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A&A 520, A12 (2010)Fig. 19. Broad-band (68 frequencies) 545-2 multi-mode power beam.Bottom figure is on a different X-Y scale (both in degrees). Color scale:un-normalised gain. Contours in dB respectively to maximum.Table 9. Single-mode channels spillover calculations (in %).Fig. 20. Main beam intensity maps for the polarised detector 143-1a atthe central frequency of 143 GHz. Same caption than for Fig. 16.Pixel Measurement Ideal Worst case Medianfrequency spillover spillover spillover100-1a 100 GHz 0.36 0.42 0.39100-3a 100 GHz 0.29 0.43 0.36143-1a 143 GHz 0.32 0.45 0.38217-8a 240 GHz 0.24 0.43 0.33217-3u 240 GHz 0.24 1.08 0.66353-5a 308 GHz 0.07 0.08 0.075Notes. Only results for horn types showing some discrepancies betweenmodel and experimental power patterns are shown. The suffix “a”denotesthe beam associated with the a detector of a PSB while “u” isrelated to an unpolarised pixel.Table 10. Spillover calculations (in %) of the high frequency channelsassuming theoretical horn beam patterns.Channel Edge taper Angle Average Spilloverfrequency (deg) %545 GHz 26 0.3857 GHz 27 0.038. ConclusionsWe have described the design optimisation of the cold optics andof the focal plane unit of Planck-HFI. The measured optical performancesof the resulting instrument flight model are presented,together with beam simulations based on the perfect optical system.Fig. 21. Main beam intensity maps for the polarised detector 217-5a atthe central frequency of 217 GHz. Same caption than for Fig. 16.Page 14 of 15
B. Maffei et al.: Planck pre-launch status: HFI beam expectations from the optical optimisation of the focal planeand high frequency foreground removal, the lower measuredefficiencies (Table 5), still within the scientific requirements, areless of an issue.Some of the ground calibration data are still being analysedand the results will be combined with in-flight calibration in orderto get a more accurate knowledge of the instrument. Furtherpost-launch publications will then be available.Fig. 22. Main beam intensity maps for the polarised detector 353-3a atthe central frequency of 353 GHz. Same caption than for Fig. 16.Much original research both in terms of modelling and experimentalverification was required to develop horns that couldmatch the very demanding optical performance requirements ofPlanck (angular resolution, edge taper and spillover) while at thesame time minimizing the length of the long wavelength horns.This required the development of complex theoretical tools andapproaches to achieve an acceptable solution.Therelevantresultsfrom the calibration campaigns have been summarised andshow that most of the optical requirements are met.Concerning the single-mode channels, the optical efficiencyrequirement is met for all but some of the 353 GHz detectionassemblies, and analysis is still ongoing in order to get a betterunderstanding of these. Most of the lower frequency pixels exceedthe goals. It is important to note (Lamarre et al. 2010) thatthe measured NETs show that the overall sensitivities exceedthe goal in most cases. Simulations show that only the 100 GHzbeams have a slightly larger beam width than required (9.6 arcmininstead of 9.2), and that all but one detection assembly hasalargerspilloverthanrequired(1%insteadof0.5%).In this paper we also described in broad terms the developmentand performance of the unique multi-mode channelsfor HFI, specially designed to have higher throughput than theCMB channels in order to increase the sensitivity, while matchingthe desired non-diffraction limited resolution. In particularthe 857 GHz horns, although challenging to manufacture (thecorrugation period is of the order of 60 microns), were shown tohave predicted beam patterns that match the resolution and edgetaper requirements with significantly improved throughput overasingle-modedesign.Thedetailsofthedesignandpredictedperformance of these channels (at 545 GHz and 857 GHz) willbe presented in a future paper (Murphy et al. 2010). Becausethese channels are mainly dedicated to point source detectionsAcknowledgements. The authors would like to acknowledge the support fromSTFC, CNRS, CNES, NASA, Enterprise Ireland and Science FoundationIreland.The authors extend their gratitude to numerous engineers and scientists who havecontributed to the design, development, construction or evaluation of HFI.ReferencesAde, P. A. R., Pisano, G., Tucker, C., et al. 2006, Proc. SPIE, 6275Ade, P. A. R., Savini, G., Sudiwala, R., et al. 2010, A&A, 520, A11Benoit, A., Ade, P. A. R., Amblard, A., et al. 2002, Astropart. Phys., 17, 101Bersanelli, M., Mandolesi, N. Butler, R. C., et al. 2010, A&A, 520, A4Bock, J. J., Chen, D., Mauskopf, P. D., et al. 1995, Space Sci. Rev., 74, 229Brossard, J. 2001, Ph.D. ThesisBrossard, J., Yurchenko, V., Gleeson, E., et al. 2004, Proc. 5th ICSO, ESA SP-554, 333Catalano, A. 2008, Ph.D. ThesisChurch, S. E., Philhour, B. J., Lange, A. E., et al. 1996, Proc. 30th ESLABsymposium on Submillimetre and Far-Infrared Space Instrumentation, ESA-ESTEC, 77Clarricoats, P. J. B., & Olver, A. D. 1984, Corrugated horns for microwaveantennas, ed. PeregrinusColgan, R. 2001, Electromagnetic and Quasi-Optical Modelling of HornAntennas for Far-IR Space Applications, Ph.D. Thesis, NUI MaynoothD’Arcangelo, O., Garavalia, S., Simonetto, A., et al. 2005, ExperimentalAstronomy, 16, 165de Bernardis, P., Ade, P. A. R., Bock, J. J., et al. 2000, Nature, 404, 955del Rio Bocio, C., Gonzalo, R., Sorolla Ayza, M., et al. 1999, IEEE Trans.Antennas Propag., 47, 1440Dodelson, S. 2003, Modern Cosmology (Amsterdam: Academic Press)Fargant, G., Dubruel, D., Cornut, M., et al. 2000, SPIE Proc., 4013, 69Gleeson, E. 2004, Single and Multi-moded Corrugated Horn Design for CosmicMicrowave Background Experiments, Ph.D. Thesis, NUI MaynoothHuffenberger, K. M., Eriksen, H. K., Hansen, F. K., et al. 2008, ApJ, 688, 1Holmes, W. A., Bock, J. J., Crill, B. P., et al. 2008, Appl. Opt., 47, 5996Jones, W. C., Bhatia, R., Bock, J. J., et al. 2003, Proc. SPIE, 4855, 227Lamarre, J. M., Puget, J. L., Bouchet, F., et al. 2003, New Astr. Rev., 47, 1017Lamarre, J. M., Puget, J. L., Ade, P. A. R., et al. 2010, A&A, 520, A9Maffei, B., Ade, P. A. R., Tucker, C. E., et al. 2000, Int. J. Infrared and Millimetrewaves, 21, 2023Maffei, B., Pisano, G., Haynes, V., et al. 2008 Proc. SPIE, 7020Murphy, J. A., Colgan, R., O’Sullivan, C., et al. 2001, Infrared Phys. Technol.,42, 515Murphy, J. A., et al. 2010, Journal of Instrumentation, submittedNoviello, F. 2008, Optical Performance of the ESA Planck Surveyor andTechniques for the Study of the Cosmic Microwave Background, Ph.D.Thesis, NUI MaynoothOlver, A. D., Clarricoats, P. J. B., Kishk, A. A., et al. 1994, Microwave Hornsand Feeds (IEEE Press)The Planck community, Blue Book: Planck the Scientific Programme, www.rssd.esa.int/SA/PLANCK/docs/Bluebook-ESA-SCI(2005)1_V2.pdfPontoppidan, K. 2005, GRASP9 Technical Description, TICRA EngineeringConsultantsRosset, C. 2004, Conference: XXXIXth Rencontres de Moriond, Exploring theUniverse, La ThuileRosset, C., Yurchenko, V., Delabrouille, J., et al. 2007, A&A, 464, 405Rosset, C., Tristam, M., Ponthieu, N., et al. 2010, A&A, 520, A13Schroeder, D. J. 2000, Astronomical Optics (San Diego: Academic Press)Sudiwala, R. V., Maffei, B., Griffin, M. J., et al. 2000, Nucl. Instr. Methods Phys.Res., Sect. A, 444, 408Tauber, J. A., Norgaard-Nielsen, H. U., Ade, P. A. R., et al. 2010a, A&A, 520,A2Tauber, J. A., Mandolesi, N., Puget, J.-L., et al. 2010b, A&A, 520, A1Woodcraft, A. L., Sudiwala, R. V., Griffin, M. J., et al. 2002, Int. J. Infrared andMillimeter Waves, 23, 575Yun, M., Bock, J. J., Holmes, W., et al. 2004, J. Vac. Sci. Technol. B, 22, 220Yurchenko, V. B., Murphy, J. A., & Lamarre, J. M., et al. 2004a, Proc. SPIE,5487, 542Yurchenko, V. B., Murphy, J. A., Lamarre, J. M., et al. 2004b, Int. J. Infrared andMillimeter Waves, 25, 601Page 15 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, A1 (2010)Fig. 2. An artist
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A&A 520, A1 (2010)Fig. 4. Planck fo
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A&A 520, A1 (2010)Fig. 6. The Planc
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A&A 520, A1 (2010)Table 4. Summary
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A&A 520, A1 (2010)three frequency c
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A&A 520, A1 (2010)Fig. 12. The left
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A&A 520, A1 (2010)Fig. 14. Left pan
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A&A 520, A1 (2010)flux limit of the
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A&A 520, A1 (2010)- University of C
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A&A 520, A1 (2010)57 Instituto de A
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A&A 520, A2 (2010)Fig. 1. (Left) Th
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A&A 520, A2 (2010)Table 2. Predicte
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Table 3. Predicted in-flight main b
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A&A 520, A2 (2010)materials. Theref
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A&A 520, A2 (2010)Fig. 11. Comparis
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A&A 520, A2 (2010)Table 5. Inputs u
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A&A 520, A2 (2010)Table 7. Optical
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A&A 520, A2 (2010)5 Università deg
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A&A 520, A3 (2010)Horizon 2000 medi
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A&A 520, A3 (2010)Fig. 1. CMB tempe
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A&A 520, A3 (2010)Ω ch 2τn s0.130
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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, A3 (2010)features of the r
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A&A 520, A3 (2010)Fig. 13. Level 2
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A&A 520, A3 (2010)GUI = graphical u
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A&A 520, A3 (2010)23 Centre of Math
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A&A 520, A4 (2010)In addition, all
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A&A 520, A4 (2010)Table 2. Sensitiv
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A&A 520, A4 (2010)Fig. 15. DAE bias
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A&A 520, A4 (2010)Table 10. Main ch
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Table 13. Principal requirements an
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A&A 520, A5 (2010)DOI: 10.1051/0004
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A. Mennella et al.: LFI calibration
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D.1. Step 1-extrapolate uncalibrate
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F. Villa et al.: Calibration of LFI
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M. Sandri et al.: Planck pre-launch
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A&A 520, A7 (2010)Fig. 8. Footprint
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-30-40-30-6-3-20A&A 520, A7 (2010)0
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A&A 520, A7 (2010)Table 4. Galactic
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A&A 520, A8 (2010)inflation, giving
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A&A 520, A8 (2010)ways the most str
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unmodelled long-timescale thermally
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A&A 520, A8 (2010)Fig. 5. Polarisat
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A&A 520, A8 (2010)where S stands fo
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stored in the LFI instrument model,
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A&A 520, A8 (2010)comparable in siz
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A&A 520, A8 (2010)Table B.1. Main b
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A&A 520, A8 (2010)Bond, J. R., Jaff
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A&A 520, A9 (2010)- (v) an optical
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