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A&A 520, A9 (2010)20 Laboratoire de Physique Subatomique et de Cosmologie (LPSC),Univ. Joseph Fourier Grenoble I, CNRS/IN2P3, Institut NationalPolytechnique de Grenoble, 53 Avenue des Martyrs, 38026Grenoble Cedex, France21 The University of Manchester, JBCA, School of Physics andAstronomy, Manchester M13 9PL, UK22 Department of Experimental Physics, National University of Ireland(NUI), Maynooth, Co. Kildare, Ireland23 Optical Science Laboratory, University College London (UCL),Gower Street, WC1E 6BT London, UK24 SUPA, Institute of Astronomy, University of Edinburgh, BlackfordHill, Edinburgh EH9 3HJ, UK25 Institute of Radiophysics and Electronics, NAS of Ukraine,12 Proskura St., 61085 Kharkov, Ukraine26 CEA, CE Saclay, IRFU/Service de Physique des Particules,91191 Gif-sur-Yvette Cedex, FrancePage 20 of 20
A&A 520, A10 (2010)DOI: 10.1051/0004-6361/200913203c○ ESO 2010Pre-launch status of the Planck missionAstronomy&AstrophysicsSpecial featurePlanck pre-launch status: HFI ground calibrationF. Pajot 1 ,P.A.R.Ade 2 ,J.-L.Beney 3 ,E.Bréelle 4 ,D.Broszkiewicz 4 ,P.Camus 5 ,C.Carabétian 1 ,A.Catalano 4 ,A. Chardin 1 ,M.Charra 1 ,J.Charra 1,† ,R.Cizeron 3 ,F.Couchot 3 ,A.Coulais 6 ,B.P.Crill 7,8 ,K.Dassas 1 ,J.Daubin 3 ,P. de Bernardis 9 ,P.deMarcillac 1 ,J.-M.Delouis 10 ,F.-X.Désert 11 ,P.Duret 1 ,P.Eng 1 ,C.Evesque 1 ,J.-J.Fourmond 1 ,S. François 1 ,M.Giard 12 ,Y.Giraud-Héraud 4 ,L.Guglielmi 4 ,G.Guyot 1 ,J.Haissinski 3 ,S.Henrot-Versillé 3 ,V. Hervier 1 ,W.Holmes 8 ,W.C.Jones 8,13 ,J.-M.Lamarre 6 ,P.Lami 1 ,A.E.Lange 7,8,† ,M.Lefebvre 1 ,B.Leriche 1 ,C. Leroy 1 ,J.Macias-Perez 14 ,T.Maciaszek 15 ,B.Maffei 16 ,A.Mahendran 1 ,B.Mansoux 3 ,C.Marty 12 ,S.Masi 9 ,C. Mercier 1 ,M.-A.Miville-Deschenes 1 ,L.Montier 12 ,C.Nicolas 1 ,F.Noviello 1 ,O.Perdereau 3 ,F.Piacentini 9 ,M. Piat 4 ,S.Plaszczynski 3 ,E.Pointecouteau 12 ,R.Pons 12 ,N.Ponthieu 1 ,J.-L.Puget 1 ,D.Rambaud 12 ,C.Renault 14 ,J.-C. Renault 10 ,C.Rioux 1 ,I.Ristorcelli 12 ,C.Rosset 3 ,G.Savini 17 ,R.Sudiwala 2 ,J.-P.Torre 1 ,M.Tristram 3 ,D.Vallée 4 ,M. Veneziani 4 ,andD.Yvon 18(Affiliations can be found after the references)Received 28 August 2009 / Accepted 15 March 2010ABSTRACTContext. The Planck satellite was successfully launched on May 14th 2009. We have completed the pre-launch calibration measurements of theHigh Frequency Instrument (HFI) on board Planck and their processing.Aims. We present the results ot the pre-launch calibration of HFI in which we have multiple objectives. First, we determine instrumental parametersthat cannot be measured in-flight and predict parameters that can. Second, we take the opportunity to operate and understand the instrument underawiderangeofanticipatedoperatingconditions.Finally,weestimatetheperformanceoftheinstrumentbuilt.Methods. We obtained our pre-launch calibration results by characterising the component and subsystems, then by calibrating the focal plane atIAS (Orsay) in the Saturne simulator, and later from the tests at the satellite level carried out in the CSL (Liège) cryogenic vacuum chamber. Wedeveloped models to estimate the instrument pre-launch parameters when no measurement could be performed.Results. We reliably measure the Planck-HFI instrument characteristics and behaviour, and determine the flight nominal setting of all parameters.The expected in-flight performance exceeds the requirements and is close or superior to the goal specifications.Key words. cosmic microwave background – space vehicles: instruments – submillimeter: general1. IntroductionThe Planck satellite 1 ,launchedonMay14th2009,willmapthesky in 9 frequency bands between 30 GHz and 1 THz. It is thethird generation satellite dedicated to the study of the CMB (cosmicmicrowave background) after COBE and WMAP. Beeingthe high frequency instrument on-board Planck,HFIcoversfrequenciesbetween 100 and 857 GHz. The HFI receiver is basedon cryogenic bolometric detectors operating at 0.1 K, a fractionof which are sensitive to polarisation. Pre-launch calibrationis an essential step in characterising the instrument, estimatingthe sensitivity, optimising its operational parameters, and identifyingits systematics. The calibration method of balloon-borneand orbital instruments in this frequency range is not well established.A diverse range of strategies have had to be devopedfor different instruments and missions, such as COBE FIRAS(Fixsen et al. 1994), PRONAOS (Pajot et al. 2006), Archeops1 Planck (http://www.esa.int/Planck) isanESAprojectwithinstrumentsprovided by two scientific Consortia funded by ESA memberstates (in particular the lead countries: France and Italy) with contributionsfrom NASA (USA), and telescope reflectors provided in collaborationbetween ESA and a scientific Consortium led and funded byDenmark.(Benoît et al. 2002), Boomerang (Masi et al. 2006), or WMAP(Page et al. 2003). This paper describes the method and resultsof the pre-launch calibration of the Planck-HFI at the instrumentlevel. The Planck mission, the satellite, and its instruments aredescribed in separate compagnion papers of this issue. In particular,the mission is detailed in Tauber (2010a), the LFI instrumentin Bersanelli et al. (2010), and its ground calibration inMennella et al. (2010).The HFI instrument consists of 54 bolometers distributed betweensix frequencies of bandwidth ∆ν/ν = 1/3, of which 32are polarisation-sensitive bolometers (PSBs), 20 are unpolarizedspider-web bolometers (SWBs), and two are dark bolometersmonitoring common-mode systematics. The polarised detectorsare oriented in the focal plane to enable the determination of thelinear polarization using combinations of three or more channels.The detectors couple to the telescope by means of 36 backto-backhorn assemblies, including the optical filters defining thefrequency bands. The bolometers, 16 thermometers on the 4 K,1.6 K, and 100 mK thermal stages, a reference resistor, and areference capacitor are read out by low noise electronics at thenominal acquisition rate (roughly 180 Hz). Four thermometerson the 4 K stage monitor the temperature of the HFI close tothe location of the reference optical loads used by LFI. OtherArticle published by EDP Sciences Page 1 of 15
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ABSTRACTThe European Space Agency
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