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BICEP2 / Keck Array IX: New bounds on anisotropies of CMB polarization rotation and implications for axionlike particles and primordial magnetic fields

Ade, P. A. R. and Aikin, R. W. and Bock, J. J. and Brevik, J. A. and Filippini, J. P. and Ghosh, T. and Hildebrandt, S. R. and Hui, H. and Kefeli, S. and Moncelsi, L. and O'Brient, R. and Schillaci, A. and Staniszewski, Z. K. and Steinbach, B. (2017) BICEP2 / Keck Array IX: New bounds on anisotropies of CMB polarization rotation and implications for axionlike particles and primordial magnetic fields. Physical Review D, 96 (10). Art. No. 102003. ISSN 2470-0010. https://resolver.caltech.edu/CaltechAUTHORS:20171113-140702052

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Abstract

We present the strongest constraints to date on anisotropies of cosmic microwave background (CMB) polarization rotation derived from 150 GHz data taken by the BICEP2 & Keck Array CMB experiments up to and including the 2014 observing season (BK14). The definition of the polarization angle in BK14 maps has gone through self-calibration in which the overall angle is adjusted to minimize the observed TB and EB power spectra. After this procedure, the QU maps lose sensitivity to a uniform polarization rotation but are still sensitive to anisotropies of polarization rotation. This analysis places constraints on the anisotropies of polarization rotation, which could be generated by CMB photons interacting with axionlike pseudoscalar fields or Faraday rotation induced by primordial magnetic fields. The sensitivity of BK14 maps (∼3  μK−arc min) makes it possible to reconstruct anisotropies of the polarization rotation angle and measure their angular power spectrum much more precisely than previous attempts. Our data are found to be consistent with no polarization rotation anisotropies, improving the upper bound on the amplitude of the rotation angle spectrum by roughly an order of magnitude compared to the previous best constraints. Our results lead to an order of magnitude better constraint on the coupling constant of the Chern-Simons electromagnetic term g_(aγ) ≤ 7.2×10^(−2)/H_I (95% confidence) than the constraint derived from the B-mode spectrum, where H_I is the inflationary Hubble scale. This constraint leads to a limit on the decay constant of 10^(−6) ≲ f_a/M_(pl) at mass range of 10^(−33) ≤ ma ≤ 10^(−28)  eV for r=0.01, assuming g_(aγ) ∼ α/(2πf_a) with α denoting the fine structure constant. The upper bound on the amplitude of the primordial magnetic fields is 30 nG (95% confidence) from the polarization rotation anisotropies.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1103/PhysRevD.96.102003DOIArticle
https://journals.aps.org/prd/abstract/10.1103/PhysRevD.96.102003PublisherArticle
https://arxiv.org/abs/1705.02523arXivDiscussion Paper
ORCID:
AuthorORCID
Ade, P. A. R.0000-0002-5127-0401
Bock, J. J.0000-0002-5710-5212
Moncelsi, L.0000-0002-4242-3015
Alternate Title:BICEP2 / Keck Array IX: New Bounds on Anisotropies of CMB Polarization Rotation and Implications for Axion-Like Particles and Primordial Magnetic Fields
Additional Information:© 2017 American Physical Society. Received 13 May 2017; revised manuscript received 28 June 2017; published 9 November 2017. The Keck Array project has been made possible through support from the National Science Foundation under Grants No. ANT-1145172 (Harvard), No. ANT-1145143 (Minnesota), and No. ANT-1145248 (Stanford) and from the Keck Foundation (Caltech). The development of antenna-coupled detector technology was supported by the JPL Research and Technology Development Fund and Grants No. 06-ARPA206-0040 and No. 10-SAT10-0017 from the NASA APRA and SAT programs. The development and testing of focal planes were supported by the Gordon and Betty Moore Foundation at Caltech. Readout electronics were supported by a Canada Foundation for Innovation grant to UBC. The computations in this paper were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. The analysis effort at Stanford and SLAC is partially supported by the U.S. Department of Energy Office of Science. We thank the staff of the U.S. Antarctic Program and in particular the South Pole Station, without whose help this research would not have been possible. Most special thanks go to our heroic winter-overs Robert Schwarz and Steffen Richter. We thank all those who have contributed past efforts to the BICEP/Keck Array series of experiments, including the BICEP1 team. We thank Chang Feng for providing the histogram data shown in Ref. [31].
Funders:
Funding AgencyGrant Number
NSFANT-1145172
NSFANT-1145143
NSFANT-1145248
W. M. Keck FoundationUNSPECIFIED
JPL Research and Technology Development Fund06-ARPA206-0040
NASA10-SAT10-0017
Gordon and Betty Moore FoundationUNSPECIFIED
Canada Foundation for InnovationUNSPECIFIED
Harvard UniversityUNSPECIFIED
Department of Energy (DOE)UNSPECIFIED
Issue or Number:10
Record Number:CaltechAUTHORS:20171113-140702052
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20171113-140702052
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:83159
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:14 Nov 2017 01:53
Last Modified:03 Oct 2019 19:03

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