Planck Telescope: optical design and verification

Philippe Martin; Jean-Bernard Riti; Daniel de Chambure

doi:10.1117/12.2500108

13 April 2018 Planck Telescope: optical design and verification

Philippe Martin, Jean-Bernard Riti, Daniel de Chambure

Author Affiliations +

Proceedings Volume 10568, International Conference on Space Optics — ICSO 2004; 105682D (2018) https://doi.org/10.1117/12.2500108
Event: International Conference on Space Optics 2004, 2004, Toulouse, France

Abstract

The cornerstone mission of the European Space Agency (ESA) scientific program Herschel/Planck is currently in the design manufacturing phase (phase C/D). The Planck satellite will be launched in 2007, together with Herschel. Located around the L2 Lagrange point, Planck aims at obtaining very accurate images of the Cosmic Wave Background fluctuations. Working up to high frequency (857GHz, i.e. 350μm wavelength), Planck is expected to give sharper images than the recently launched WMAP satellite. The Planck Telescope is an off-axis (unobscured) Gregorian antenna, with a 1.5m diameter pupil, a small F-number (~1) and a large FOV (+/-5° circular), owing to place a large number of detectors (bolometers) in the focal plane. This paper presents the optical design, performance, and verification concept of the Planck telescope. The custom made sequential Hartmann system is described. Working at 10.6μm, it will directly measure the wavefront of the telescope in cryogenic environment i.e. at operational conditions. This will be a major milestone in the spacecraft development.

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Philippe Martin, Jean-Bernard Riti, and Daniel de Chambure "Planck Telescope: optical design and verification", Proc. SPIE 10568, International Conference on Space Optics — ICSO 2004, 105682D (13 April 2018); https://doi.org/10.1117/12.2500108

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