THE ATACAMA COSMOLOGY TELESCOPE: A MEASUREMENT OF THE 600 < l < 8000 COSMIC MICROWAVE BACKGROUND POWER SPECTRUM AT 148 GHz

被引：99

作者：

Fowler, J. W. ^{[1
]}

Acquaviva, V. ^{[2
,3
]}

Ade, P. A. R. ^{[4
]}

Aguirre, P. ^{[5
]}

Amiri, M. ^{[6
]}

Appel, J. W. ^{[1
]}

Barrientos, L. F. ^{[5
]}

Battistelli, E. S. ^{[6
,7
]}

Bond, J. R. ^{[8
]}

Brown, B. ^{[9
]}

Burger, B. ^{[6
]}

Chervenak, J. ^{[10
]}

Das, S. ^{[1
,2
,11
,12
]}

Devlin, M. J. ^{[13
]}

Dicker, S. R. ^{[13
]}

Doriese, W. B. ^{[14
]}

Dunkley, J. ^{[1
,2
,15
]}

Duenner, R. ^{[5
]}

Essinger-Hileman, T. ^{[1
]}

Fisher, R. P. ^{[1
]}

Hajian, A. ^{[1
,2
]}

Halpern, M. ^{[6
]}

Hasselfield, M. ^{[6
]}

Hernandez-Monteagudo, C. ^{[16
]}

Hilton, G. C. ^{[14
]}

Hilton, M. ^{[17
,18
]}

Hincks, A. D. ^{[1
]}

Hlozek, R. ^{[15
]}

Huffenberger, K. M. ^{[19
]}

Hughes, D. H. ^{[20
]}

Hughes, J. P. ^{[3
]}

Infante, L. ^{[5
]}

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

Jimenez, R. ^{[21
,22
]}

Juin, J. B. ^{[5
]}

Kaul, M. ^{[13
]}

Klein, J. ^{[13
]}

Kosowsky, A. ^{[9
]}

Lau, J. M. ^{[1
,23
,24
]}

Limon, M. ^{[1
,13
,25
]}

Lin, Y. -T. ^{[2
,5
,26
]}

Lupton, R. H. ^{[2
]}

Marriage, T. A. ^{[2
]}

Marsden, D. ^{[13
]}

Martocci, K. ^{[1
,27
]}

Mauskopf, P. ^{[4
]}

Menanteau, F. ^{[3
]}

Moodley, K. ^{[17
,18
]}

Moseley, H. ^{[10
]}

Netterfield, C. B. ^{[28
]}

机构：

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

[2] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA

[3] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA

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

[5] Pontificia Univ Catolica Chile, Fac Fis, Dept Astron & Astrofis, Santiago 22, Chile

[6] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z4, Canada

[7] Univ Roma La Sapienza, Dept Phys, I-00185 Rome, Italy

[8] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada

[9] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA

[10] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA

[11] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, LBL, Berkeley, CA 94720 USA

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

[13] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA

[14] NIST, Quantum Devices Grp, Boulder, CO 80305 USA

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

[16] Max Planck Inst Astrophys, D-85741 Garching, Germany

[17] Univ KwaZulu Natal, Astrophys & Cosmol Res Unit, Sch Math Sci, ZA-4041 Durban, South Africa

[18] CSIR Campus, Ctr High Performance Comp, Cape Town, South Africa

[19] Univ Miami, Dept Phys, Coral Gables, FL 33124 USA

[20] INAOE, Puebla, Mexico

[21] Univ Barcelona, ICREA, E-08028 Barcelona, Spain

[22] Univ Barcelona, ICC, E-08028 Barcelona, Spain

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

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

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

[26] Univ Tokyo, Inst Phys & Math Universe, Chiba 2778568, Japan

[27] Kavli Inst Cosmol Phys, Chicago, IL 60637 USA

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

[29] Haverford Coll, Dept Phys & Astron, Haverford, PA 19041 USA

[30] W Chester Univ Penn, Dept Phys, W Chester, PA 19383 USA

[31] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA

[32] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA

来源：

ASTROPHYSICAL JOURNAL | 2010年 / 722卷 / 02期

基金：

新加坡国家研究基金会; 加拿大自然科学与工程研究理事会;

关键词：

cosmic background radiation; cosmology: observations; 1200-MU-M MAMBO SURVEY; GOODS-N FIELD; ANISOTROPY POWER; DUST EMISSION; PROBE; TEMPERATURE; MAPS; POLARIZATION; CONSTRAINTS; PREDICTIONS;

D O I：

10.1088/0004-637X/722/2/1148

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present a measurement of the angular power spectrum of the cosmic microwave background (CMB) radiation observed at 148 GHz. The measurement uses maps with 1'.4 angular resolution made with data from the Atacama Cosmology Telescope (ACT). The observations cover 228 deg(2) of the southern sky, in a 4 degrees.2 wide strip centered on declination 53 degrees south. The CMB at arcminute angular scales is particularly sensitive to the Silk damping scale, to the Sunyaev-Zel'dovich (SZ) effect from galaxy clusters, and to emission by radio sources and dusty galaxies. After masking the 108 brightest point sources in our maps, we estimate the power spectrum between 600 < l < 8000 using the adaptive multi-taper method to minimize spectral leakage and maximize use of the full data set. Our absolute calibration is based on observations of Uranus. To verify the calibration and test the fidelity of our map at large angular scales, we cross-correlate the ACT map to the WMAP map and recover the WMAP power spectrum from 250 < l < 1150. The power beyond the Silk damping tail of the CMB (l similar to 5000) is consistent with models of the emission from point sources. We quantify the contribution of SZ clusters to the power spectrum by fitting to a model normalized to sigma(8) = 0.8. We constrain the model's amplitude A(SZ) < 1.63 (95% CL). If interpreted as a measurement of sigma(8), this implies sigma(SZ)(8) < 0.86 (95% CL) given our SZ model. A fit of ACT and WMAP five-year data jointly to a six-parameter Lambda CDM model plus point sources and the SZ effect is consistent with these results.

引用

页码：1148 / 1161

页数：14

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THE ATACAMA COSMOLOGY TELESCOPE: A MEASUREMENT OF THE 600 &lt; l &lt; 8000 COSMIC MICROWAVE BACKGROUND POWER SPECTRUM AT 148 GHz

THE ATACAMA COSMOLOGY TELESCOPE: A MEASUREMENT OF THE 600 < l < 8000 COSMIC MICROWAVE BACKGROUND POWER SPECTRUM AT 148 GHz