KEYWORDS: Sensors, Mirrors, Space telescopes, Telescopes, Control systems, Calibration, Sensor calibration, Temperature metrology, Image quality, Process control
The Segment Alignment Maintenance System (SAMS) is a control system to maintain the alignment of the 91 segment Hobby-Eberly Telescope (HET) primary mirror array. The system was developed by Blue-Line Engineering (Colorado Springs, CO) and NASA-Marshall Space Flight Center (Huntsville-Al). The core of the system is a set of 480 inductive edge sensors which measure relative shear between adjacent segments. The relative shear is used to calculate segment tip/tilt and piston corrections. Although the system has dramatically improved the performance of the HET it does not meet its error budget due to thermal drifts in the sensors. The system is now sufficiently stable that it routinely requires only one primary mirror alignment at the beginning of the night. We describe methods to calibrate this sensor drift.
KEYWORDS: Mirrors, Sensors, Telescopes, Space telescopes, Control systems, Image segmentation, Simulation of CCA and DLA aggregates, Image quality, Calibration, Observatories
A sensing and control system for maintaining the optical alignment of the ninety-one 1-meter diameter hexagonal segments forming the Hobby-Eberly Telescope (HET) primary mirror array has been developed by NASA - Marshall Space Flight Center (Huntsville, AL) and Blue Line Engineering (Colorado Springs, CO) and implemented. This Segment Alignment Maintenance System (SAMS) employs 480 edge sensors to measure the relative shear motion between each segment edge pair and compute individual segment tip, tilt and piston position errors. Error information is sent to the HET primary mirror control system, which then corrects the physical position of each segment every 90 seconds. On-site installation of the SAMS sensors, ancillary electronics and software was completed in September 2001. Since that time, SAMS has undergone engineering testing. The system has operated almost nightly, improving HET's overall operational capability and image quality performance. SAMS has not yet, however, demonstrated performance at the specified levels for tip, tilt, piston and Global Radius of Curvature (GRoC) maintenance. Additional systems development and in situ calibration are expected to bring SAMS to completion and improved operation performance by the end of this year.
The Segment Alignment Maintenance System (SAMS) was installed on McDonald Observatory's Hobby-Eberly Telescope (HET) in August 2001. The SAMS became fully operational in October 2001. The SAMS uses a system of 480 inductive edge sensors to correct misalignments of the HET's 91 primary mirror segments when the segments are perturbed from their aligned reference positions. A special observer estimates and corrects for the global radius of curvature (GRoC) mode, a mode unobservable by the edge sensors. The SAMS edge sensor system and GRoC estimator are able to maintain HET's primary figure for longer durations than previously had been observed. This paper gives a functional description of the SAMS control system and presents performance verification data.
KEYWORDS: Sensors, Mirrors, Telescopes, Space telescopes, Control systems, Image segmentation, Process control, Signal processing, Simulation of CCA and DLA aggregates, Image quality
NASA's Marshall Space Flight Center, in collaboration with Blue Line Engineering of Colorado Springs, Colorado, is developing a Segment Alignment Maintenance System (SAMS) for McDonald Observatory's Hobby-Eberly Telescope (HET). The SAMS shall sense motions of the 91 primary mirror segments and send corrections to HET's primary mirror controller as the mirror segments misalign due to thermo-elastic deformations of the mirror support structure. The SAMS consists of inductive edge sensors. All measurements are sent to the SAMS computer where mirror motion corrections are calculated. In October 2000, a prototype SAMS was installed on a seven-segment cluster of the HET. Subsequent testing has shown that the SAMS concept and architecture are a viable practical approach to maintaining HET's primary mirror figure, or the figure of any large segmented telescope. This paper gives a functional description of the SAMS sub-array components and presents test data to characterize the performance of the sub-array SAMS.
KEYWORDS: Mirrors, Sensors, Telescopes, Image segmentation, Control systems, Space telescopes, Telecommunications, Actuators, Digital signal processing, Process control
A sensing and control system for maintaining optical alignment of ninety-one 1-meter mirror segments forming the Hobby-Eberly Telescope (HET) primary mirror array is now under development. The Segment Alignment Maintenance System (SAMS) is designed to sense relative shear motion between each segment edge pair and calculated individual segment tip, tilt, and piston position errors. Error information is sent to the HET primary mirror control system, which corrects the physical position of each segment as often as once per minute. Development of SAMS is required to meet optical images quality specifications for the telescope. Segment misalignment over time is though to be due to thermal inhomogeneity within the steel mirror support truss. Challenging problems of sensor resolution, dynamic range, mechanical mounting, calibration, stability, robust algorithm development, and system integration must be overcome to achieve a successful operational solution.
The Phased Array Mirror, Extendible Large Aperture (PAMELA) prototype telescope phase I testing and verification has been completed. The prototype telescope is the first to have a fully adaptive primary mirror which consists of 36 hexagonal injection-molded Pyrex segments that are seven centimeters flat-to-flat. The segments are mounted on three long-throw voice-coil actuators for tip, tilt, and piston motion. The segments' tilts are measured with a Hartmann- Shack wavefront sensor, and the piston errors between adjacent segments are measured via inductive edge-sensors. The 0.5 meter telescope was successfully operated with simultaneously closed tilt and piston control loops for the entire array. Phase I test and verification results are shown for the closed loop operations.
The Phased Array Mirror, Extendible Large Aperture telescope has been fully assembled and testing has started. The telescope is the first to have a fully adaptive primary mirror, which consists of 36 hexagonal injection-molded Pyrex segments that are seven centimeters flat-to- flat. The segments are mounted on three long-throw voice-coil actuators for tip, tilt, and piston motion. The segment tiles are measured with a Hartmann-Shack wavefront sensor and the piston errors between adjacent segments are measured via inductive edge-sensors. The personnel at NASA MSFC are performing a significant amount of testing in the area of controls/structure interactions; therefore, in addition to a description of the optical performance and aberration correction capability of the telescope, a description of the plan to model the mechanical structure with emphasis on how this will interact with the adaptive optics system is presented.
KEYWORDS: Mirrors, Actuators, Silicon, Telescopes, Process control, Signal processing, Digital signal processing, Space telescopes, Silicon carbide, Crystals
Some applications for high energy beam directors will require near diffraction limited performance at near visible wavelengths even in the presence of severe environmental conditions and operational requirements. Telescopes based on the PAMELA architecture appear to be the only viable candidate for such applications which necessitate wave front correction on a spatial scale of a few centimeters over an aperture of 10 to 12 meters. Past work under the sponsorship of DARPA and the SDIO has demonstrated the feasibility of constructing such telescopes based on light weight silicon carbide segments which are 7 cm flat to flat. More recent work has been directed at assessing the feasibility of producing 3 cm segments using single crystal silicon micromachining technology. This paper describes the latest activities and results of this work.
KEYWORDS: Control systems, Spatial frequencies, Actuators, Optical components, Wavefront sensors, Adaptive optics, Sensors, Space telescopes, Wavefronts, Local area networks
The PAMELA segmented optical surface concept uses the cellular automata paradigm to build up an active surface of individually controlled elements that maintain edge-match by relying on electronically sensed nearest neighbor edge-to-edge errors. The segments are controlled in tilt directly from a wavefront sensor (e.g., of the Hartmann-Schack type) in a separate parallel loop. The approach obviates the matrix operations needed in a typical multiple-input, multiple- out (MIMO) servo control system. In this manner, the segmented optical system is extensible to arbitrary aperture diameter by gradually building up the active surface using identical elements. This paper addresses methods to improve the real-time adaptive control of such a surface using hierarchical control architectures.
A hardware demonstration of segmented mirror systems for adaptive optics is described. The basis of the phased array mirror extendible large aperture (PAMELATM) concept is that large adaptive mirrors can be fabricated from many small segments by utilizing edge-sensors, which measure the piston error between segments. We have investigated the interaction between the piston and tilt control loops which direct the motion of individual segments. The segment tilt, which is set by a wavefront-sensor-based control loop, directly affects the piston error between segments; therefore, the segment piston control loop must be able to perform corrections much faster than the rate at which the tilt corrections are being performed. In this experiment, we have one fully actuated segment with a wavefront sensor measuring the error in the wavefront gradient. An adjacent segment is driven in piston to produce the piston error signal. We measure and present the bandwidth trade-offs between the two control loops and predict how this will affect the performance of larger systems. This interactive control loop methodology has an advantage over normal adaptive optics systems in that the computationally intensive wavefront reconstruction process can be removed due to the direct measurement of both the tilt and the piston errors.
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