supported by the World Premier International Research Center Initiative (WPI), MEXT, Japan. Support from the Ax Center for Experimental Cosmology at UC San Diego is gratefully acknowledged. The SISSA group acknowledges the INDARK INFN Initiative and the COSMOS and LiteBIRD networks of the Italian Space Agency (cosmosnet.it). The Melbourne group acknowledges support from the Australian Research Council's Discovery Projects scheme (DP210102386). The Dalhousie group acknowledges support from the Natural Sciences and Engineering Research Council (NSERC) and Canada Foundation for Innovation (CFI). M.A. acknowledges support from CONICYT UC Berkeley-Chile Seed Grant (CLAS fund) Number 77047, Fondecyt project 1130777 and 1171811, the DFI postgraduate scholarship program and the DFI Postgraduate Competitive Fund for Support in the Attendance to Scientific Events. G.F. acknowledges the support of the European Research Council under the Marie Sk{\l}odowska Curie actions through the Individual Global Fellowship No. 892401 PiCOGAMBAS. D.P. acknowledges support from the COSMOS Network from the Italian Space Agency. Publisher Copyright: {\textcopyright} 2022. The Author(s). Published by the American Astronomical Society.",

year = "2022",

month = jun,

day = "1",

doi = "10.3847/1538-4357/ac6809",

language = "English",

volume = "931",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "IOP Publishing Ltd.",

number = "2",

}

TY - JOUR

T1 - Improved Upper Limit on Degree-scale CMB B-mode Polarization Power from the 670 Square-degree POLARBEAR Survey

AU - Adachi, S.

AU - Adkins, T.

AU - Aguilar Faúndez, M. A.O.

AU - Arnold, K. S.

AU - Baccigalupi, C.

AU - Barron, D.

AU - Chapman, S.

AU - Cheung, K.

AU - Chinone, Y.

AU - Crowley, K. T.

AU - Elleflot, T.

AU - Errard, J.

AU - Fabbian, G.

AU - Feng, C.

AU - Fujino, T.

AU - Galitzki, N.

AU - Halverson, N. W.

AU - Hasegawa, M.

AU - Hazumi, M.

AU - Hirose, H.

AU - Howe, L.

AU - Ito, J.

AU - Jeong, O.

AU - Kaneko, D.

AU - Katayama, N.

AU - Keating, B.

AU - Kisner, T.

AU - Krachmalnicoff, N.

AU - Kusaka, A.

AU - Lee, A. T.

AU - Linder, E.

AU - Lonappan, A. I.

AU - Lowry, L. N.

AU - Matsuda, F.

AU - Matsumura, T.

AU - Minami, Y.

AU - Murata, M.

AU - Nishino, H.

AU - Nishinomiya, Y.

AU - Poletti, D.

AU - Reichardt, C. L.

AU - Ross, C.

AU - Segawa, Y.

AU - Siritanasak, P.

AU - Stompor, R.

AU - Suzuki, A.

AU - Tajima, O.

AU - Takakura, S.

AU - Takatori, S.

AU - Tanabe, D.

AU - Teply, G.

AU - Yamada, K.

AU - Zhou, Y.

N1 - Funding Information: The P olarbear 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 Astronómico Atacama in Northern Chile under the auspices of the Comisión Nacional de Investigación Científica y Tecnológica de Chile (CONICYT). 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. In Japan, this work was supported by MEXT KAKENHI grant Nos. JP21111002, JP15H05891, JP18H05539, and JP18H04362, JSPS KAKENHI grant Nos. JP26220709, JP26800125, JP14J01662, JP16K21744, JP17K18785, JP18H01240, JP18J02133, JP18K13558, JP19H00674, JP19KK0079, JP20H01921, JP20K14481, JP20K14497, JP21K03585, and the JSPS Core-to-Core Program. This research used resources of the Central Computing System, owned and operated by the Computing Research Center at KEK. This work was supported by the World Premier International Research Center Initiative (WPI), MEXT, Japan. Support from the Ax Center for Experimental Cosmology at UC San Diego is gratefully acknowledged. The SISSA group acknowledges the INDARK INFN Initiative and the COSMOS and LiteBIRD networks of the Italian Space Agency (cosmosnet.it). The Melbourne group acknowledges support from the Australian Research Council's Discovery Projects scheme (DP210102386). The Dalhousie group acknowledges support from the Natural Sciences and Engineering Research Council (NSERC) and Canada Foundation for Innovation (CFI). M.A. acknowledges support from CONICYT UC Berkeley-Chile Seed Grant (CLAS fund) Number 77047, Fondecyt project 1130777 and 1171811, the DFI postgraduate scholarship program and the DFI Postgraduate Competitive Fund for Support in the Attendance to Scientific Events. G.F. acknowledges the support of the European Research Council under the Marie Skłodowska Curie actions through the Individual Global Fellowship No. 892401 PiCOGAMBAS. D.P. acknowledges support from the COSMOS Network from the Italian Space Agency. Publisher Copyright: © 2022. The Author(s). Published by the American Astronomical Society.

PY - 2022/6/1

Y1 - 2022/6/1

N2 - We report an improved measurement of the degree-scale cosmic microwave background B-mode angular-power spectrum over 670 deg2 sky area at 150 GHz with Polarbear. In the original analysis of the data, errors in the angle measurement of the continuously rotating half-wave plate, a polarization modulator, caused significant data loss. By introducing an angle-correction algorithm, the data volume is increased by a factor of 1.8. We report a new analysis using the larger data set. We find the measured B-mode spectrum is consistent with the ΛCDM model with Galactic dust foregrounds. We estimate the contamination of the foreground by cross-correlating our data and Planck 143, 217, and 353 GHz measurements, where its spectrum is modeled as a power law in angular scale and a modified blackbody in frequency. We place an upper limit on the tensor-to-scalar ratio r < 0.33 at 95% confidence level after marginalizing over the foreground parameters.

AB - We report an improved measurement of the degree-scale cosmic microwave background B-mode angular-power spectrum over 670 deg2 sky area at 150 GHz with Polarbear. In the original analysis of the data, errors in the angle measurement of the continuously rotating half-wave plate, a polarization modulator, caused significant data loss. By introducing an angle-correction algorithm, the data volume is increased by a factor of 1.8. We report a new analysis using the larger data set. We find the measured B-mode spectrum is consistent with the ΛCDM model with Galactic dust foregrounds. We estimate the contamination of the foreground by cross-correlating our data and Planck 143, 217, and 353 GHz measurements, where its spectrum is modeled as a power law in angular scale and a modified blackbody in frequency. We place an upper limit on the tensor-to-scalar ratio r < 0.33 at 95% confidence level after marginalizing over the foreground parameters.

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UR - http://www.scopus.com/inward/citedby.url?scp=85131670072&partnerID=8YFLogxK

U2 - 10.3847/1538-4357/ac6809

DO - 10.3847/1538-4357/ac6809

M3 - Article

AN - SCOPUS:85131670072

SN - 0004-637X

VL - 931

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 2

M1 - 101

ER -

Improved Upper Limit on Degree-scale CMB B-mode Polarization Power from the 670 Square-degree POLARBEAR Survey

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