Planck pre-launch status: The optical architecture of the HFI

P.A.R. Ade; G. Savini; R. Sudiwala; C. Tucker; A. Catalano; S. Church; R. Colgan; F.-X. Desert; E. Gleeson; W. C. Jones; J.-M. Lamarre; A. Lange; Y. Longval; B. Maffei; J.A. Murphy; F. Noviello; F. Pajot; J.-L. Puget; I. Ristorcelli; A. Woodcraft; V. Yurchenko

HAL : in2p3-00714420, version 1

Code Bibliographique ADS : 2010A&A...520A..11A

DOI : 10.1051/0004-6361/200913039

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Astronomy and Astrophysics 520 (2010) A11

Planck pre-launch status: The optical architecture of the HFI

P.A.R. Ade, G. Savini, R. Sudiwala, C. Tucker, A. Catalano ^1, 2, S. Church, R. Colgan, F.-X. Desert ³, E. Gleeson, W. C. Jones, J.-M. Lamarre ¹, A. Lange, Y. Longval ⁴, B. Maffei, J.A. Murphy, F. Noviello ⁴, F. Pajot ⁴, J.-L. Puget ⁴, I. Ristorcelli ⁵, A. Woodcraft, V. Yurchenko

(09/2010)

The Planck High Frequency Instrument, HFI, has been designed to allow a clear unobscured view of the CMB sky through an off-axis Gregorian telescope. The prime science target is to measure the polarized anisotropy of the CMB with a sensitivity of 1 part in 106 with a maximum spatial resolution of 5 arcmin (Cl ~ 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.

1 :	Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA)

	CNRS : UMR8112 – INSU – Observatoire de Paris – Université Pierre et Marie Curie [UPMC] - Paris VI – Université de Cergy Pontoise – Ecole normale supérieure de Paris - ENS Paris

2 :	AstroParticule et Cosmologie (APC)

	CNRS : UMR7164 – IN2P3 – Observatoire de Paris – Université Paris VII - Paris Diderot – CEA : DSM/IRFU

3 :	Laboratoire d'Astrophysique de Grenoble (LAOG)

	CNRS : UMR5571 – OSUG – INSU – Université Joseph Fourier - Grenoble I

4 :	Institut d'astrophysique spatiale (IAS)

	CNRS : UMR8617 – INSU – Université Paris XI - Paris Sud

5 :	Centre d'étude spatiale des rayonnements (CESR)

	CNRS : UMR5187 – Observatoire Midi-Pyrénées – INSU – Université Paul Sabatier [UPS] - Toulouse III

équipe(s) de recherche : APC - Cosmologie et gravitation

Thème(s)

Physique/Astrophysique/Cosmologie et astrophysique extra-galactique

Planète et Univers/Astrophysique/Cosmologie et astrophysique extra-galactique

Mot(s)-clé(s) : cosmic microwave background – space vehicles: instruments – instrumentation: detectors – instrumentation: polarimeters – submillimeter: general – techniques: photometric


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Contributeur : Yannick Giraud-Héraud <>
Déposé pour le compte de : Yannick Giraud-Héraud <>
Soumis le : Mercredi 4 Juillet 2012, 14:47:09
Dernière modification le : Mercredi 4 Juillet 2012, 15:10:22