MODELING ATMOSPHERIC EMISSION FOR CMB GROUND-BASED OBSERVATIONS

被引：33

作者：

Errard, J. ^{[1
,2
]}

Ade, P. A. R. ^{[3
]}

Akiba, Y. ^{[4
]}

Arnold, K. ^{[5
]}

Atlas, M. ^{[5
]}

Baccigalupi, C. ^{[6
]}

Barron, D. ^{[5
]}

Boettger, D. ^{[7
]}

Borrill, J. ^{[1
,2
]}

Chapman, S. ^{[8
]}

Chinone, Y. ^{[4
,9
]}

Cukierman, A. ^{[9
]}

Delabrouille, J. ^{[10
]}

Dobbs, M. ^{[11
]}

Ducout, A. ^{[12
]}

Elleflot, T. ^{[5
]}

Fabbian, G. ^{[6
]}

Feng, C. ^{[13
]}

Feeney, S. ^{[12
]}

Gilbert, A. ^{[11
]}

Goeckner-Wald, N. ^{[9
]}

Halverson, N. W. ^{[14
,15
,16
]}

Hasegawa, M. ^{[4
,17
]}

Hattori, K. ^{[4
]}

Hazumi, M. ^{[4
,17
,18
]}

Hill, C. ^{[9
]}

Holzapfel, W. L. ^{[9
]}

Hori, Y. ^{[9
]}

Inoue, Y. ^{[4
]}

Jaehnig, G. C. ^{[14
,16
]}

Jaffe, A. H. ^{[12
]}

Jeong, O. ^{[9
]}

Katayama, N. ^{[18
]}

Kaufman, J. ^{[5
]}

Keating, B. ^{[5
]}

Kermish, Z. ^{[19
]}

Keskitalo, R. ^{[2
]}

Kisner, T. ^{[1
,2
]}

Le Jeune, M. ^{[10
]}

Lee, A. T. ^{[9
,20
]}

Leitch, E. M. ^{[21
,22
]}

Leon, D. ^{[5
]}

Linder, E. ^{[20
]}

Matsuda, F. ^{[5
]}

Matsumura, T. ^{[23
]}

Miller, N. J. ^{[24
]}

Myers, M. J. ^{[9
]}

Navaroli, M. ^{[5
]}

Nishino, H. ^{[18
]}

Okamura, T. ^{[4
]}

机构：

[1] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA

[2] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA

[3] Cardiff Univ, Sch Phys & Astron, Cardiff CF10 3XQ, S Glam, Wales

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

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

[6] Int Sch Adv Studies SISSA, I-34014 Trieste, Italy

[7] Pontificia Univ Catolica Chile, Dept Astron, Santiago, Chile

[8] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 4R2, Canada

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

[10] Univ Paris Diderot, Sorbonne Paris Cite, AstroParticule & Cosmol, CNRS,IN2P3,CEA,Irfu,Obs Paris, Paris, France

[11] McGill Univ, Dept Phys, Montreal, PQ H3A 0G4, Canada

[12] Univ London Imperial Coll Sci Technol & Med, Dept Phys, London SW7 2AZ, England

[13] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA USA

[14] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA

[15] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA

[16] Univ Colorado, Dept Phys, Boulder, CO 80309 USA

[17] Grad Univ Adv Studies, Miura Dist, Kanagawa 2400115, Japan

[18] Univ Tokyo, Todai Inst Adv Study, Kavli Inst Phys & Math Universe WPI, Kashiwa, Chiba 2778583, Japan

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

[20] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA

[21] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA

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

[23] JAXA, Chofu, Tokyo, Japan

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

[25] Univ Calif San Diego, Dept Elect & Comp Engn, La Jolla, CA 92093 USA

[26] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia

[27] Univ Calif Berkeley, Miller Inst Basic Res Sci, Berkeley, CA 94720 USA

[28] Osaka Univ, Toyonaka, Osaka 5600043, Japan

来源：

ASTROPHYSICAL JOURNAL | 2015年 / 809卷 / 01期

基金：

美国国家科学基金会;

关键词：

atmospheric effects; methods: data analysis; methods: observational; MICROWAVE BACKGROUND EXPERIMENTS; COMPONENT SEPARATION; FLUCTUATIONS; POLARIZATION; TURBULENCE; SITES; NOISE;

D O I：

10.1088/0004-637X/809/1/63

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Atmosphere is one of the most important noise sources for ground-based cosmic microwave background (CMB) experiments. By increasing optical loading on the detectors, it amplifies their effective noise, while its fluctuations introduce spatial and temporal correlations between detected signals. We present a physically motivated 3D-model of the atmosphere total intensity emission in the millimeter and sub-millimeter wavelengths. We derive a new analytical estimate for the correlation between detectors time-ordered data as a function of the instrument and survey design, as well as several atmospheric parameters such as wind, relative humidity, temperature and turbulence characteristics. Using an original numerical computation, we examine the effect of each physical parameter on the correlations in the time series of a given experiment. We then use a parametric-likelihood approach to validate the modeling and estimate atmosphere parameters from the POLARBEAR-I project first season data set. We derive a new 1.0% upper limit on the linear polarization fraction of atmospheric emission. We also compare our results to previous studies and weather station measurements. The proposed model can be used for realistic simulations of future ground-based CMB observations.

引用

页数：19

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