2022•Space Telescopes and Instrumentation 2022: Optical, Infrared, and Millimeter WaveRequires access

Phasing the Webb telescope

D. Scott Acton, Scott S. Knight, María Cristina Carrasquilla, Nick Weiser, Michaela Masciarelli, Sarah Jurczyk, Greg Rapp, Julio Mueckay, Erin Wolf, Jess Murphy, Larkin Carey, Eric Coppock, Chanda Walker, Joel Runnels, Garrett West, Greg Wirth, Brian M. Hicks, Katie Melbourne, Michael Gordon, Bob Brown, Stefano Grimaldi, Derek Sabatke, Ray Wright, Laura Coyle, Taylor S. Chonis, Kevin Whiteaker, Marshall D. Perrin, Tom Comeau, Charles-Philippe Lajoie, G. Hartig, Tracy L. Beck, Matthew Lallo, M A Regan, Randal Telfer, M. Meléndez, Gregory R. Brady, Laurent Pueyo, Nicolas Flagey, Bernard Kulp, Edward Nelan, Keira Brooks, P. Chayer, Shannon Osborne, S. T. Holfeltz, Tony Sohn, Thomas P. Zielinski, Alden S. Jurling, Matthew D. Bergkoetter, Charles W. Bowers, Bruce H. Dean, Lee D. feinberg, Ritva Keski-kuha, Jeffrey R. Kirk, Joseph M. Howard

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Abstract

The James Webb Space Telescope (JWST) is a segmented deployable telescope, currently operating at L2. The telescope utilizes 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). After deployment, the PM segments and the SM arrived in their correct optical positions to within a ~1 mm, with accordingly large wavefront errors. A Wavefront Sensing and Controls (WFSC) process was executed to adjust each of these optical elements in order to correct the deployment errors and produce diffraction-limited images across the entire science field. This paper summarizes the application of the WFSC process.

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Key concepts: James Webb Space Telescope, Telescope, Wavefront, Primary mirror, Active optics, Secondary mirror, Software deployment, Degrees of freedom (physics and chemistry)