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A&A 520, A4 (2010)DOI: 10.1051/0004-6361/200912853c○ ESO 2010Pre-launch status of the Planck missionAstronomy&AstrophysicsSpecial featurePlanck pre-launch status: Design and description of the LowFrequency InstrumentM. Bersanelli 1,2 ,N.Mandolesi 3 ,R.C.Butler 3 ,A.Mennella 1,2 ,F.Villa 3 ,B.Aja 4 ,E.Artal 4 ,E.Artina 5 ,C. Baccigalupi 6,15 ,M.Balasini 5 ,G.Baldan 5 ,A.Banday 7,32 ,P.Bastia 5 ,P.Battaglia 5 ,T.Bernardino 8 ,E.Blackhurst 9 ,L. Boschini 5 ,C.Burigana 3 ,G.Cafagna 5 ,B.Cappellini 1,2 ,F.Cavaliere 1 ,F.Colombo 5 ,G.Crone 10 ,F.Cuttaia 3 ,O. D ′ Arcangelo 11 ,L.Danese 6 ,R.D.Davies 9 ,R.J.Davis 9 ,L.DeAngelis 12 ,G.C.DeGasperis 13 ,L.DeLaFuente 4 ,A. De Rosa 3 ,G.DeZotti 14 ,M.C.Falvella 12 ,F.Ferrari 5 ,R.Ferretti 5 ,L.Figini 11 ,S.Fogliani 15 ,C.Franceschet 1 ,E. Franceschi 3 ,T.Gaier 16 ,S.Garavaglia 11 ,F.Gomez 17 ,K.Gorski 16 ,A.Gregorio 18 ,P.Guzzi 5 ,J.M.Herreros 17 ,S. R. Hildebrandt 17 ,R.Hoyland 17 ,N.Hughes 19 ,M.Janssen 16 ,P.Jukkala 19 ,D.Kettle 9 ,V.H.Kilpiä 19 ,M.Laaninen 20 ,P. M. Lapolla 5 ,C.R.Lawrence 16 ,D.Lawson 9 ,J.P.Leahy 9 ,R.Leonardi 21 ,P.Leutenegger 5 ,S.Levin 16 ,P.B.Lilje 22 ,S. R. Lowe 9 ,P.M.Lubin 21 ,D.Maino 1 ,M.Malaspina 3 ,M.Maris 15 ,J.Marti-Canales 10 ,E.Martinez-Gonzalez 8 ,A. Mediavilla 4 ,P.Meinhold 21 ,M.Miccolis 5 ,G.Morgante 3 ,P.Natoli 13 ,R.Nesti 23 ,L.Pagan 5 ,C.Paine 16 ,B. Partridge 24 ,J.P.Pascual 4 ,F.Pasian 15 ,D.Pearson 16 ,M.Pecora 5 ,F.Perrotta 15,6 ,P.Platania 11 ,M.Pospieszalski 25 ,T. Poutanen 26,27,28 ,M.Prina 16 ,R.Rebolo 17 ,N.Roddis 9 ,J.A.Rubiño-Martin 17 ,M.J.Salmon 8 ,M.Sandri 3 ,M. Seiffert 16 ,R.Silvestri 5 ,A.Simonetto 11 ,P.Sjoman 19 ,G.F.Smoot 29 ,C.Sozzi 11 ,L.Stringhetti 3 ,E.Taddei 5 ,J. Tauber 30 ,L.Terenzi 3 ,M.Tomasi 1 ,J.Tuovinen 31 ,L.Valenziano 3 ,J.Varis 31 ,N.Vittorio 13 ,L.A.Wade 16 ,A. Wilkinson 9 ,F.Winder 9 ,A.Zacchei 15 ,andA.Zonca 1,2(Affiliations can be found after the references)Received 8 July 2009 / Accepted 15 December 2009ABSTRACTIn this paper we present the Low Frequency Instrument (LFI), designed and developed as part of the Planck space mission, the ESA programmededicated to precision imaging of the cosmic microwave background (CMB). Planck-LFI will observe the full sky in intensity and polarisationin three frequency bands centred at 30, 44 and 70 GHz, while higher frequencies (100−850 GHz) will be covered by the HFI instrument. TheLFI is an array of microwave radiometers based on state-of-the-art indium phosphide cryogenic HEMT amplifiers implemented in a differentialsystem using blackbody loads as reference signals. The front end is cooled to 20 K for optimal sensitivity and the reference loads are cooled to4Ktominimiselow-frequencynoise.WeprovideanoverviewoftheLFI,discuss the leading scientific requirements, and describe the designsolutions adopted for the various hardware subsystems. The main drivers of theradiometric,optical,andthermaldesignarediscussed,includingthe stringent requirements on sensitivity, stability, and rejection of systematic effects. Further details on the key instrument units and the results ofground calibration are provided in a set of companion papers.Key words. cosmic microwave background – cosmology: observations – space vehicles: instruments1. IntroductionObservations of the cosmic microwave background (CMB) haveplayed a central role in the enormous progress of cosmologyin the past few decades. Technological developments in bothcoherent radio receivers and bolometric detectors have supportedan uninterrupted chain of successful experiments, fromthe initial discovery (Penzias & Wilson 1965) uptothepresentgeneration of precision measurements. Following COBE 1 andWMAP 2 ,thePlanck 3 satellite, launched on 14 May 2009, is thenext-generation space mission dedicated to CMB observations.1 http://lambda.gsfc.nasa.gov/product/cobe/2 http://map.gsfc.nasa.gov/3 Planck (http://www.esa.int/Planck) is a project of theEuropean Space Agency – ESA – with instruments provided by two scientificConsortia funded by ESA member states (in particular the leadcountries: France and Italy) with contributions from NASA (USA), andThe Planck instruments are designed to extract all the cosmologicalinformation encoded in the CMB temperature anisotropieswith an accuracy set by cosmic variance and astrophysical confusionlimits, and to push polarisation measurements well beyondpreviously reached results. Planck will image the sky innine frequency bands across the CMB blackbody peak, leadingto a full-sky map of the CMB temperature fluctuations withsignal-to-noise >10 and angular resolution
A&A 520, A4 (2010)In addition, all Planck bands between 30 and 350 GHz are sensitiveto linear polarisation.The imaging power of Planck is sized to extract the temperaturepower spectrum with high precision over the entire angularrange dominated by primordial fluctuations. This will lead toaccurate estimates of cosmological parameters that describe thegeometry, dynamics, and matter-energy content of the universe.The Planck polarisation measurements are expected to delivercomplementary information on cosmological parameters and toprovide a unique probe of the thermal history of the universein the early phase of structure formation. Planck will also testthe inflationary paradigm with unprecedented sensitivity throughstudies of non-Gaussianity and of B-mode polarisation as a signatureof primordial gravitational waves (Planck Collaboration2005).The wide frequency range of Planck is required primarilyto ensure accurate discrimination of foreground emissions fromthe cosmological signal. However, the nine Planck maps willalso represent a rich data set for galactic and extragalactic astrophysics.Up to now, no single technology can reach the requiredperformances in the entire Planck frequency range. Forthis reason two complementary instruments are integrated at thePlanck focal plane exploiting state-of-the-art radiometric andbolometric detectors in their best windows of operation. TheLow Frequency Instrument (LFI), described in this paper, coversthe 27−77 GHz range with a radiometer array cooled to 20 K.The High Frequency Instrument (HFI) will observe in six bandsin the 90−900 GHz range with a bolometer array cooled to 0.1 K(Lamarre et al. 2010). The two instruments share the focal planeof a single telescope, a shielded off-axis dual reflector Gregoriansystem with 1.5 × 1.9 m primary aperture (Tauber et al. 2010b).The design of the Planck satellite and mission plan is largelydriven by the extreme thermal requirements imposed by the instruments.The cold payload enclosure (
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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, A1 (2010)Fig. 2. An artist
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A&A 520, A1 (2010)Table 4. Summary
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A&A 520, A12 (2010)Table 1. Summary
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arrangement was also constrained by
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