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P. A. R. Ade et al.: Planck pre-launch status: the optical architecture of the HFIFig. 9. Plot of thermal optical loading for the different spectral bands.The red line is the loading due to the emission of the warmer stages ofthe optics and pink is the loading from the CMB emission. Dark andlight blue are respectively the loading contribution from the telescopeat the nominal (60 K) and expected (45 K) temperature. Dotted linesrepresent the same for the polarisation sensitive detectors.both need to be at 100 mK to minimize out of band power at thedetectors. The other edges are placed at 1.6 K and 4 K to distributethe power loading in accordance with heat lift margins.The target was to cool the telescope using passive technologyto a temperature below 50 K such that the photon noisefrom the primary and secondary mirrors with an assumed
A&A 520, A12 (2010)DOI: 10.1051/0004-6361/200912999c○ ESO 2010Pre-launch status of the Planck missionAstronomy&AstrophysicsSpecial featurePlanck pre-launch status: HFI beam expectations from the opticaloptimisation of the focal planeB. Maffei 1 ,F.Noviello 2,3 ,J.A.Murphy 3 ,P.A.R.Ade 4 ,J.-M.Lamarre 5 ,F.R.Bouchet 12 ,J.Brossard 7,6 ,A.Catalano 5 ,R. Colgan 3 ,R.Gispert 2 ,E.Gleeson 3 ,C.V.Haynes 1 ,W.C.Jones 8,10 ,A.E.Lange 8,† ,Y.Longval 2 ,I.McAuley 3 ,F. Pajot 2 ,T.Peacocke 3 ,G.Pisano 1 ,J.-L.Puget 2 ,I.Ristorcelli 6 ,G.Savini 9,4 ,R.Sudiwala 4 ,R. J. Wylde 13 ,andV.Yurchenko 3,111 The University of Manchester, JBCA, School of Physics and Astronomy, Manchester M13 9PL, UKe-mail: Bruno.maffei@manchester.ac.uk2 Institut d’Astrophysique Spatiale, CNRS & Université Paris 11, Bâtiment 121, 91405 Orsay, France3 NUI Maynooth, Department of Experimental Physics, Maynooth, Co. Kildare, Ireland4 Cardiff University, School of Physics and Astronomy, The Parade, Cardiff CF24 3AA, UK5 LERMA, CNRS, Observatoire de Paris, 61 Avenue de l’Observatoire, 75014 Paris, France6 CESR, CNRS-Université, 9 Av. du colonel Roche, BP44346, 31038 Toulouse Cedex 4, France7 Laboratoire de l’Accélérateur Linéaire, CNRS & Université Paris 11, Bâtiment 200, 91898 Orsay, France8 Caltech/JPL, Caltech Observational Cosmology, Mail code: 59-33, Pasadena, CA 91125, USA9 Optical Science Laboratory, Dept. of Physics and Astronomy, UCL, London, WC1E 6BT, UK10 Princeton University, Dept. of Physics, Princeton, NJ 08544, USA11 Institute of Radiophysics and Electronics, NAS of Ukraine, 12 Proskura St., 61085, Kharkov, Ukraine12 Institut d’Astrophysique de Paris, CNRS & Université Paris 6, 98bis Bd Arago, 75014 Paris, France13 School of Physics and Astronomy, North Haugh, St Andrews, Fife KY16 9SS, UKReceived 27 July 2009 / Accepted 26 January 2010ABSTRACTPlanck is a European Space Agency (ESA) satellite, launched in May 2009, which will map the cosmic microwave backgroundanisotropies in intensity and polarisation with unprecedented detail and sensitivity. It will also provide full-sky maps of astrophysicalforegrounds. An accurate knowledge of the telescope beam patterns is an essential element for a correct analysis of the acquiredastrophysical data. We present a detailed description of the optical design of the High Frequency Instrument (HFI) together with someof the optical performances measured during the calibration campaigns. We report on the evolution of the knowledge of the pre-launchHFI beam patterns when coupled to ideal telescope elements, and on their significance for the HFI data analysis procedure.Key words. space vehicles: instruments – submillimeter: general – telescopes – cosmic microwave background –instrumentation: polarimeters – instrumentation: detectors1. IntroductionThe primary objective of the Planck mission 1 (Tauber et al.2010b) istomeasurethetemperaturefluctuationsofthecosmicmicrowave background (CMB) with an accuracy limited only byastrophysical processes. This will greatly improve constraints onthe values of fundamental cosmological parameters, such as thedensity parameter Ω, theHubbleparameterH 0 and the cosmologicalconstant Λ. Inaddition,Planck will deliver a wealth ofinformation on the polarisationpropertiesoftheCMB.Becauseof its extended frequency coverage (30−857 GHz), Planck willimprove our understanding of foreground emissions from bothGalactic and extragalactic sources.1 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.The Planck payload is equipped with two focal plane instruments,the Low Frequency Instrument (LFI) operating in threefrequency bands at 30, 44 and 70 GHz (Bersanelli et al. 2010),and the High Frequency Instrument (HFI) operating in six frequencybands centred at 100, 143, 217, 353, 545 and 857 GHz(Lamarre et al. 2003, 2010). While all the detectors of LFI aredual-linearly-polarised, HFI contains both un-polarised (total intensity)and dual-linearly-polarised pixels. The detectors of thesetwo instruments are optically coupled to an off-axis dual-mirrortelescope through corrugated feedhorns (Tauber et al. 2010a).The primary mirror has a projected diameter of 1.5 m, whichconstitutes a dimensioning parameter of the satellite. The angularresolution of Planck, rangingfrom4.5to30arcmin,resultsfrom an under-illumination of the primary reflector that minimizethe spillover (see Sect. 3.2). Since the observed signal arrivingfrom an astronomical source (such as the CMB) will beconvolved with the beam response of the observing instrument,it is of paramount importance to acquire the best possible knowledgeof the instrument.Article published by EDP Sciences Page 1 of 15
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A&A 520, E1 (2010)DOI: 10.1051/0004
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ABSTRACTThe European Space Agency
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A&A 520, A3 (2010)Fig. 6. Integral
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A&A 520, A3 (2010)Table 2. LFI opti
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3.3.1. SpecificationsThe main requi
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A&A 520, A4 (2010)In addition, all
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A. Mennella et al.: LFI calibration
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-30-40-30-6-3-20A&A 520, A7 (2010)0
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