Self-calibration of BICEP1 three-year data and constraints on astrophysical polarization rotation

被引：60

作者：

Kaufman, J. P. ^{[1
]}

Miller, N. J. ^{[2
]}

Shimon, M. ^{[1
,3
]}

Barkats, D. ^{[4
]}

Bischoff, C. ^{[5
]}

Buder, I. ^{[5
]}

Keating, B. G. ^{[1
]}

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

Ade, P. A. R. ^{[6
]}

Aikin, R. ^{[7
]}

Battle, J. O. ^{[8
]}

Bierman, E. M. ^{[1
]}

Bock, J. J. ^{[7
,8
]}

Chiang, H. C. ^{[9
]}

Dowell, C. D. ^{[8
]}

Duband, L. ^{[10
]}

Filippini, J. ^{[7
]}

Hivon, E. F. ^{[11
]}

Holzapfel, W. L. ^{[12
]}

Hristov, V. V. ^{[7
]}

Jones, W. C. ^{[13
]}

Kernasovskiy, S. S. ^{[14
,15
]}

Kuo, C. L. ^{[14
,15
]}

Leitch, E. M. ^{[16
]}

Mason, P. V. ^{[7
]}

Matsumura, T. ^{[17
]}

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

Ponthieu, N. ^{[18
]}

Pryke, C. ^{[19
]}

Richter, S. ^{[7
]}

Rocha, G. ^{[7
,8
]}

Sheehy, C. ^{[16
]}

Su, M. ^{[20
,21
]}

Takahashi, Y. D. ^{[12
]}

Tolan, J. E. ^{[14
,15
]}

Yoon, K. W. ^{[14
,15
]}

机构：

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

[2] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA

[3] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel

[4] ESO, Joint ALMA Observ, Santiago 19001, Chile

[5] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA

[6] Univ Wales Coll Cardiff, Dept Phys & Astron, Cardiff CF24 3YB, S Glam, Wales

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

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

[9] Univ KwaZulu Natal, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa

[10] Commissariat Energie Atom, SBT, F-38054 Grenoble, France

[11] Inst Astrophys, F-75014 Paris, France

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

[13] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA

[14] Stanford Univ, Palo Alto, CA 94305 USA

[15] Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA

[16] Univ Chicago, Chicago, IL 60637 USA

[17] KEK, High Energy Accelerator Res Org, Tsukuba, Ibaraki 3050801, Japan

[18] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France

[19] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA

[20] MIT, Dept Phys, Cambridge, MA 02139 USA

[21] MIT, Kavli Ctr Astrophys & Space Res, Cambridge, MA 02139 USA

来源：

PHYSICAL REVIEW D | 2014年 / 89卷 / 06期

基金：

美国国家科学基金会;

关键词：

MICROWAVE BACKGROUND POLARIZATION; ANISOTROPY;

D O I：

10.1103/PhysRevD.89.062006

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Cosmic microwave background (CMB) polarimeters aspire to measure the faint B-mode signature predicted to arise from inflationary gravitational waves. They also have the potential to constrain cosmic birefringence, rotation of the polarization of the CMB arising from parity-violating physics, which would produce nonzero expectation values for the CMB's temperature to B-mode correlation (TB) and E-mode to B-mode correlation (EB) spectra. However, instrumental systematic effects can also cause these TB and EB correlations to be nonzero. In particular, an overall miscalibration of the polarization orientation of the detectors produces TB and EB spectra which are degenerate with isotropic cosmological birefringence, while also introducing a small but predictable bias on the BB spectrum. We find that BICEP1 three-year spectra, which use our standard calibration of detector polarization angles from a dielectric sheet, are consistent with a polarization rotation of alpha = -2.77 degrees +/- 0.86 degrees (statistical) +/- 1.3 degrees (systematic). We have revised the estimate of systematic error on the polarization rotation angle from the two-year analysis by comparing multiple calibration methods. We also account for the (negligible) impact of measured beam systematic effects. We investigate the polarization rotation for the BICEP1 100 GHz and 150 GHz bands separately to investigate theoretical models that produce frequency-dependent cosmic birefringence. We find no evidence in the data supporting either of these models or Faraday rotation of the CMB polarization by the Milky Way galaxy's magnetic field. If we assume that there is no cosmic birefringence, we can use the TB and EB spectra to calibrate detector polarization orientations, thus reducing bias of the cosmological B-mode spectrum from leaked E-modes due to possible polarization orientation miscalibration. After applying this "self-calibration" process, we find that the upper limit on the tensor-to-scalar ratio decreases slightly, from r < 0.70 to r < 0.65 at 95% confidence.

引用

页数：11

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