Planck 2013 results. IX. HFI spectral response

被引：81

作者：

Ade, P. A. R. ^{[83
]}

Aghanim, N. ^{[57
]}

Armitage-Caplan, C.

Arnaud, M. ^{[69
]}

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

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

Aumont, J. ^{[57
]}

Baccigalupi, C. ^{[82
]}

Banday, A. J. ^{[10
,89
]}

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

Battaner, E. ^{[90
,91
]}

Benabed, K. ^{[58
,88
]}

Benoit, A. ^{[55
]}

Benoit-Levy, A. ^{[24
,58
,88
]}

Bernard, J. -P. ^{[10
,89
]}

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

Bielewicz, P. ^{[10
,82
,89
]}

Bobin, J. ^{[69
]}

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

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

Borrill, J. ^{[14
,84
]}

Bouchet, F. R. ^{[58
,88
]}

Boulanger, F. ^{[57
]}

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

Bucher, M. ^{[1
]}

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

Cardoso, J. -F. ^{[1
,32
,70
,71
]}

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

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

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

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

Chen, X. ^{[54
]}

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

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

Christensen, P. R. ^{[37
,78
]}

Church, S. ^{[86
]}

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

Colombi, S. ^{[88
]}

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

Combet, C. ^{[72
]}

Comis, B. ^{[72
]}

Couchot, F. ^{[67
]}

Coulais, A. ^{[68
]}

Crill, B. P. ^{[64
,79
]}

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

Cuttaia, F. ^{[47
]}

Danese, L. ^{[82
]}

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

de Bernardis, P. ^{[33
]}

de Rosa, A. ^{[47
]}

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, ZA-7701 Cape Town, South Africa

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

[5] Agenzia Spaziale Italiana, Rome, Italy

[6] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 OHE, 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 7630355, Chile

[9] Univ Toronto, CITA, Toronto, ON M55 3H8, Canada

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

[11] CALTECH, Pasadena, CA 91125 USA

[12] Univ Cambridge, DAMTP, Ctr Theoret Cosmol, 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, 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, Dipartimento 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-34131 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

基金：

加拿大自然科学与工程研究理事会;

关键词：

instrumentation: detectors; instrumentation: photometers; space vehicles: instruments; cosmology: observations; cosmic background radiation; MOLECULAR CLOUDS; COBE;

D O I：

10.1051/0004-6361/201321531

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The Planck High Frequency Instrument (HFI) spectral response was determined through a series of ground based tests conducted with the HFI focal plane in a cryogenic environment prior to launch. The main goal of the spectral transmission tests was to measure the relative spectral response (including the level of out-of-band signal rejection) of all HFI detectors to a known source of electromagnetic radiation individually. This was determined by measuring the interferometric output of a continuously scanned Fourier transform spectrometer with all HFI detectors. As there is no on-board spectrometer within HFI, the ground-based spectral response experiments provide the definitive data set for the relative spectral calibration of the HFI. Knowledge of the relative variations in the spectral response between HFI detectors allows for a more thorough analysis of the HFI data. The spectral response of the HFI is used in Planck data analysis and component separation, this includes extraction of CO emission observed within Planck bands, dust emission, Sunyaev-Zeldovich sources, and intensity to polarization leakage. The HFI spectral response data have also been used to provide unit conversion and colour correction analysis tools. While previous papers describe the pre-flight experiments conducted on the Planck HFI, this paper focusses on the analysis of the pre-flight spectral response measurements and the derivation of data products, e.g. band-average spectra, unit conversion coefficients, and colour correction coefficients, all with related uncertainties. Verifications of the HFI spectral response data are provided through comparisons with photometric HFI flight data. This validation includes use of HFI zodiacal emission observations to demonstrate out-of-band spectral signal rejection better than 10(8). The accuracy of the HFI relative spectral response data is verified through comparison with complementary flight-data based unit conversion coefficients and colour correction coefficients. These coefficients include those based upon HFI observations of CO, dust, and Sunyaev-Zeldovich emission. General agreement is observed between the ground-based spectral characterization of HFI and corresponding in-flight observations, within the quoted uncertainty of each; explanations are provided for any discrepancies.

引用

页数：27

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