NGST wavefront sensing and control
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Engineering topics
Publications and source records attributed to Lowman, A..
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A piston sensing and control algorithm for the segmented mirror coarse phasing using a dispersed fringe sensor (DFS) has been developed for Next Generation Space Telescope (NGST) wavefront sensing and control. The DFS can detect residual piston errors as large as order of a depth-of-focus and can phase the segment mirrors with an accuracy less than 0.1 micron, which is within the capture range of the fine phasing for NGST. A series of experiments has been carried out on the NGST's Wavefront Control Testbed (WCT) to validate the modeling results, evaluate the DFS performance, and systematically explore the factors that affect the DFS performance. This paper reports the testbed results for several critical issues of DFS performance, including DFS dynamic range, accuracy, fringe visibility, and the effects of segment mirror aberrations.
This paper describes the engineering version of the STCS, the algorithms it incorporates, and methods of communicating with the testbed hardware.
A method of coarse phasing segmented mirrors using white light interferometry (WLI) has been developed for Next Generation Space Telescope (NGST) wavefront sensing and control. Using the broadband point spread function (PSF) of the segmented mirrors taken during a segment piston scan, the WLI can accurately detect small residual piston errors. WLI does not rely on any extra optics and uses only the final imaging camera. With its high sensitivity to small segment piston error WLI can be used as a complementary phasing algorithm to the dispersed fringe sensor (DFS) for NGST. The paper will present the results from modeling and experiment on the NGST's Wavefront Control Testbed (WCT).
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By segmenting and folding the primary mirror, quite large telescopes can be packed into the nose cone of a rocket.
Control algorithms developed for coarse phasing the segmented mirrors of the Next Generation Space Telescope (NGST)are being tested in realistic modeling and on the NGST wavefront control testbed, also known as DCATT.
A telescope simulator was built as part of the Nexus wavefront control testbed, an NGST technology experiment at NASA's Goddard Space Flight Center.
An Integrated Product Team (IPT) was formed to develop a detailed concept for optical test methodology for testing of the NGST individual primary, secondary and tertiary mirrors and the full telescope system on the ground. Optical testing is a significant cost driver therefore the testing has to understood in detailed fashion early. A brief summary of the preliminary metrology test plan at the mirror component and telescope system level is presented.
The NGST wavefront control testbed (also known as DCATT) is being used to map out the accuracy and dynamic range of the baseline NGST wavefront control system.
The alignment and phasing control of NGST's segment primary mirrors use images from the science camera instead of dedicated instruments.
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Designing an imaging spectrometer using and AOTF can be a difficult task since there is no software that can simulate the bulk diffraction that takes place in the AOTF material.
An 85 cm aperture beryllium mirror was fabricated as part of the Infrared Telescope Technology Testbed (ITTT), a facility to which the SIRTF flight telescope will be traceable.