Planck early results. IV. First assessment of the High Frequency Instrument in-flight performance

被引:142
作者
Ade, P. A. R. [49 ]
Aghanim, N. [27 ]
Ansari, R. [42 ]
Arnaud, M. [37 ]
Ashdown, M. [3 ,36 ]
Aumont, J. [27 ]
Banday, A. J. [7 ,43 ,54 ]
Bartelmann, M. [43 ,53 ]
Bartlett, J. G. [2 ,34 ]
Battaner, E. [56 ]
Benabed, K. [28 ]
Benoit, A. [2 ,26 ]
Bernard, J. -P. [7 ,54 ]
Bersanelli, M. [16 ,21 ]
Bhatia, R. [4 ]
Bock, J. J. [8 ,34 ]
Bond, J. R. [5 ]
Borrill, J. [44 ,51 ]
Bouchet, F. R. [28 ]
Boulanger, F. [27 ]
Bradshaw, T. [47 ]
Breelle, E. [2 ]
Bucher, M. [2 ]
Camus, P. [26 ]
Cardoso, J. -F. [2 ,28 ,38 ,39 ]
Catalano, A. [1 ,2 ]
Challinor, A. [2 ,9 ,32 ,36 ]
Chamballu, A. [2 ,24 ]
Charra, J. [27 ]
Charra, M. [27 ]
Chary, R. -R. [25 ]
Chiang, C. [12 ]
Church, S. [52 ]
Clements, D. L. [24 ]
Colombi, S. [28 ]
Couchot, F. [42 ]
Coulais, A. [1 ]
Cressiot, C. [2 ]
Crill, B. P. [8 ,34 ]
Crook, M. [47 ]
de Bernardis, P. [15 ]
Delabrouille, J. [2 ]
Delouis, J. -M. [28 ]
Desert, F. -X. [23 ]
Dolag, K. [43 ]
Dole, H. [27 ]
Dore, O. [8 ,34 ]
Douspis, M. [27 ]
Efstathiou, G. [32 ]
Eng, P. [27 ]
机构
[1] Observ Paris, CNRS, LERMA, F-75014 Paris, France
[2] Univ Paris 07, CNRS, UMR 7164, Paris, France
[3] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England
[4] ALMA Santiago Cent Off, Santiago, Chile
[5] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada
[6] CNES, F-31401 Toulouse 9, France
[7] IRAP, CNRS, F-31028 Toulouse 4, France
[8] CALTECH, Pasadena, CA 91125 USA
[9] Univ Cambridge, DAMTP, Ctr Math Sci, Cambridge CB3 0WA, England
[10] CEA Saclay, DSM Irfu SPP, F-91191 Gif Sur Yvette, France
[11] Natl Space Inst, DTU Space, Copenhagen, Denmark
[12] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA
[13] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA
[14] Univ Illinois, Dept Phys, Urbana, IL USA
[15] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy
[16] Univ Milan, Dipartimento Fis, Milan, Italy
[17] ESO Vitacura, European So Observ, Santiago, Chile
[18] ESTEC, European Space Agcy, NL-2201 AZ Noordwijk, Netherlands
[19] INAF Osservatorio Astron Trieste, Trieste, Italy
[20] INAF IASF Bologna, Bologna, Italy
[21] INAF IASF Milano, Milan, Italy
[22] CNRS, Inst Sci Univers, INSU, F-75794 Paris 16, France
[23] Univ Grenoble 1, Grenoble CNRS INSU 1, UMR 5274, IPAG, F-38041 Grenoble, France
[24] Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, Blackett Lab, London SW7 2AZ, England
[25] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA
[26] Univ Grenoble 1, CNRS, Inst Neel, F-38041 Grenoble, France
[27] Univ Paris 11, CNRS, Inst Astrophys Spatiale, UMR8617, F-91405 Orsay, France
[28] Univ Paris 06, CNRS, UMR7095, Inst Astrophys Paris, Paris, France
[29] Fac Ciencies, CSIC IEEC, Inst Ciencies Espai, Bellaterra 08193, Spain
[30] Inst Radioastron Millimetrique IRAM, Granada 18012, Spain
[31] Inst Radioastron Millimetr IRAM, F-38406 Grenoble, France
[32] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England
[33] Inst Astrofis Canarias, Tenerife, Spain
[34] CALTECH, Jet Prop Lab, Pasadena, CA USA
[35] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England
[36] Kavli Inst Cosmol Cambridge, Cambridge CB3 0HA, England
[37] Univ Paris Diderot, CNRS, DSM, Lab AIM,IRFU,Serv Astrophys,CEA, F-91191 Gif Sur Yvette, France
[38] CNRS, Lab Traitement & Commun Informat, UMR 5141, F-75634 Paris, France
[39] Telecom ParisTech, F-75634 Paris, France
[40] Lab Astrophys Marseille, F-13388 Marseille 13, France
[41] Univ Grenoble 1, Inst Natl Polytech Grenoble, CNRS, Lab Phys Subatom & Cosmol,IN2P3, F-38026 Grenoble, France
[42] Univ Paris 11, CNRS, IN2P3, Lab Accelerateur Lineaire, F-91405 Orsay, France
[43] Max Planck Inst Astrophys, D-85741 Garching, Germany
[44] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA
[45] Natl Univ Ireland, Dept Expt Phys, Maynooth, Kildare, Ireland
[46] UCL, Opt Sci Lab, London, England
[47] Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England
[48] Univ Edinburgh, Inst Astron, SUPA, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland
[49] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales
[50] Russian Acad Sci, Space Res Inst IKI, Moscow, Russia
关键词
instrumentation: detectors; methods: data analysis; instrumentation: photometers; cosmic background radiation; cosmology: observations; PRE-LAUNCH STATUS; POWER SPECTRUM; ANISOTROPY; HFI; BOLOMETERS; CRYOCOOLER; RECEIVER; READOUT; SYSTEM;
D O I
10.1051/0004-6361/201116487
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
The Planck High Frequency Instrument (HFI) is designed to measure the temperature and polarization anisotropies of the cosmic microwave background and Galactic foregrounds in six similar to 30% bands centered at 100, 143, 217, 353, 545, and 857 GHz at an angular resolution of 10' (100 GHz), 7' (143 GHz), and 5' (217 GHz and higher). HFI has been operating flawlessly since launch on 14 May 2009, with the bolometers reaching 100 mK the first week of July. The settings of the readout electronics, including bolometer bias currents, that optimize HFI's noise performance on orbit are nearly the same as the ones chosen during ground testing. Observations of Mars, Jupiter, and Saturn have confirmed that the optical beams and the time responses of the detection chains are in good agreement with the predictions of physical optics modeling and pre-launch measurements. The Detectors suffer from a high flux of cosmic rays due to historically low levels of solar activity. As a result of the redundancy of Planck's observation strategy, the removal of a few percent of data contaminated by glitches does not significantly affect the instrumental sensitivity. The cosmic ray flux represents a significant and variable heat load on the sub-Kelvin stage. Temporal variation and the inhomogeneous distribution of the flux results in thermal fluctuations that are a probable source of low frequency noise. The removal of systematic effects in the time ordered data provides a signal with an average noise equivalent power that is 70% of the goal in the 0.6-2.5 Hz range. This is slightly higher than was achieved during the pre-launch characterization but better than predicted in the early phases of the project. The improvement over the goal is a result of the low level of instrumental background loading achieved by the optical and thermal design of the HFI.
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