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A Measurement of the Cosmic Microwave Background B-mode Polarization Power Spectrum at Subdegree Scales from Two Years of polarbear Data

  • Author(s): Ade, PAR
  • Aguilar, M
  • Akiba, Y
  • Arnold, K
  • Baccigalupi, C
  • Barron, D
  • Beck, D
  • Bianchini, F
  • Boettger, D
  • Borrill, J
  • Chapman, S
  • Chinone, Y
  • Crowley, K
  • Cukierman, A
  • Dünner, R
  • Dobbs, M
  • Ducout, A
  • Elleflot, T
  • Errard, J
  • Fabbian, G
  • Feeney, SM
  • Feng, C
  • Fujino, T
  • Galitzki, N
  • Gilbert, A
  • Goeckner-Wald, N
  • Groh, JC
  • Hall, G
  • Halverson, N
  • Hamada, T
  • Hasegawa, M
  • Hazumi, M
  • Hill, CA
  • Howe, L
  • Inoue, Y
  • Jaehnig, G
  • Jaffe, AH
  • Jeong, O
  • Kaneko, D
  • Katayama, N
  • Keating, B
  • Keskitalo, R
  • Kisner, T
  • Krachmalnicoff, N
  • Kusaka, A
  • Jeune, ML
  • Lee, AT
  • Leitch, EM
  • Leon, D
  • Linder, E
  • Lowry, L
  • Matsuda, F
  • Matsumura, T
  • Minami, Y
  • Montgomery, J
  • Navaroli, M
  • Nishino, H
  • Paar, H
  • Peloton, J
  • Pham, ATP
  • Poletti, D
  • Puglisi, G
  • Reichardt, CL
  • Richards, PL
  • Ross, C
  • Segawa, Y
  • Sherwin, BD
  • Silva-Feaver, M
  • Siritanasak, P
  • Stebor, N
  • Stompor, R
  • Suzuki, A
  • Tajima, O
  • Takakura, S
  • et al.
Abstract

© 2017. The American Astronomical Society. All rights reserved. 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 Cold Dark Matter (ΛCDM) framework by fitting for a single lensing amplitude parameter A L = 0.60 +0.26-0.24(stat)+0.00-0.04 (inst) ± 0.14(foreground) ± 0.04(multi), where A L = 1 relative to the Planck 2015 best-fit model prediction. We obtain ±0.14(foreground) ±0.04(multi), where is the fiducial ΛCDM value.

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