The 25.4m diameter Giant Magellan Telescope utilizes a segmented adaptive secondary mirror subsystem (ASMS) for correction of atmospheric wavefront error (r0=7cm), wind-induced telescope vibrations up to 17m/s wind speed, and M1 and M2 segment alignment errors. The ASMS is composed of seven ASM segments. Each is a 1.05m diameter concave circular segment with a 2mm thick face sheet that is driven by 675 voice coil motor motors to provide wave front and phasing control. The face sheet surface figure can be updated at up to 2kHz with a -3dB bandwidth greater than 800Hz. The ASMS is integrated to the top end of the telescope by actively controlled 6 DOF hexapods. Each hexapod provides 7Hz position control to maintain the alignment within the capture range of the wave front control system. The first off-axis ASM segment is currently being manufactured by the AdOptica Consortium and their subcontractors. The Zerodur Reference Body, Zerodur face sheet, and major structural components have been manufactured and integrated. Structural and dynamic testing of the ASM primary load path has been completed. A phasing testbed is in the build stage that utilizes the single ASM segment, edge sensors, and a reference frame to simulate the phasing of an array of 4 ASM segments. This document presents an overview of the ASMS design and the results of the manufacturing, assembly and testing of the first ASM segment.
The GMT Adaptive Secondary Mirror (ASM) has recently completed the final design phase and the construction of the first segment has begun [1]. For the purpose of risk reduction, we developed a prototype with 72 actuators and a diameter of 354 mm, featuring the four innermost rings of actuators of the on-axis ASM segment. The prototype, named P72, has been conceived with the main goals of validating several new technical solutions adopted for the GMT ASM and not yet deployed in the current generation of large, contactless, VCM driven adaptive mirrors, in particular on LBT 672 and on the VLT DSM. These include larger actuators spacing, new external membranes to provide the in-plane constraint for the thin shell, improved connection to the capacitive sensors that measure the gap between reference body, RB, and thin shell and a completely new generation of control electronics. P72 has undergone a comprehensive test campaign including the electromechanical tests intended to identify and optimize the dynamic response of the adaptive mirror, and the optical tests characterizing the actual optical correction performance and the behavior of the new mirror flexures. The tests have been performed using a dedicated optical test setup with variable elevation in a climatic test facility at Microgate, which also allowed verification of the sensitivity to temperature changes. We report the prototype design and results of the test campaign, that included matching the experimental results and numerical results obtained by means of internally developed multiphysics numerical simulators.
One of the most challenging aspects of the Giant Magellan Telescope (GMT) is the need to co-phase the seven segments for the Laser Tomographic Adaptive Optics (LTAO) mode of operation. Low and high frequency co-phasing systems are used that overlap at 1/30 Hz. The high frequency co-phasing of the seven Adaptive Secondary Mirrors (ASMs) is obtained using 48 interferometric distance measuring systems mounted on the Reference Bodies outer edges. The goal is to keep optically co-phased for 120 seconds, this period being related to the bandwidth of the optical phasing sensor that will be available at the telescope. A complex control system computes the co-phasing correction based on commands from the Observatory Control Systems and measurements from the interferometric sensors. The correction command is distributed to the deformable mirror actuators. The disturbances to be compensated are quasi static ones, including gravity and thermal, together with dynamic contributions, in particular wind and telescope vibrations. A comprehensive numerical simulation has been developed and used to predict the overall system behavior, including the telescope optical loop. We report the control architecture and the results of the numerical simulation, which includes the calibration procedure with its error propagation. Moreover, we present the test results of the sensor’s stability and noise levels obtained with a dedicated breadboard mounting three pairs of sensors.
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