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AN OVERVIEW of the ACTIVE OPTICS CONTROL STRATEGY for the THIRTY METER TELESCOPE Mark J

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AN OVERVIEW of the ACTIVE OPTICS CONTROL STRATEGY for the THIRTY METER TELESCOPE Mark J Proceedings of ICALEPCS2011, Grenoble, France MOPKS023 AN OVERVIEW OF THE ACTIVE OPTICS CONTROL STRATEGY FOR THE THIRTY METER TELESCOPE Mark J. Sirota, George Z. Angeli, Douglas G. MacMynowski, TMT Observatory Corporation, Pasadena, CA. 91105, U.S.A. Terry Mast, Jerry Nelson, University of California, Santa Cruz, CA. 95064, U.S.A. Gary Chanan, University of California, Irvine, 92697, U.S.A. M. Mark Colavita, Christian Lindensmith, Chris Shelton, Mitchell Troy, Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA. 01109, U.S.A. Peter M. Thompson, Systems Technology, Inc., Hawthorne, CA. 90250, U.S.A. Abstract TMT will be sited at Mauna Kea, Hawaii. The primary (M1), secondary (M2) and tertiary (M3) Construction of the telescope is scheduled to begin in mirrors of the Thirty Meter Telescope (TMT), taken 2014 with first light with all 492 segments in 2021. together, have over 10,000 degrees of freedom. The vast majority of these are associated with the 492 individual primary mirror segments. The individual segments are converted into the equivalent of a monolithic thirty meter primary mirror via the Alignment and Phasing System (APS) and the Primary Mirror Control System (M1CS). In this paper we first provide an introduction to the TMT. We then describe the overall optical alignment and control strategy for the TMT and follow up with additional descriptions of the M1CS and the APS. We conclude with a short description of the TMT error budget process and provide an example of error allocation and predicted performance for wind induced segment jitter. INTRODUCTION The Thirty Meter Telescope (TMT) is a collaborative Figure 1: The Thirty Meter Telescope. project between the California Institute of Technology, the University of California, the Association of Canadian Universities for Research in Astronomy, the National CONTROL SYSTEM OVERVIEW Astronomical Observatory of Japan, the Department of The TMT image quality control architecture can be Science and Technology of India, and the National decomposed into two major systems; Active and Adaptive Astronomical Observatory of China. Optics. Active Optics (aO) is accomplished by the three The TMT design is a f/15, wide-field, altitude over mirror telescope and is responsible for the image quality azimuth, Ritchey-Chretien telescope with a 30 m primary of the optical beam delivered to the seeing limited science mirror composed of 492 hexagonal segments. The instruments or the Adaptive Optics system. The Adaptive telescope when pointing at zenith is ~ 51 m high and Optics (AO) system is responsible for delivering weighs approximately 1800 metric tons. diffraction limited image quality to the infrared The tertiary mirror is articulated and in combination instruments by attenuating the blurring effects of the with the large Nasmyth platforms enables the mounting of atmosphere, reducing image jitter induced by the eight or more different AO/instrument combinations. telescope drives and wind shake, and reducing residual The telescope will support observations from 0.31 to 28 image quality errors in the beam delivered by the aO μm. The TMT will include integrated advanced adaptive system. The remainder of this paper is focused on the aO optics capabilities, including a laser guide star system, system. supporting diffraction-limited observations at The aO system maintains TMT image quality with a wavelengths beyond 1 µm over most of the sky. The total of 11,815 degrees of freedom distributed across four wide, 20 arc-minute diameter, field-of-view will enable principle local control loops; the Mount Control System the use of wide-field, multi-object spectrographs. The [1], the M1CS, the M2 Control System (M2CS), and the “early light instruments” that are delivered as part of the M3 Control System (M3CS). Each of the principle control construction effort include IRIS (Infrared Imaging loops, with the exception of the M3CS, takes advantage Spectrometer), WFOS (Wide Field Optcal Spectrometer) of real time corrections based on on-sky measurements 2011 by the respective authors — cc Creative Commons Attribution 3.0 (CC BY 3.0) and IRMS (InfraRed Multi-slit Spectrometer). c provided by an outer control loop. The on-sky ○ corrections can come from one of three sources; the APS, Process tuning and feedback systems 211 Copyright MOPKS023 Proceedings of ICALEPCS2011, Grenoble, France an Acquisition, Guider and Wave-Front Sensor (AGWFS) An accounting of the degrees of freedom along with a system located in each of the seeing limited instruments listing of the key characteristics of each principle local [2], or offloads from the AO system. The APS is used control loop is tabulated in Table 1. Table 1 also includes only when aligning the telescope optics and calibrating a description of the relationship between each of the the sensors associated with the principle local control principle local control systems and the APS and AGWFS loops whereas the other two sources of correction are outer control loops used during alignment and science used during science observations. observations respectively. Table 1: Characteristics of M1, M2, M3, and Outer Control Loops Alignment and Operational Outer Principle Local Control Loops Calibration Loop Loop Degrees of Rate (Hz) (Hz) Rate Actuators Actuators Loop BW BW Loop Rate (Hz) (Hz) Rate Freedom Freedom Refresh Refresh Sensors Sensors Update Update Update Update Sensor Sensor Sensor Rate Rate (Hz) Name Azimuth & Direct Tape AGWFS 2 ≥ 40 ~ 1 APS camera Monthly 1 Elevation Drive encoders (Guider) Mount Mount Global Segment Actuator Surveying/F 3 ≥ 10 ~ 1 > 1 year No outer control loop Tip, Tilt, Piston actuators sensors EM Segment Segment Edge 2 to 4 AGWFS 1476 ≥ 10 ~ 1 APS 0.003 M1 M1 Tip, Tilt, Piston actuators sensors weeks (WFS) Warping Warping Strain Set & 2 to 4 10,332 na APS No outer control loop Harness harness gauges Forget weeks Local 2 to 4 AGWFS De-center 2 Hexapod ≥ 10 < 1 APS 0.003 encoders weeks (WFS) Local Tip/Tilt 2 Hexapod ≥ 10 < 1 Surveying > 1 year No outer control loop M2 M2 encoder Local 2 to 4 AGWFS Piston 1 Hexapod ≥ 10 < 1 APS 0.003 encoder weeks (WFS) APS Local Tilt 1 DC drive ≥ 10 < 1 (Pupil > 1 year No outer control loop encoder Tracker) M3 M3 Local APS (Pupil Rotation 1 DC drive ≥ 10 < 1 > 1year No outer control loop encoder Tracker) For simplicity we can describe the TMT aO image the desired edge sensor readings as well as attenuate quality control strategy using five objectives. Each temporal and thermal drifts in the M1, M2, and M3 objective is accomplished using one or more of the four shapes. principle local control loops defined previously in combination with the APS or the AGWFS. The five M1 Segment Shape objectives are M1 global shape, M1 Segment Shape, The individual segments will have shape errors Alignment, Acquisition and Pointing, and Guiding. In associated with polishing, coating stresses, and the practice these objectives are coupled but for the purposes support system. In addition, there will be segment shape of this paper we assume they are independent. Although errors associated with segment positions in the telescope Acquisition and Pointing is not, strictly speaking deviating from their ideal positions. associated with image quality, it is included here for The shape of each segment can be adjusted via a 21- completeness. Each objective is briefly described below. actuator warping harnesses that is built into the support assembly for each segment. The APS measures and M1 Global Shape partially corrects, via the M1CS, the shape of each of the The APS is used on-sky to determine the 2772 M1 edge 492 segments using the 21 warping harness actuators. sensor readings that result in the formation of the These corrections are typically made after a segment equivalent of a 30 m monolithic mirror. The APS exchange and held constant until the next exchange. Ten achieves this by accurately measuring, and then segments are exchanged every two weeks for re-coating. positioning each of the 492 segments in piston, tip, and tilt. Once the APS determines that the global shape of the Alignment M1 is correct the corresponding edge sensor readings are The optical axis of the telescope is defined by the recorded for later use by the M1CS. global position of the M1. The global position (piston, In operation the M1CS will use the edge sensor tip, tilt) of the segmented M1 is allowed to systematically readings recorded by the APS to maintain the overall follow the deformations of the M1 support structure due shape of the M1 despite structural deformations caused by to gravity as the telescope rotates about the elevation axis temperature and gravity, and disturbances from wind and in a manner that minimizes the maximum stroke of the vibrations. In addition the M1CS will receive low 1472 segment actuators. To achieve this result the desired 2011 bytemporal the respective authors — cc Creative Commons Attribution 3.0 (CC BY 3.0) and spatial frequency real time corrections from global position of the M1 as a function of elevation angle c ○ the AGWFS. These corrections reduce residual errors in is determined via analysis of the telescope structure Finite Copyright 212 Process tuning and feedback systems Proceedings of ICALEPCS2011, Grenoble, France MOPKS023 Element Model (FEM). Real time measurement of the M1CS global M1 position in operation is achieved by The M1CS is responsible for maintaining the overall determining the best fit plane through M1 as determined shape of the segmented M1 mirror over all conditions. by the actuator sensors Properly supported, the mirror segments can be treated as In operation the M2 is constantly re-positioned in rigid bodies; hence, their positions can be described by translation to maintain alignment with the M1 and in six parameters. The three in-plane motions are controlled piston to keep the optical system in focus.
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