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Erratum: "A Measurement of the Cosmic Microwave Background B-Mode Polarization Power Spectrum at Sub-degree Scales with POLARBEAR" (2014, ApJ, 794, 171)

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Published 2017 October 12 • © 2017. The American Astronomical Society. All rights reserved.
, , Citation The Polarbear Collaboration: P. A. R. Ade et al 2017 ApJ 848 73 DOI 10.3847/1538-4357/aa8c70

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arnold@ucsd.edu

Author affiliations

1 School of Physics and Astronomy, Cardiff University, Cardiff CF10 3XQ, UK

2 The Graduate University for Advanced Studies, Hayama, Miura District, Kanagawa 240-0115, Japan

3 Center for Astrophysics and Space Astronomy, University of Colorado, Boulder, CO 80309, USA

4 Department of Astrophysical and Planetary Sciences, University of Colorado, Boulder, CO 80309, USA

5 Department of Physics, University of California, San Diego, CA 92093-0424, USA; arnold@ucsd.edu

6 Computational Cosmology Center, Lawrence Berkeley National Laboratory, Berkeley, CA 94720, USA

7 Space Sciences Laboratory, University of California, Berkeley, CA 94720, USA

8 Department of Physics and Atmospheric Science, Dalhousie University, Halifax, NS, B3H 4R2, Canada

9 Department of Physics, University of California, Berkeley, CA 94720, USA

10 High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan

11 Physics Department, McGill University, Montreal, QC H3A 0G4, Canada

12 AstroParticule et Cosmologie, Univ Paris Diderot, CNRS/IN2P3, CEA/Irfu, Obs de Paris, Sorbonne Paris Cité, France

13 International School for Advanced Studies (SISSA), Trieste 34014, Italy

14 Department of Physics, Columbia University, New York, NY 10027, USA

15 Rutherford Appleton Laboratory, STFC, Swindon, SN2 1SZ, United Kingdom

16 Department of Physics, University of Colorado, Boulder, CO 80309, USA

17 Kavli Institute for the Physics and Mathematics of the Universe (WPI), Todai Institutes for Advanced Study, The University of Tokyo, Kashiwa, Chiba 277-8583, Japan

18 Department of Physics, University of Oxford, Oxford OX1 2JD, UK

19 Physics Department, Austin College, Sherman, TX 75090, USA

20 Department of Physics, Imperial College London, London SW7 2AZ, UK

21 Department of Physics, Princeton University, Princeton, NJ 08544, USA

22 Physics Division, Lawrence Berkeley National Laboratory, Berkeley, CA 94720, USA

23 Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637, USA

24 Kavli Institute for Cosmological Physics, University of Chicago, Chicago, IL 60637, USA

25 Department of Physics and Astronomy, University of Pennsylvania, Philadelphia, PA 19104-6396, USA

26 Observational Cosmology Laboratory, Code 665, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA

27 Physics Department, Napa Valley College, Napa, CA 94558, USA

28 Department of Electrical and Computer Engineering, University of California, San Diego, CA 92093, USA

29 Miller Institute for Basic Research in Science, University of California, Berkeley, CA 94720, USA

30 Department of Physics and Astronomy, University of California, Irvine, CA 92697-4575, USA

31 School of Physics and Astronomy, Tel Aviv University, Tel Aviv 69978, Israel

32 Three-Speed Logic, Inc., Vancouver, B.C., V6A 2J8, Canada

33 Osaka University, Toyonaka, Osaka 560-0043, Japan

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Dates

  1. Received 2017 September 7
  2. Accepted 2017 September 11
  3. Published

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In preparing our second-season results, we found a simple mathematical error in our calculation of the upper bound for contamination by synchrotron radiation. In this erratum, we do not include any new foreground information, we simply fix the calculation error. This has the effect of changing the confidence of the rejection of no B-mode polarization power from gravitational lensing from 97.2% to 97.1%. Note that, to the precision reported in number of σ, this does not affect the significance of the Polarbear B-mode measurement.

There are four places where this affects the text of the paper.

  • 1.  
    The sentence in the abstract "Including both systematic and statistical uncertainties, the hypothesis of no B-mode polarization power from gravitational lensing is rejected at 97.2% confidence." should read as follows. "Including both systematic and statistical uncertainties, the hypothesis of no B-mode polarization power from gravitational lensing is rejected at 97.1% confidence."
  • 2.  
    In Table 4, the upper bound for contamination by synchrotron radiation should be changed; the corrected values are shown in Table 4 here.
  • 3.  
    The second to last sentence of Section 8 should be changed from "The measurement rejects the hypothesis of no ${C}_{{\ell }}^{{BB}}$ from lensing with a confidence of 97.2%" to read as follows. "The measurement rejects the hypothesis of no ${C}_{{\ell }}^{{BB}}$ from lensing with a confidence of 97.1%."
  • 4.  
    In the summary of the reported Polarbear systematic uncertainties, presented in Table 9, the row for synchrotron should be changed, as shown in the corrected Table 9 here. Note that the total is unchanged, to the precision shown here.

Table 4.  Sources of Foreground Power and Their Predicted Power in ${\ell }({\ell }+1){C}_{{\ell }}^{{BB}}/2\pi $

Foreground Predicted power in ${\ell }({\ell }+1){C}_{{\ell }}^{{BB}}/2\pi $
  (${10}^{-4}$ $\mu {{\rm{K}}}^{2}$)
  500–900 900–1300 1300–1700 1700–2100
Galactic dust 40 28 22 9.7
Galactic synchrotron 2.3 1.8 1.6 1.4
Radio galaxies 6.3 15 28 46
Dusty galaxies 2.8 4.5 6.5 8.7
Total bias 51 49 58 66

Note. All foreground power is small compared to our statistical uncertainties, and we do not subtract it. The total bias on the final line is the linear sum of the individual foreground powers.

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Table 9.  Summary of Possible Contributions to the Amplitude of ABB from Major Sources of Systematic Uncertainty

Type Source of systematics Effect on ABB
Systematic uncertainty: Galactic dust 0.045
astrophysical foreground Galactic synchrotron 0.003
  Radio galaxies 0.011
  Dusty galaxies 0.004
Systematic uncertainty: Differential & Boresight pointing 0.017
instrument Instrument & relative polarization angle 0.014
  Pixel-pair relative gain: HWP-independent 0.002
  Pixel-pair relative gain: HWP-dependent 0.010
  Pixel-pair relative gain: drift 0.001
  Differential beam ellipticity 0.001
  Differential beam size 0.003
  Electrical crosstalk 0.002
Systematic uncertainty: Scan synchronous template 0.002
analysis E-to-B leakage subtraction 0.006 ± 0.037
  Total 0.121 ± 0.037
Multiplicative effect Statistical variance and beam co-variance ±0.041
  Polarization efficiency ±0.036
  Transfer function ±0.039
  Total ±0.06

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10.3847/1538-4357/aa8c70