Planck pre-launch status: The optical architecture of the HFI

被引：23

作者：

Ade, P. A. R. ^{[1
]}

Savini, G. ^{[1
,2
]}

Sudiwala, R. ^{[1
]}

Tucker, C. ^{[1
]}

Catalano, A. ^{[3
]}

Church, S. ^{[4
]}

Colgan, R. ^{[5
]}

Desert, F. X. ^{[6
]}

Gleeson, E. ^{[5
]}

Jones, W. C. ^{[7
,8
]}

Lamarre, J. -M.

Lange, A. ^{[7
,9
]}

Longval, Y. ^{[10
]}

Maffei, B. ^{[11
]}

Murphy, J. A. ^{[5
]}

Noviello, F. ^{[10
]}

Pajot, F. ^{[10
]}

Puget, J. -L. ^{[10
]}

Ristorcelli, I. ^{[12
]}

Woodcraft, A. ^{[13
]}

Yurchenko, V. ^{[5
,14
]}

机构：

[1] Cardiff Univ, Astron & Instrumentat Grp, Cardiff, S Glam, Wales

[2] UCL, Opt Sci Lab, London WC1E 6BT, England

[3] Observ Paris, CNRS, LERMA, F-75014 Paris, France

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

[5] NUI, Dept Expt Phys, Maynooth, Kildare, Ireland

[6] CNRS, Astrophys Lab, Observ Grenoble LOAG, F-38041 Grenoble 9, France

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

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

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

[10] Univ Paris 11, CNRS, IAS, Inst Astrophys Spatiale, F-91405 Orsay, France

[11] Univ Manchester, JBCA, Sch Phys & Astron, Manchester M13 9PL, Lancs, England

[12] CNRS, CESR, F-31038 Toulouse 4, France

[13] Univ Edinburgh, SUPA, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland

[14] NAS Ukraine, Inst Radiophys & Elect, UA-61085 Kharkov, Ukraine

来源：

ASTRONOMY & ASTROPHYSICS | 2010年 / 520卷

基金：

爱尔兰科学基金会;

关键词：

cosmic microwave background; space vehicles: instruments; instrumentation: detectors; instrumentation: polarimeters; submillimeter: general; techniques: photometric;

D O I：

10.1051/0004-6361/200913039

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The Planck High Frequency Instrument, HFI, has been designed to allow a clear unobscured view of the CMB sky through an off-axis Gregorian telescope. The prime science target is to measure the polarized anisotropy of the CMB with a sensitivity of 1 part in 10(6) with a maximum spatial resolution of 5 arcmin (C(l) similar to 3000) in four spectral bands with two further high-frequency channels measuring total power for foreground removal. These requirements place critical constraints on both the telescope configuration and the receiver coupling and require precise determination of the spectral and spatial characteristics at the pixel level, whilst maintaining control of the polarisation. To meet with the sensitivity requirements, the focal plane needs to be cooled with the optics at a few Kelvin and detectors at 100 mK. To limit inherent instrumental thermal emission and diffraction effects, there is no vacuum window, so the detector feedhorns view the telescope secondary directly. This requires that the instrument is launched warm with the cooler chain only being activated during its cruise to L2. Here we present the novel optical configuration designed to meet with all the above criteria.

引用

页数：7

共 12 条

[1]

Ade P. A. R., 2006, P SPIE, V6275

[2]

CHURCH SE, 1996, P 30 ESLAB S ESTEC N

[3] OFFSET MULTI-REFLECTOR ANTENNAS WITH PERFECT PATTERN SYMMETRY AND POLARIZATION DISCRIMINATION [J].

DRAGONE, C .

BELL SYSTEM TECHNICAL JOURNAL, 1978, 57 (07) :2663-2684

[4]

*ESA SCI, 2005, ESASCI20051

[5] A polarization sensitive bolometric receiver for observations of the cosmic microwave background [J].

Jones, WC ;

Bhatia, RS ;

Bock, JJ ;

Lange, AE .

MILLIMETER AND SUBMILLIMETER DETECTORS FOR ASTRONOMY, 2003, 4855 :227-238

[6] Planck pre-launch status: The HFI instrument, from specification to actual performance [J].

Lamarre, J. -M. ;

Puget, J. -L. ;

Ade, P. A. R. ;

Bouchet, F. ;

Guyot, G. ;

Lange, A. E. ;

Pajot, F. ;

Arondel, A. ;

Benabed, K. ;

Beney, J. -L. ;

Benoit, A. ;

Bernard, J. -Ph. ;

Bhatia, R. ;

Blanc, Y. ;

Bock, J. J. ;

Breelle, E. ;

Bradshaw, T. W. ;

Camus, P. ;

Catalano, A. ;

Charra, J. ;

Charra, M. ;

Church, S. E. ;

Couchot, F. ;

Coulais, A. ;

Crill, B. P. ;

Crook, M. R. ;

Dassas, K. ;

de Bernardis, P. ;

Delabrouille, J. ;

de Marcillac, P. ;

Delouis, J. -M. ;

Desert, F. -X. ;

Dumesnil, C. ;

Dupac, X. ;

Efstathiou, G. ;

Eng, P. ;

Evesque, C. ;

Fourmond, J. -J. ;

Ganga, K. ;

Giard, M. ;

Gispert, R. ;

Guglielmi, L. ;

Haissinski, J. ;

Henrot-Versille, S. ;

Hivon, E. ;

Holmes, W. A. ;

Jones, W. C. ;

Koch, T. C. ;

Lagardere, H. ;

Lami, P. .

ASTRONOMY & ASTROPHYSICS, 2010, 520

[7] Planck pre-launch status: HFI beam expectations from the optical optimisation of the focal plane [J].

Maffei, B. ;

Noviello, F. ;

Murphy, J. A. ;

Ade, P. A. R. ;

Lamarre, J. -M. ;

Bouchet, F. R. ;

Brossard, J. ;

Catalano, A. ;

Colgan, R. ;

Gispert, R. ;

Gleeson, E. ;

Haynes, C. V. ;

Jones, W. C. ;

Lange, A. E. ;

Longval, Y. ;

McAuley, I. ;

Pajot, F. ;

Peacocke, T. ;

Pisano, G. ;

Puget, J. -L. ;

Ristorcelli, I. ;

Savini, G. ;

Sudiwala, R. ;

Wylde, R. J. ;

Yurchenko, V. .

ASTRONOMY & ASTROPHYSICS, 2010, 520

[8] Radiation patterns of multi-moded corrugated horns for far-IR space applications [J].

Murphy, JA ;

Colgan, R ;

O'Sullivan, C ;

Maffei, B ;

Ade, P .

INFRARED PHYSICS & TECHNOLOGY, 2001, 42 (06) :515-528

[9]

OLVER AD, 1994, IEE ELECTROMAGNETIC, V39, P490

[10] Planck pre-launch status: HFI ground calibration [J].

Pajot, F. ;

Ade, P. A. R. ;

Beney, J. -L. ;

Breelle, E. ;

Broszkiewicz, D. ;

Camus, P. ;

Carabetian, C. ;

Catalano, A. ;

Chardin, A. ;

Charra, M. ;

Charra, J. ;

Cizeron, R. ;

Couchot, F. ;

Coulais, A. ;

Crill, B. P. ;

Dassas, K. ;

Daubin, J. ;

de Bernardis, P. ;

de Marcillac, P. ;

Delouis, J. -M. ;

Desert, F. -X. ;

Duret, P. ;

Eng, P. ;

Evesque, C. ;

Fourmond, J. -J. ;

Francois, S. ;

Giard, M. ;

Giraud-Heraud, Y. ;

Guglielmi, L. ;

Guyot, G. ;

Haissinski, J. ;

Henrot-Versille, S. ;

Hervier, V. ;

Holmes, W. ;

Jones, W. C. ;

Lamarre, J. -M. ;

Lami, P. ;

Lange, A. E. ;

Lefebvre, M. ;

Leriche, B. ;

Leroy, C. ;

Macias-Perez, J. ;

Maciaszek, T. ;

Maffei, B. ;

Mahendran, A. ;

Mansoux, B. ;

Marty, C. ;

Masi, S. ;

Mercier, C. ;

Miville-Deschenes, M. -A. .

ASTRONOMY & ASTROPHYSICS, 2010, 520

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