Ade, P.A.R. and Aghanim, N. and Ansari, R. and Arnaud, M. and Ashdown, M. and Aumont, J. and Banday, A.J. and Bartelmann, M. and Bartlett, J.G. and Battaner, E. and Benabed, K. and Benoit, A. and Bernard, J.-P. and Bersanelli, M. and Bhatia, R. and Bock, J.J. and Bond, J.R. and Borrill, J. and Bouchet, F.R. and Boulanger, F. and Bradshaw, T. and Breelle, E. and Bucher, M. and Camus, P. and Cardoso, J.-F. and Catalano, A. and Challinor, A. and Chamballu, A. and Charra, J. and Charra, M. and Chary, R.-R. and Chiang, C. and Church, S. and Clements, D.L. and Colombi, S. and Couchot, F. and Coulais, A. and Cressiot, C. and Crill, B.P. and Crook, M. and De Bernardis, P. and Delabrouille, J. and Delouis, J.-M. and Desert, F.-X. and Dolag, K. and Dole, H. and Dore, O. and Douspis, M. and Efstathiou, G. and Eng, P. and Filliard, C. and Forni, O. and Fosalba, P. and Fourmond, J.-J. and Ganga, K. and Giard, M. and Girard, D. and Giraud-Héraud, Y. and Gispert, R. and Gorski, K.M. and Gratton, S. and Griffin, M. and Guyot, G. and Haissinski, J. and Harrison, D. and Helou, G. and Henrot-Versille, S. and Hernandez-Monteagudo, C. and Hildebrandt, S.R. and Hills, R. and Hivon, E. and Hobson, M. and Holmes, W.A. and Huffenberger, K.M. and Jaffe, A.H. and Jones, W.C. and Kaplan, J. and Kneissl, R. and Knox, L. and Lagache, G. and Lamarre, J.-M. and Lami, P. and Lange, A.E. and Lasenby, A. and Lavabre, A. and Lawrence, C.R. and Leriche, B. and Leroy, C. and Longval, Y. and Macias-Perez, J.F. and Maciaszek, T. and MacTavish, C.J. and Maffei, B. and Mandolesi, N. and Mann, R. and Mansoux, B. and Masi, S. and Matsumura, T. and McGehee, P. and Melin, J.-B. and Mercier, C. and Miville-Deschenes, M.-A. and Moneti, A. and Montier, L. and Mortlock, D. and Murphy, J.Anthony and Nati, F. and Netterfield, C.B. and Norgaard-Nielsen, H.U. and North, C. and Noviello, F. and Novikov, D. and Osborne, S. and Paine, C. and Pajot, F. and Patanchon, G. and Peacocke, T. and Pearson, T.J. and Perdereau, O. and Perotto, L. and Piacentini, F. and Piat, M. and Plaszczynski, S. and Pointecouteau, E. and Pons, R. and Ponthieu, N. and Prezeau, G. and Prunet, S. and Puget, J.-L. and Reach, W.T. and Renault, C. and Ristorcelli, I. and Rocha, G. and Rosset, C. and Roudier, G. and Rowan-Robinson, M. and Rusholme, B. and Santos, D. and Savini, G. and Schaefer, B.M. and Shellard, P. and Spencer, L. and Starck, J.-L. and Stassi, P. and Stolyarov, V. and Stompor, R. and Sudiwala, R. and Sunyaev, R. and Sygnet, J.-F. and Tauber, J.A. and Thum, C. and Torre, J.-P. and Touze, F. and Tristram, M. and van Leeuwen, B.-J. and Vibert, L. and Vibert, D. and Wade, L.A. and White, S.D.M. and Wiesemeyer, H. and Woodcraft, A. and Yurchenko, V. and Yvon, D. and Zacchei, A. (2011) Planck early results. IV. First assessment of the High Frequency Instrument in-flight performance. Astronomy & Astrophysics, 536 (A4). pp. 1-20. ISSN 0004-6361

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Abstract

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 ∼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.

Item Type:	Article
Keywords:	instrumentation; detectors – methods; data analysis – instrumentation; photometers – cosmic background radiation – cosmology; observations;
Academic Unit:	Faculty of Science and Engineering > Experimental Physics
Item ID:	4314
Depositing User:	Dr. Anthony Murphy
Date Deposited:	12 Apr 2013 14:28
Journal or Publication Title:	Astronomy & Astrophysics
Publisher:	EDP Sciences
Refereed:	Yes
URI:	Publisher
Use Licence:	This item is available under a Creative Commons Attribution Non Commercial Share Alike Licence (CC BY-NC-SA). Details of this licence are available here

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