Wavefront Sensing and Controls for the James Webb Space Telescope

被引：62

作者：

Acton, D. Scott ^{[1
]}

Knight, J. Scott ^{[1
]}

Contos, A. ^{[1
]}

Grimaldi, S. ^{[1
]}

Terry, J. ^{[1
]}

Lightsey, P. ^{[1
]}

Barto, A. ^{[1
]}

League, B. ^{[1
]}

Dean, Bruce ^{[2
]}

Smith, J. Scott ^{[2
]}

Bowers, Charles ^{[2
]}

Aronstein, D. ^{[2
]}

Feinberg, L. ^{[2
]}

Hayden, W. ^{[2
]}

Comeau, T. ^{[3
]}

Soummer, R. ^{[3
]}

Elliott, E. ^{[3
]}

Perrin, M. ^{[3
]}

Starr, Carl W., Jr. ^{[4
]}

机构：

[1] Ball Aerosp & Technol Corp, 1600 Commerce St, Boulder, CO 80501 USA

[2] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA

[3] Space Telescope Sci Inst, Baltimore, MD 21218 USA

[4] Northrop Grumman Areosp Syst, Redondo Beach, CA USA

来源：

SPACE TELESCOPES AND INSTRUMENTATION 2012: OPTICAL, INFRARED, AND MILLIMETER WAVE | 2012年 / 8442卷

关键词：

JWST; Wavefront Sensing and Controls;

D O I：

10.1117/12.925015

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The James Webb Space Telescope (JWST) is a segmented deployable telescope, utilizing 6 degrees of freedom for adjustment of the Secondary Mirror (SM) and 7 degrees of freedom for adjustment of each of its 18 segments in the Primary Mirror (PM). When deployed, the PM segments and the SM will be placed in their correct optical positions to within a few mm, with accordingly large wavefront errors. The challenge, therefore, is to position each of these optical elements in order to correct the deployment errors and produce a diffraction-limited telescope, at lambda=2 mu m, across the entire science field. This paper describes a suite of processes, algorithms, and software that has been developed to achieve this precise alignment, using images taken from JWST's science instruments during commissioning. The results of flight-like end-to-end simulations showing the commissioning process are also presented.

引用

页数：11

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