FIRST SEASON QUIET OBSERVATIONS: MEASUREMENTS OF COSMIC MICROWAVE BACKGROUND POLARIZATION POWER SPECTRA AT 43 GHz IN THE MULTIPOLE RANGE 25 ≤ l ≤ 475

被引：79

作者：

Bischoff, C. ^{[1
,24
]}

Brizius, A. ^{[1
,2
,24
]}

Buder, I. ^{[1
,24
]}

Chinone, Y. ^{[3
,4
]}

Cleary, K. ^{[5
]}

Dumoulin, R. N. ^{[6
,7
]}

Kusaka, A. ^{[1
,24
]}

Monsalve, R. ^{[8
]}

Naess, S. K. ^{[9
]}

Newburgh, L. B. ^{[6
,7
]}

Reeves, R. ^{[5
]}

Smith, K. M. ^{[1
,24
]}

Wehus, I. K. ^{[10
]}

Zuntz, J. A. ^{[11
,12
,13
]}

Zwart, J. T. L. ^{[6
,7
]}

Bronfman, L. ^{[14
]}

Bustos, R. ^{[8
,14
,15
]}

Church, S. E. ^{[16
,17
]}

Dickinson, C. ^{[18
]}

Eriksen, H. K. ^{[9
,19
]}

Ferreira, P. G.

Gaier, T. ^{[20
]}

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

Hasegawa, M. ^{[3
]}

Hazumi, M. ^{[3
]}

Huffenberger, K. M. ^{[8
]}

Jones, M. E. ^{[11
]}

Kangaslahti, P. ^{[20
]}

Kapner, D. J. ^{[1
,24
]}

Lawrence, C. R. ^{[20
]}

Limon, M. ^{[6
,7
]}

May, J. ^{[14
]}

McMahon, J. J. ^{[21
]}

Miller, A. D. ^{[6
,7
]}

Nguyen, H. ^{[22
]}

Nixon, G. W. ^{[23
]}

Pearson, T. J. ^{[5
]}

Piccirillo, L. ^{[18
]}

Radford, S. J. E. ^{[5
]}

Readhead, A. C. S. ^{[5
]}

Richards, J. L. ^{[5
]}

Samtleben, D. ^{[2
]}

Seiffert, M. ^{[20
]}

Shepherd, M. C. ^{[5
]}

Staggs, S. T.

Tajima, O. ^{[1
,3
,24
]}

Thompson, K. L. ^{[16
,17
]}

Vanderlinde, K. ^{[1
,24
]}

Williamson, R. ^{[6
,7
]}

Winstein, B. ^{[1
,24
]}

机构：

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

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

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

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

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

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

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

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

[9] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway

[10] Univ Oslo, Dept Phys, N-0316 Oslo, Norway

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

[12] Oxford Martin Sch, Oxford OX1 3BD, England

[13] UCL, Dept Phys & Astron, London WC1E, England

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

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

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

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

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

[19] Univ Oslo, Ctr Math Applicat, N-0316 Oslo, Norway

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

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

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

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

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

来源：

ASTROPHYSICAL JOURNAL | 2011年 / 741卷 / 02期

基金：

美国国家科学基金会; 英国科学技术设施理事会; 美国国家航空航天局;

关键词：

cosmic background radiation; cosmology: observations; gravitational waves; inflation; polarization; PROBE WMAP OBSERVATIONS; PERSEUS MOLECULAR-COMPLEX; MAPS; TEMPERATURE; CALIBRATION; EMISSION; ANTENNAS; DESIGN; FLIGHT;

D O I：

10.1088/0004-637X/741/2/111

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The Q/U Imaging ExperimenT (QUIET) employs coherent receivers at 43 GHz and 94 GHz, operating on the Chajnantor plateau in the Atacama Desert in Chile, to measure the anisotropy in the polarization of the cosmic microwave background (CMB). QUIET primarily targets the B modes from primordial gravitational waves. The combination of these frequencies gives sensitivity to foreground contributions from diffuse Galactic synchrotron radiation. Between 2008 October and 2010 December, over 10,000 hr of data were collected, first with the 19 element 43 GHz array (3458 hr) and then with the 90 element 94 GHz array. Each array observes the same four fields, selected for low foregrounds, together covering approximate to 1000 deg(2). This paper reports initial results from the 43 GHz receiver, which has an array sensitivity to CMB fluctuations of 69 mu K root s. The data were extensively studied with a large suite of null tests before the power spectra, determined with two independent pipelines, were examined. Analysis choices, including data selection, were modified until the null tests passed. Cross-correlating maps with different telescope pointings is used to eliminate a bias. This paper reports the EE, BB, and EB power spectra in the multipole range l = 25-475. With the exception of the lowest multipole bin for one of the fields, where a polarized foreground, consistent with Galactic synchrotron radiation, is detected with 3 sigma significance, the E-mode spectrum is consistent with the Lambda CDM model, confirming the only previous detection of the first acoustic peak. The B-mode spectrum is consistent with zero, leading to a measurement of the tensor-to-scalar ratio of r = 0.35(-0.87)(+1.06). The combination of a new time-stream "double-demodulation" technique, side-fed Dragonian optics, natural sky rotation, and frequent boresight rotation leads to the lowest level of systematic contamination in the B-mode power so far reported, below the level of r = 0.1.

引用

页数：18

共 57 条

[1] Polarization observations of the anomalous microwave emission in the perseus molecular complex with the cosmosomas experiment
Battistelli, E. S.
Rebolo, R.
Rubino-Martin, J. A.
Hildebrandt, S. R.
Watson, R. A.
Gutierrez, C.
Hoyland, R. J.
[J]. ASTROPHYSICAL JOURNAL, 2006, 645 (02) : L141 - L144
[2] Statistical properties of polarized radio sources at high frequency and their impact on cosmic microwave background polarization measurements
Battye, R. A.
Browne, I. W. A.
Peel, M. W.
Jackson, N. J.
Dickinson, C.
[J]. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 2011, 413 (01) : 132 - 148
[3] New measurements of fine-scale CMB polarization power spectra from CAPMAP at both 40 and 90 Ghz
Bischoff, C.
Hyatt, L.
McMahon, J. J.
Nixon, G. W.
Samtleben, D.
Smith, K. M.
Vanderlinde, K.
Barkats, D.
Farese, P.
Gaier, T.
Gundersen, J. O.
Hedman, M. M.
Staggs, S. T.
Winstein, B.
[J]. ASTROPHYSICAL JOURNAL, 2008, 684 (02) : 771 - 789
[4] Estimating the power spectrum of the cosmic microwave background
Bond, JR
Jaffe, AH
Knox, L
[J]. PHYSICAL REVIEW D, 1998, 57 (04): : 2117 - 2137
[5] Bornemann J., 1995, IEEE T MTT, V43, P95
[6] IMPROVED MEASUREMENTS OF THE TEMPERATURE AND POLARIZATION OF THE COSMIC MICROWAVE BACKGROUND FROM QUaD
Brown, M. L.
Ade, P.
Bock, J.
Bowden, M.
Cahill, G.
Castro, P. G.
Church, S.
Culverhouse, T.
Friedman, R. B.
Ganga, K.
Gear, W. K.
Gupta, S.
Hinderks, J.
Kovac, J.
Lange, A. E.
Leitch, E.
Melhuish, S. J.
Memari, Y.
Murphy, J. A.
Orlando, A.
Sullivan, C. O'
Piccirillo, L.
Pryke, C.
Rajguru, N.
Rusholme, B.
Schwarz, R.
Taylor, A. N.
Thompson, K. L.
Turner, A. H.
Wu, E. Y. S.
Zemcov, M.
[J]. ASTROPHYSICAL JOURNAL, 2009, 705 (01) : 978 - 999
[7] Buder I., 2010, P SPIE, V7741
[8] The Parkes Galactic Meridian Survey: observations and CMB polarization foreground analysis
Carretti, E.
Haverkorn, M.
McConnell, D.
Bernardi, G.
McClure-Griffiths, N. M.
Cortiglioni, S.
Poppi, S.
[J]. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 2010, 405 (03) : 1670 - 1689
[9] Error analysis of quadratic power spectrum estimates for cosmic microwave background polarization: sampling covariance
Challinor, A
Chon, G
[J]. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 2005, 360 (02) : 509 - 532
[10] The design of classical offset Dragonian reflector antennas with circular apertures
Chang, SH
Prata, A
[J]. IEEE TRANSACTIONS ON ANTENNAS AND PROPAGATION, 2004, 52 (01) : 12 - 19

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