Ade, P. A. R. and Savini, G. and Sudiwala, R. and Tucker, C. and Catalano, A. and Church, S. and Colgan, R. and Desert, F. X. and Gleeson, E. and Jones, W. C. and Lamarre, J.-M and Lange, A. and Longval, Y. and Maffei, B. and Murphy, J. A. and Noviello, F. and Pajot, F. and Puget, J.-L and Ristorcelli, I. and Woodcraft, A. and Yurchenko, V. (2010) Planck pre-launch status: The optical architecture of the HFI. Astronomy and Astrophysics, 520 . Art. No. A11. ISSN 0004-6361 http://resolver.caltech.edu/CaltechAUTHORS:20101111-141312874
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The Planck High Frequency Instrument, HFI, has been designed to allow a clear unobscured view of the CMB sky through an offaxis Gregorian telescope. The prime science target is to measure the polarized anisotropy of the CMB with a sensitivity of 1 part in 10^6 with a maximum spatial resolution of 5 arcmin (C_l ~ 3000) in four spectral bands with two further high-frequency channels measuring total power for foreground removal. These requirements place critical constraints on both the telescope configuration and the receiver coupling and require precise determination of the spectral and spatial characteristics at the pixel level, whilst maintaining control of the polarisation. To meet with the sensitivity requirements, the focal plane needs to be cooled with the optics at a few Kelvin and detectors at 100 mK. To limit inherent instrumental thermal emission and diffraction effects, there is no vacuum window, so the detector feedhorns view the telescope secondary directly. This requires that the instrument is launched warm with the cooler chain only being activated during its cruise to L2. Here we present the novel optical configuration designed to meet with all the above criteria.
|Additional Information:||© 2010 ESO. Received 31 July 2009. Accepted 21 December 2009. Published online 15 September 2010. The authors would like to acknowledge the support from the UK STFC, CNES, NASA, Enterprise Ireland and Science Foundation Ireland. The authors extend their gratitude to numerous engineers and scientists who have somehow contributed to the design, development, construction or evaluation of HFI.|
|Subject Keywords:||cosmic microwave background; space vehicles: instruments; instrumentation: detectors; instrumentation: polarimeters; submillimeter: general, techniques: photometric|
|Official Citation:||Planck pre-launch status: The optical architecture of the HFI A11 P. A. R. Ade et al. DOI: 10.1051/0004-6361/200913039|
|Usage Policy:||No commercial reproduction, distribution, display or performance rights in this work are provided.|
|Deposited By:||Ruth Sustaita|
|Deposited On:||12 Nov 2010 16:09|
|Last Modified:||26 Dec 2012 12:37|
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