Planck 2013 results. V. LFI calibration

被引：64

作者：

Aghanim, N. ^{[59
]}

Armitage-Caplan, C. ^{[91
]}

Arnaud, M. ^{[72
]}

Ashdown, M. ^{[6
,69
]}

Atrio-Barandela, F. ^{[17
]}

Aumont, J. ^{[59
]}

Baccigalupi, C. ^{[85
]}

Banday, A. J. ^{[8
,94
]}

Barreiro, R. B. ^{[66
]}

Battaner, E. ^{[95
]}

Benabed, K. ^{[60
,93
]}

Benoit, A. ^{[57
]}

Benoit-Levy, A. ^{[24
,60
,93
]}

Bernard, J. -P. ^{[8
,94
]}

Bersanelli, M. ^{[34
,49
]}

Bielewicz, P. ^{[8
,85
,94
]}

Bobin, J. ^{[72
]}

Bock, J. J. ^{[9
,67
]}

Bonaldi, A. ^{[68
]}

Bonavera, L. ^{[66
]}

Bond, J. R. ^{[7
]}

Borrill, J. ^{[12
,88
]}

Bouchet, F. R. ^{[60
,93
]}

Bridges, M. ^{[6
,63
,69
]}

Bucher, M. ^{[1
]}

Burigana, C. ^{[32
,48
]}

Butler, R. C. ^{[48
]}

Cappellini, B. ^{[49
]}

Cardoso, J. -F. ^{[1
,60
,73
,74
]}

Catalano, A. ^{[71
,75
]}

Chamballu, A. ^{[14
,59
,72
]}

Chen, X. ^{[56
]}

Chiang, L. -Y ^{[62
]}

Christensen, P. R. ^{[37
,82
]}

Church, S. ^{[90
]}

Colombi, S. ^{[60
,93
]}

Colombo, L. P. L. ^{[23
,67
]}

Crill, B. P. ^{[67
,83
]}

Curto, A. ^{[6
,66
]}

Cuttaia, F. ^{[48
]}

Danese, L. ^{[85
]}

Davies, R. D. ^{[68
]}

Davis, R. J. ^{[68
]}

de Bernardis, P. ^{[33
]}

de Rosa, A. ^{[48
]}

de Zotti, G. ^{[44
,85
]}

Delabrouille, J. ^{[1
]}

Dickinson, C.

Diego, J. M. ^{[66
]}

Dole, H. ^{[58
,59
]}

机构：

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

[2] Aalo 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, Rome, Italy

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

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

[8] CNRS, IRAP, F-31028 Toulouse 4, France

[9] CALTECH, Pasadena, CA 91125 USA

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

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

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

[13] CSIC, Madrid, Spain

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

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

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

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

[18] Univ Oviedo, Dept Fis, E-33007 Oviedo, 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 Latter 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, 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 Urbana hampaign, 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, Via Celoria 16, Milan, Italy

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

[36] Univ Roma Tor Vergata, Dipartimento Fis, I-00173 Rome, Italy

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

[38] Univ La Laguna, Dept Astrifis, E-38206 Tenerife, Spain

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

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

[41] Haverford Coll, Dept Astron, Haverford, PA 19041 USA

[42] Aalto Univ, Univ Helsinki, Helsinki Inst Phys, Helsinki, Finland

[43] Osserv Astrofis Catania, INAF, I-95125 Catania, Italy

[44] Osserv Astron Padova, INAF, Padua, Italy

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

[46] Osserv Astron Trieste, INAF, I-34131 Trieste, Italy

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

[48] INAF, IASF Bologna, Bologna, Italy

[49] INAF, IASF Milano, Milan, Italy

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

来源：

ASTRONOMY & ASTROPHYSICS | 2014年 / 571卷

关键词：

cosmic background radiation; instrumentation: polarimeters; methods: data analysis; PROBE WMAP OBSERVATIONS; PRE-LAUNCH STATUS; SKY MAPS; ANISOTROPY;

D O I：

10.1051/0004-6361/201321527

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We discuss the methods employed to photometrically calibrate the data acquired by the Low Frequency Instrument on Planck. Our calibration is based on a combination of the orbital dipole plus the solar dipole, caused respectively by the motion of the Planck spacecraft with respect to the Sun and by motion of the solar system with respect to the cosmic microwave background (CMB) rest frame. The latter provides a signal of a few mK with the same spectrum as the CMB anisotropies and is visible throughout the mission. In this data release we rely on the characterization of the solar dipole as measured by WMAP. We also present preliminary results (at 44 GHz only) on the study of the Orbital Dipole, which agree with the WMAP value of the solar system speed within our uncertainties. We compute the calibration constant for each radiometer roughly once per hour; in order to keep track of changes in the detectors' gain. Since non-idealities in the optical response of the beams proved to be important, we implemented a fast convolution algorithm which considers the full beam response in estimating the signal generated by the dipole. Moreover, in order to further reduce the impact of residual systematics due to sidelobes, we estimated time variations in the calibration constant of the 30 GHz radiometers (the ones with the largest sidelobes) using the signal of an internal reference load at 4 K instead of the CMB dipole. We have estimated the accuracy of the LFI calibration following two strategies: (1) we have run a set of simulations to assess the impact of statistical errors and systematic effects in the instrument and in the calibration procedure; and (2) we have performed a number of internal consistency checks on the data and on the brightness temperature of Jupiter. Errors in the calibration of this Planck/LFI data release are expected to be about 0.6% at 44 and 70 GHz, and 0.8% at 30 GHz. Both these preliminary results at low and high l are consistent with WMAP results within uncertainties and comparison of power spectra indicates good consistency in the absolute calibration with HFI (0.3%) and a 1.4 sigma discrepancy with WMAP (0.9%).

引用

页数：29

共 69 条

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