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

被引：30

作者：

Ade, P. A. R. ^{[1
]}

Ahmed, Z. ^{[2
,3
]}

Aikin, R. W. ^{[4
]}

Alexander, K. D. ^{[5
]}

Barkats, D. ^{[5
]}

Benton, S. J. ^{[6
]}

Bischoff, C. A. ^{[7
]}

Bock, J. J. ^{[4
,8
]}

Bowens-Rubin, R. ^{[5
]}

Brevik, J. A. ^{[4
]}

Buder, I. ^{[5
]}

Bullock, E. ^{[9
]}

Buza, V. ^{[5
,10
]}

Connors, J. ^{[5
]}

Crill, B. P. ^{[8
]}

Duband, L. ^{[11
]}

Dvorkin, C. ^{[10
]}

Filippini, J. P. ^{[12
]}

Fliescher, S. ^{[13
]}

Germaine, T. St. ^{[10
]}

Ghosh, T. ^{[4
]}

Grayson, J. ^{[3
]}

Harrison, S. ^{[5
]}

Hildebrandt, S. R. ^{[8
]}

Hilton, G. C.

Hui, H. ^{[4
]}

Irwin, K. D. ^{[2
,3
,14
]}

Kang, J. ^{[2
,3
]}

Karkare, K. S. ^{[5
]}

Karpel, E. ^{[3
]}

Kaufman, J. P. ^{[15
]}

Keating, B. G. ^{[15
]}

Kefeli, S. ^{[4
]}

Kernasovskiy, S. A. ^{[3
]}

Kovac, J. M. ^{[5
,10
]}

Kuo, C. L. ^{[2
,3
]}

Larson, N. ^{[16
]}

Leitch, E. M. ^{[17
]}

Megerian, K. G. ^{[8
]}

Moncelsi, L. ^{[4
]}

Namikawa, T. ^{[2
,3
]}

Netterfield, C. B. ^{[18
]}

Nguyen, H. T. ^{[8
]}

O'Brient, R. ^{[4
,8
]}

Ogburn, R. W. ^{[2
,3
]}

Pryke, C. ^{[9
,13
]}

Richter, S. ^{[5
]}

Schillaci, A. ^{[4
]}

Schwarz, R. ^{[13
]}

Sheehy, C. D. ^{[19
]}

机构：

[1] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales

[2] Kavli Inst Particle Astrophys & Cosmol, SLAC Natl Accelerator Lab, 2575 Sand Hill Rd, Menlo Pk, CA 94025 USA

[3] Stanford Univ, Dept Phys, Stanford, CA 94305 USA

[4] CALTECH, Dept Phys, Pasadena, CA 91125 USA

[5] Harvard Smithsonian Ctr Astrophys, 60 Garden St MS 42, Cambridge, MA 02138 USA

[6] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada

[7] Univ Cincinnati, Dept Phys, Cincinnati, OH 45221 USA

[8] Jet Prop Lab, Pasadena, CA 91109 USA

[9] Univ Minnesota, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA

[10] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA

[11] CEA, Serv Basses Temp, F-38054 Grenoble, France

[12] Univ Illinois, Dept Phys, Urbana, IL 61801 USA

[13] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA

[14] NIST, Boulder, CO 80305 USA

[15] Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA

[16] Univ Chicago, Enrico Fermi Inst, Dept Phys, Chicago, IL 60637 USA

[17] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA

[18] Canadian Inst Adv Res, Toronto, ON M5G 1Z8, Canada

[19] Brookhaven Natl Lab, Upton, NY 11973 USA

[20] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada

[21] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA

来源：

PHYSICAL REVIEW D | 2017年 / 96卷 / 10期

基金：

加拿大创新基金会; 美国国家科学基金会;

关键词：

D O I：

10.1103/PhysRevD.96.102003

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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 (similar to 3 mu K-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(ar) <= 7.2 x 10(-2) / H-1 (95% confidence) than the constraint derived from the B-mode spectrum, where HI is the inflationary Hubble scale. This constraint leads to a limit on the decay constant of 10(-6) less than or similar to f(a) / M-pl at mass range of 10(-33) <= m(a) <= 10(-28) eV for r = 0.01, assuming g(ar) similar to alpha/(2 pi f(a)) with a 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.

引用

页数：7

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