SECOND SEASON QUIET OBSERVATIONS: MEASUREMENTS OF THE COSMIC MICROWAVE BACKGROUND POLARIZATION POWER SPECTRUM AT 95 GHz

被引：71

作者：

Araujo, D. ^{[1
]}

Bischoff, C. ^{[3
,4
]}

Brizius, A. ^{[3
,5
]}

Buder, I. ^{[3
,4
]}

Chinone, Y. ^{[6
,7
]}

Cleary, K. ^{[8
]}

Dumoulin, R. N. ^{[1
,2
]}

Kusaka, A. ^{[3
,9
]}

Monsalve, R. ^{[10
,11
]}

Kaess, S. ^{[12
]}

Newburgh, L. B. ^{[1
,2
,9
]}

Reeves, R. ^{[8
]}

Wehus, I. K. ^{[13
,14
]}

Zwart, J. T. L. ^{[1
,2
,15
]}

Bronfman, L. ^{[16
]}

Bustos, R. ^{[10
,16
,17
]}

Church, S. E. ^{[18
,19
]}

Dickinson, C. ^{[20
]}

Eriksen, H. K. ^{[12
,21
]}

Gaier, T. ^{[22
]}

Gundersen, J. O. ^{[10
]}

Hasegawa, M. ^{[6
]}

Hazumi, M. ^{[6
]}

Huffenberger, K. M. ^{[10
]}

Ishidoshiro, K. ^{[6
]}

Jones, M. E. ^{[13
]}

Kangaslahti, P. ^{[22
]}

Kapner, D. J. ^{[3
,23
]}

Kubik, D. ^{[24
]}

Lawrence, C. R. ^{[22
]}

Limon, M. ^{[1
,2
]}

McMahon, J. J. ^{[25
]}

Miller, A. D. ^{[1
,2
]}

Nagai, M. ^{[6
]}

Nguyen, H. ^{[24
]}

Nixon, G. ^{[9
,26
]}

Pearson, T. J. ^{[8
]}

Piccirillo, L. ^{[20
]}

Radford, S. J. E. ^{[8
]}

Readhead, A. C. S. ^{[8
]}

Richards, J. L. ^{[8
]}

Samtleben, D. ^{[5
,27
]}

Seiffert, M. ^{[22
]}

Shepherd, M. C. ^{[8
]}

Smith, K. M. ^{[3
,9
]}

Staggs, S. T. ^{[9
]}

Tajima, O. ^{[3
,6
]}

Thompson, K. L. ^{[18
,19
]}

Vanderlinde, K. ^{[3
,28
]}

Williamson, R. ^{[1
,2
,3
]}

机构：

[1] Columbia Univ, Dept Phys, New York, NY 10027 USA

[2] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA

[3] Univ Chicago, Dept Phys, Kavli Inst Cosmol Phys, Enrico Fermi Inst, Chicago, IL 60637 USA

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

[5] Max Planck Inst Radioastron, D-53121 Bonn, Germany

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

[7] Tohoku Univ, Grad Sch Sci, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan

[8] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA

[9] Princeton Univ, Joseph Henry Labs Phys, Princeton, NJ 08544 USA

[10] Univ Miami, Dept Phys, Coral Gables, FL 33146 USA

[11] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA

[12] Univ Oslo, Inst Theoret Astrophys, NO-0315 Oslo, Norway

[13] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England

[14] Univ Oslo, Dept Phys, NO-0316 Oslo, Norway

[15] Univ Western Cape, Dept Phys, ZA-7535 Bellville, South Africa

[16] Univ Chile, Dept Astron, Santiago, Chile

[17] Univ Concepcion, Dept Astron, Concepcion, Chile

[18] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA

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

[20] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England

[21] Univ Oslo, Ctr Math Applicat, NO-0316 Oslo, Norway

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

[23] Micro Encoder Inc, Kirkland, WA 98034 USA

[24] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA

[25] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA

[26] Tradeworx Inc, Red Bank, NJ 07701 USA

[27] Nikhef, Amsterdam, Netherlands

[28] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada

来源：

ASTROPHYSICAL JOURNAL | 2012年 / 760卷 / 02期

基金：

美国国家科学基金会;

关键词：

cosmic background radiation; cosmology: observations; gravitational waves; inflation; polarization; GRAVITY-WAVES; PROBE; CONSTRAINTS; TEMPERATURE;

D O I：

10.1088/0004-637X/760/2/145

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The Q/U Imaging ExperimenT (QUIET) has observed the cosmic microwave background (CMB) at 43 and 95 GHz. The 43 GHz results have been published in a previous paper, and here we report the measurement of CMB polarization power spectra using the 95 GHz data. This data set comprises 5337 hr of observations recorded by an array of 84 polarized coherent receivers with a total array sensitivity of 87 mu K root s. Four low-foreground fields were observed, covering a total of similar to 1000 deg(2) with an effective angular resolution of 12.'8, allowing for constraints on primordial gravitational waves and high signal-to-noise measurements of the E-modes across three acoustic peaks. The data reduction was performed using two independent analysis pipelines, one based on a pseudo-C-l (PCL) cross-correlation approach, and the other on a maximum-likelihood (ML) approach. All data selection criteria and filters were modified until a predefined set of null tests had been satisfied before inspecting any non-null power spectrum. The results derived by the two pipelines are in good agreement. We characterize the EE, EB, and BB power spectra between l = 25 and 975 and find that the EE spectrum is consistent with Lambda CDM, while the BB power spectrum is consistent with zero. Based on these measurements, we constrain the tensor-to-scalar ratio to r = 1.1(-0.8)(+0.9) (r < 2.8 at 95% C. L.) as derived by the ML pipeline, and r = 1.2(-0.8)(+0.9) (r < 2.7 at 95% C. L.) as derived by the PCL pipeline. In one of the fields, we find a correlation with the dust component of the Planck Sky Model, though the corresponding excess power is small compared to statistical errors. Finally, we derive limits on all known systematic errors, and demonstrate that these correspond to a tensor-to-scalar ratio smaller than r = 0.01, the lowest level yet reported in the literature.

引用

页数：10

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