Planck pre-launch status: The HFI instrument, from specification to actual performance

被引：190

作者：

Lamarre, J. -M. ^{[1
]}

Puget, J. -L. ^{[2
,3
]}

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

Bouchet, F. ^{[5
,6
]}

Guyot, G. ^{[2
,3
]}

Lange, A. E. ^{[7
,8
]}

Pajot, F. ^{[2
,3
]}

Arondel, A. ^{[2
,3
]}

Benabed, K. ^{[5
,6
]}

Beney, J. -L. ^{[10
,11
]}

Benoit, A. ^{[12
]}

Bernard, J. -Ph. ^{[13
]}

Bhatia, R. ^{[9
]}

Blanc, Y. ^{[14
]}

Bock, J. J. ^{[7
,8
]}

Breelle, E. ^{[15
,16
]}

Bradshaw, T. W. ^{[17
]}

Camus, P. ^{[12
]}

Catalano, A. ^{[1
,15
,16
]}

Charra, J. ^{[2
,3
]}

Charra, M. ^{[2
,3
]}

Church, S. E. ^{[18
,19
]}

Couchot, F. ^{[10
,11
]}

Coulais, A. ^{[1
]}

Crill, B. P. ^{[7
,8
]}

Crook, M. R. ^{[17
]}

Dassas, K. ^{[2
,3
]}

de Bernardis, P. ^{[20
]}

Delabrouille, J. ^{[15
,16
]}

de Marcillac, P. ^{[2
,3
]}

Delouis, J. -M. ^{[5
,6
]}

Desert, F. -X. ^{[21
]}

Dumesnil, C. ^{[2
,3
]}

Dupac, X. ^{[22
]}

Efstathiou, G. ^{[23
]}

Eng, P. ^{[2
,3
]}

Evesque, C. ^{[2
,3
]}

Fourmond, J. -J. ^{[2
,3
]}

Ganga, K. ^{[15
,16
]}

Giard, M. ^{[13
]}

Gispert, R. ^{[2
,3
]}

Guglielmi, L. ^{[15
,16
]}

Haissinski, J. ^{[10
,11
]}

Henrot-Versille, S. ^{[10
,11
]}

Hivon, E. ^{[5
,6
]}

Holmes, W. A. ^{[8
]}

Jones, W. C. ^{[8
,24
]}

Koch, T. C. ^{[8
]}

Lagardere, H. ^{[2
,3
]}

Lami, P. ^{[2
,3
]}

机构：

[1] UCP, UPMC, CNRS, Observ Paris,ENS,LERMA, F-75014 Paris, France

[2] CNRS, IAS, Inst Astrophys Spatiale, F-91405 Orsay, France

[3] Univ Paris 11, F-91405 Orsay, France

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

[5] CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France

[6] Univ Paris 06, F-75014 Paris, France

[7] CALTECH, Dept Phys, Pasadena, CA 91125 USA

[8] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA

[9] European Space Agcy ESTEC, Div Astrophys, NL-2201 AZ Noordwijk, Netherlands

[10] CNRS, LAL, Lab Accelerateur Lineaire, F-91898 Orsay, France

[11] Univ Paris 11, F-91898 Orsay, France

[12] Univ Grenoble 1, CNRS, Inst Neel, F-38042 Grenoble 9, France

[13] CNRS, CESR, Ctr Etud Spatiale Rayonnements, F-31038 Toulouse 4, France

[14] CNES, F-31401 Toulouse 9, France

[15] CNRS, Lab Astroparticule & Cosmol APC, F-75205 Paris 13, France

[16] Univ Paris 07, F-75205 Paris 13, France

[17] STFC, Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England

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

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

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

[21] CNRS, LAOG, F-38041 Grenoble 9, France

[22] European Space Agcy ESAC, Madrid 28691, Spain

[23] Univ Cambridge, Inst Astron, Cambridge CB3 OHA, England

[24] Princeton Univ, Dept Phys, Joseph Henry Lab, Princeton, NJ 08544 USA

来源：

ASTRONOMY & ASTROPHYSICS | 2010年 / 520卷

关键词：

cosmic microwave background; space vehicles: instruments; submillimeter: general; techniques: photometric; techniques: polarimetric; HIGH-FREQUENCY INSTRUMENT; MICROWAVE BACKGROUND ANISOTROPIES; THERMAL ARCHITECTURE; DESIGN; BOLOMETERS; MILLIMETER; SYSTEM; BOOMERANG; RECEIVER; NOISE;

D O I：

10.1051/0004-6361/200912975

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. The High Frequency Instrument (HFI) is one of the two focal instruments of the Planck mission. It will observe the whole sky in six bands in the 100 GHz-1 THz range. Aims. The HFI instrument is designed to measure the cosmic microwave background (CMB) with a sensitivity limited only by fundamental sources: the photon noise of the CMB itself and the residuals left after the removal of foregrounds. The two high frequency bands will provide full maps of the submillimetre sky, featuring mainly extended and point source foregrounds. Systematic effects must be kept at negligible levels or accurately monitored so that the signal can be corrected. This paper describes the HFI design and its characteristics deduced from ground tests and calibration. Methods. The HFI instrumental concept and architecture are feasible only by pushing new techniques to their extreme capabilities, mainly: (i) bolometers working at 100 mK and absorbing the radiation in grids; (ii) a dilution cooler providing 100 mK in microgravity conditions; (iii) a new type of AC biased readout electronics and (iv) optical channels using devices inspired from radio and infrared techniques. Results. The Planck-HFI instrument performance exceeds requirements for sensitivity and control of systematic effects. During ground-based calibration and tests, it was measured at instrument and system levels to be close to or better than the goal specification.

引用

页数：20

共 58 条

[1] Planck pre-launch status: The optical architecture of the HFI [J].

Ade, P. A. R. ;

Savini, G. ;

Sudiwala, R. ;

Tucker, C. ;

Catalano, A. ;

Church, S. ;

Colgan, R. ;

Desert, F. X. ;

Gleeson, E. ;

Jones, W. C. ;

Lamarre, J. -M. ;

Lange, A. ;

Longval, Y. ;

Maffei, B. ;

Murphy, J. A. ;

Noviello, F. ;

Pajot, F. ;

Puget, J. -L. ;

Ristorcelli, I. ;

Woodcraft, A. ;

Yurchenko, V. .

ASTRONOMY & ASTROPHYSICS, 2010, 520

[2]

Baranov V. K., 1966, Soviet Journal of Optical Technology, V33, P408

[3] Calibration and first light of the Diabolo photometer at the Millimetre and Infrared Testa Grigia Observatory [J].

Benoit, A ;

Zagury, F ;

Coron, N ;

De Petris, M ;

Désert, FX ;

Giard, M ;

Bernard, JP ;

Crussaire, JP ;

Dambier, G ;

de Bernardis, P ;

Delabrouille, J ;

De Luca, A ;

de Marcillac, P ;

Jegoudez, G ;

Lamarre, JM ;

Leblanc, J ;

Lepeltier, JP ;

Leriche, B ;

Mainella, G ;

Narbonne, J ;

Pajot, F ;

Pons, R ;

Puget, JL ;

Pujol, S ;

Recouvreur, G ;

Serra, G ;

Soglasnova, V ;

Torre, JP ;

Vozzi, B .

ASTRONOMY & ASTROPHYSICS SUPPLEMENT SERIES, 2000, 141 (03) :523-532

[4] Archeops:: a high resolution, large sky coverage balloon experiment for mapping cosmic microwave background anisotropies [J].

Benoît, A ;

Ade, P ;

Amblard, A ;

Ansari, R ;

Aubourg, E ;

Bartlett, J ;

Bernard, JP ;

Bhatia, RS ;

Blanchard, A ;

Bock, JJ ;

Boscaleri, A ;

Bouchet, FR ;

Bourrachot, A ;

Camus, P ;

Couchot, F ;

de Bernardis, P ;

Delabrouille, J ;

Désert, FX ;

Doré, O ;

Douspis, M ;

Dumoulin, L ;

Dupac, X ;

Filliatre, P ;

Ganga, K ;

Gannaway, F ;

Gautier, B ;

Giard, M ;

Giraud-Héraud, Y ;

Gispert, R ;

Guglielmi, L ;

Hamilton, JC ;

Hanany, S ;

Henrot-Versillé, S ;

Hristov, VV ;

Kaplan, J ;

Lagache, G ;

Lamarre, JM ;

Lange, AE ;

Madet, K ;

Maffei, B ;

Marrone, D ;

Masi, S ;

Murphy, JA ;

Naraghi, F ;

Nati, F ;

Perrin, G ;

Piat, M ;

Puget, JL ;

Santos, D ;

Sudiwala, RV .

ASTROPARTICLE PHYSICS, 2002, 17 (02) :101-124

[5]

Benoit A, 1997, ESA SP PUBL, V400, P497

[6] Planck pre-launch status: Design and description of the Low Frequency Instrument [J].

Bersanelli, M. ;

Mandolesi, N. ;

Butler, R. C. ;

Mennella, A. ;

Villa, F. ;

Aja, B. ;

Artal, E. ;

Artina, E. ;

Baccigalupi, C. ;

Balasini, M. ;

Baldan, G. ;

Banday, A. ;

Bastia, P. ;

Battaglia, P. ;

Bernardino, T. ;

Blackhurst, E. ;

Boschini, L. ;

Burigana, C. ;

Cafagna, G. ;

Cappellini, B. ;

Cavaliere, F. ;

Colombo, F. ;

Crone, G. ;

Cuttaia, F. ;

D'Arcangelo, O. ;

Danese, L. ;

Davies, R. D. ;

Davis, R. J. ;

De Angelis, L. ;

De Gasperis, G. C. ;

De La Fuente, L. ;

De Rosa, A. ;

De Zotti, G. ;

Falvella, M. C. ;

Ferrari, F. ;

Ferretti, R. ;

Figini, L. ;

Fogliani, S. ;

Franceschet, C. ;

Franceschi, E. ;

Gaier, T. ;

Garavaglia, S. ;

Gomez, F. ;

Gorski, K. ;

Gregorio, A. ;

Guzzi, P. ;

Herreros, J. M. ;

Hildebrandt, S. R. ;

Hoyland, R. ;

Hughes, N. .

ASTRONOMY & ASTROPHYSICS, 2010, 520

[7] A NOVEL BOLOMETER FOR INFRARED AND MILLIMETER-WAVE ASTROPHYSICS [J].

BOCK, JJ ;

CHEN, D ;

MAUSKOPF, PD ;

LANGE, AE .

SPACE SCIENCE REVIEWS, 1995, 74 (1-2) :229-235

[8]

BOUCHET FR, 1996, AIP C P, V348, P255

[9]

Bradshaw TW, 1997, ESA SP PUBL, V400, P465

[10]

Brienza D., 2006, Seventh International Workshop on Low Temperature Electronics, WOLTE-7, P283

← 1 2 3 4 5 6 →