Planck 2013 results. VII. HFI time response and beams

被引：90

作者：

Ade, P. A. R. ^{[84
]}

Aghanim, N. ^{[57
]}

Armitage-Caplan, C. ^{[88
]}

Arnaud, M. ^{[69
]}

Ashdown, M. ^{[6
,66
]}

Atrio-Barandela, E. ^{[18
]}

Aumont, J. ^{[57
]}

Baccigalupi, C. ^{[83
]}

Banday, A. J. ^{[10
,91
]}

Barreiro, R. B. ^{[63
]}

Battaner, E. ^{[92
]}

Benabed, K. ^{[58
,90
]}

Benoit, A. ^{[55
]}

Benoit-Levy, A. ^{[24
,58
,90
]}

Bernard, J. -P. ^{[10
,91
]}

Bersanelli, M. ^{[34
,48
]}

Bielewicz, P. ^{[10
,83
,91
]}

Bobin, J. ^{[69
]}

Bock, J. J. ^{[11
,64
]}

Bond, J. R. ^{[9
]}

Borrill, J. ^{[14
,85
]}

Bouchet, F. R. ^{[58
,90
]}

Bowyer, J. W. ^{[53
]}

Bridges, M. ^{[6
,61
,66
]}

Bucher, M. ^{[1
]}

Burigana, C. ^{[32
,47
]}

Cardoso, J. -E ^{[1
,58
,70
,71
]}

Catalano, A. ^{[68
,72
]}

Challinor, A. ^{[12
,61
,66
]}

Chamballu, A. ^{[15
,57
,69
]}

Chary, R. -R. ^{[54
]}

Chiang, H. C. ^{[7
,27
]}

Chiang, L. -Y ^{[60
]}

Christensen, P. R. ^{[37
,79
]}

Church, S. ^{[87
]}

Clements, D. L. ^{[53
]}

Colombi, S.

Colombo, L. P. L. ^{[23
,64
]}

Couchot, F. ^{[67
]}

Coulais, A. ^{[68
]}

Crill, B. P. ^{[64
,80
]}

Curto, A. ^{[6
,63
]}

Cuttaia, E.

Danese, L. ^{[83
]}

Davies, R. D. ^{[65
]}

de Bernardis, P. ^{[33
]}

de Rosa, A.

de Zotti, G. ^{[43
,83
]}

Delabrouille, J. ^{[1
]}

Delouis, J. -M. ^{[58
,90
]}

机构：

[1] Univ Paris Diderot, Observ Paris, Sorbonne Paris Cite, CNRS IN2P3,CEA lrfu,APC, F-75205 Paris 13, France

[2] Aalto Univ, Metsahovi Radio Observ, Kylmala 02540, Finland

[3] African Inst Math Sci, Cape Town, South Africa

[4] Agenzia Spaziale Italiana, Sci Data Ctr, I-00133 Rome, Italy

[5] Agenzia Spaziale Italiana, I-00198 Rome, Italy

[6] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England

[7] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, ZA-4000 Durban, South Africa

[8] ALMA Santiago Cent Off, Santiago 0355, Chile

[9] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada

[10] CNRS, TRAP, F-31028 Toulouse 4, France

[11] CALTECH, Pasadena, CA 91125 USA

[12] Univ Cambridge, Ctr Theoret Cosmol, DAMTP, Cambridge CB3 0WA, England

[13] Ctr Estudios Fis Cosmos Aragon, Teruel 44001, Spain

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

[15] CEA Saclay, DSM Irfu SPP, F-91191 Gif Sur Yvette, France

[16] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark

[17] Univ Geneva, Dept Phys Theor, CH-1211 Geneva 4, Switzerland

[18] Univ Salamanca, Fac Ciencias, Dept Fis Fundamental, E-37008 Salamanca, Spain

[19] Univ Toronto, Dept Astron & Astrophys, Toronto, ON, Canada

[20] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, Netherlands

[21] Univ Calif Berkeley, Dept Elect Engn & Comp Sci, Berkeley, CA 94720 USA

[22] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada

[23] Univ So Calif, Dept Phys & Astron, Dana & David Dornsife Coll Letter Arts & Sci, Los Angeles, CA 90089 USA

[24] UCL, Dept Phys & Astron, London WC1E 6BT, England

[25] Florida State Univ, Dept Phys, Tallahassee, FL 32306 USA

[26] Univ Helsinki, Dept Phys, FIN-00014 Helsinki, Finland

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

[28] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA

[29] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA

[30] Univ Illinois UrbanaChampaign, Dept Phys, Urbana, IL USA

[31] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy

[32] Univ Ferrara, Dipartimento Fis & Sci Terra, I-44122 Ferrara, Italy

[33] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy

[34] Univ Milan, Dipartimento Fis, I-20133 Milan, Italy

[35] Univ Trieste, Dipartmento Fis, I-34127 Trieste, Italy

[36] Univ Roma Tor Vergata, Dipartmento Fis, I-00133 Rome, Italy

[37] Niels Bohr Inst, Discovery Ctr, DK-2100 Copenhagen, Denmark

[38] European So Observ, ESO Vitacura, Santiago 19001, Chile

[39] European Space Agcy, ESAC, Planck Sci Off, Madrid 28692, Spain

[40] European Space Agcy, Estec, NL-2201 AZ Noordwijk, Netherlands

[41] Aalto Univ, Univ Helsinki, Helsinki Inst Phys, FIN-00014 Helsinki, Finland

[42] Osserv Astrofis Catania, INAF, I-95123 Catania, Italy

[43] Osserv Astron Padova, INAF, I-35122 Padua, Italy

[44] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy

[45] Osserv Astron Trieste, INAF, I-34143 Trieste, Italy

[46] INAF Ist Radioastron, I-40129 Bologna, Italy

[47] INAF IASF Bologna, I-40129 Bologna, Italy

[48] INAF IASF Milano, I-20133 Milan, Italy

[49] Ist Nazl Fis Nucl, Sez Bologna, I-40126 Bologna, Italy

[50] Univ Roma La Sapienza, Ist Nazl Fis Nucl, Sez Roma 1, I-00185 Rome, Italy

来源：

ASTRONOMY & ASTROPHYSICS | 2014年 / 571卷

关键词：

cosmic background radiation; cosmology: observations; instrumentation: detectors; surveys; PRE-LAUNCH STATUS; POWER SPECTRUM; MICROWAVE; MAPS; CALIBRATION;

D O I：

10.1051/0004-6361/201321535

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

This paper characterizes the effective beams, the effective beam window functions and the associated errors for the Planck High Frequency Instrument (HFI) detectors. The effective beam is the angular response including the effect of the optics, detectors, data processing and the scan strategy. The window function is the representation of this beam in the harmonic domain which is required to recover an unbiased measurement of the cosmic microwave background angular power spectrum. The HFI is a scanning instrument and its effective beams are the convolution of: a) the optical response of the telescope and feeds; b) the processing of the time-ordered data and deconvolution of the bolometric and electronic transfer function; and c) the merging of several surveys to produce maps. The time response transfer functions are measured using observations of Jupiter and Saturn and by minimizing survey difference residuals. The scanning beam is the post-deconvolution angular response of the instrument, and is characterized with observations of Mars. The main beam solid angles are determined to better than 0.5% at each HFI frequency band. Observations of Jupiter and Saturn limit near sidelobes (within 5 degrees) to about 0.1% of the total solid angle. Time response residuals remain as long tails in the scanning beams, but contribute less than 0.1% of the total solid angle. The bias and uncertainty in the beam products are estimated using ensembles of simulated planet observations that include the impact of instrumental noise and known systematic effects. The correlation structure of these ensembles is well-described by five errors eigenmodes that are sub-dominant to sample variance and instrumental noise in the harmonic domain. A suite of consistency tests provide confidence that the error model represents a sufficient description of the data. The total error in the effective beam window functions is below 1% at 100 GHz up to multiple l similar to 1500, below 0.5% at 143 and 217 GHz up to l similar to 2000.

引用

页数：31

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