We are under integrating off-axis freeform mirrors for the KASI Deep Rolling Imaging Fast Telescope Generation 1 (KDRIFT G1) using a coordinate measuring machine and assembly jig. The telescope is a confocal off-axis freeform threemirror system designed for the detection of extremely low surface brightness structures in the sky. The optical specifications of the K-DRIFT G1 are as follows: the entrance pupil diameter is 300 mm, the focal ratio is 3.5, and the field of view is 4.43° × 4.43°. During the integration stage, we used a coordinate measuring machine to measure the positions of the mirrors, flexures, and bezels within a tolerance range. Following the system integration, we will measure wavefront errors at several edge fields using an interferometer at 633 nm. In this paper, we briefly present the current status of the K-DRIFT G1 and the future plans for the project.
In this paper, we investigate several bonding methods for attaching lateral flexures to the side of a mirror in order to mitigate the potential long-term instability caused by thermal stress. To analyze the behavior of the mirror, bonding, and flexures under different mechanical and thermal loads, we utilize finite element models and examine three key aspects of the flexure bonding: the bonding area, the use of an additional block for bonding, and the choice of flexure material. Our study utilizes the primary mirror of the GEMINI telescope as a sample application and for validation purposes. Through our simulations and analysis, we aim to address various options for the flexure-bonding design and optimization.
We are developing the KASI-Deep Rolling Imaging Fast Telescope Generation 1 (K-DRIFT G1) based on the on-site performance assessment of the K-DRIFT pathfinder. The telescope is a confocal off-axis freeform three-mirror system designed for the detection of extremely low surface brightness structures in the sky. The optical specifications of the K-DRIFT G1 are as follows: the entrance pupil diameter is 300 mm, the focal ratio is 3.5, the field of view is 4.43° × 4.43°, and the image area is 81.2 mm × 81.2 mm with 10 μm pixels. We performed sensitivity analysis and tolerance simulations to integrate and align the system. We present the analysis results and development plan of the K-DRIFT G1.
This conference presentation was prepared for the Ground-based and Airborne Telescopes IX conference at SPIE Astronomical Telescopes + Instrumentation, 2022.
Design and development of large SiC mirror has been conducted. By using the finite element analysis program NX NASTRAN we calculated the opto-mechanical performance of mirror and its support system under various design loads including gravity, temperature and dynamic loads. The optical performance has been analyzed by using Zernike polynomials based on corrected RMS surface error. We also optimized a bi-pod type flexure bonded at the backside of the mirror with proper strength under environment of space-borne application. The prototype SiC mirror has been generated with proper opto-mechanical strength and good optical performance. Detailed development process of manufacturing of the mirror with grinding, polishing, bonding and environment test will be discussed herein.
The Fast-steering Secondary Mirror (FSM) of Giant Magellan Telescope (GMT) consists of seven 1.1 m diameter circular segments with an effective diameter of 3.2 m, which are conjugated 1:1 to the seven 8.4 m segments of the primary. Each FSM segment contains a tip-tilt capability for fast guiding to attenuate telescope wind shake and mount control jitter by adapting axial support actuators. Breakaway System (BAS) is installed for protecting FSM from seismic overload or other unknown shocks in the axial support. When an earthquake or other unknown shocks come in, the springs in the BAS should limit the force along the axial support axis not to damage the mirror. We tested a single BAS in the lab by changing the input force to the BAS in a resolution of 10 N and measuring the displacement of the system. In this paper, we present experimental results from changing the input force gradually. We will discuss the detailed characteristics of the BAS in this report.
KEYWORDS: Mirrors, Telescopes, Actuators, Space telescopes, Off axis mirrors, Integrated modeling, Interfaces, Optical instrument design, Phase transfer function, Control systems
The Fast-Steering Secondary Mirror (FSM) of Giant Magellan Telescope (GMT) consists of seven 1.1m diameter segments with effective diameter of 3.2m. Each segment is held by three axial supports and a central lateral support with a vacuum system for pressure compensation. Both on-axis and off-axis mirror segments are optimized under various design considerations. Each FSM segment contains a tip-tilt capability for guiding to attenuate telescope wind shake and mount control jitter. The design of the FSM mirror and support system configuration was optimized using finite element analyses and optical performance analyses. The design of the mirror cell assembly will be performed including sub-assembly parts consisting of axial supports, lateral support, breakaway mechanism, seismic restraints, and pressure seal. . In this paper, the mechanical results and optical performance results are addressed for the optimized FSM mirror and mirror cell assembly, the design considerations are addressed, and performance prediction results are discussed in detail with respect to the specifications
The Giant Magellan Telescope (GMT) will feature two Gregorian secondary mirrors, an adaptive secondary mirror (ASM) and a fast-steering secondary mirror (FSM). The FSM has an effective diameter of 3.2 m and consists of seven 1.1 m diameter circular segments, which are conjugated 1:1 to the seven 8.4m segments of the primary. Each FSM segment contains a tip-tilt capability for fast guiding to attenuate telescope wind shake and mount control jitter. This tiptilt capability thus enhances performance of the telescope in the seeing limited observation mode. The tip-tilt motion of the mirror is produced by three piezo actuators. In this paper we present a simulation model of the tip-tilt system which focuses on the piezo-actuators. The model includes hysteresis effects in the piezo elements and the position feedback control loop.
The Giant Magellan Telescope (GMT) will be equipped with two Gregorian secondary mirrors; a fast-steering secondary mirror (FSM) for seeing-limited operations and an adaptive secondary mirror (ASM) for adaptive optics observing modes. The FSM has an effective diameter of 3.2 m and is comprised of seven 1.1 m diameter circular segments, which are conjugated 1:1 to the seven 8.4m segments of the primary mirror. Each FSM segment has a tip-tilt capability for fast guiding to attenuate telescope wind shake and jitter. The FSM is mounted on a two-stage positioning system; a macro-cell that positions the entire FSM segments as an assembly and seven hexapod actuators that position and drive the individual FSM segments. In this paper, we present a technical overview of the FSM development status. More details in each area of development will be presented in other papers by the FSM team.
The Giant Magellan Telescope (GMT) will be equipped with two Gregorian secondary mirrors: a fast-steering mirror (FSM) system for seeing-limited operations and an adaptive secondary mirror (ASM) for adaptive optics observing modes. The FSM has an effective diameter of 3.2 m and is comprised of seven 1.1 m diameter circular segments, which are conjugated 1:1 to the seven 8.4m segments of the primary. Each FSM segment has a tip-tilt capability for fast guiding to attenuate telescope wind shake and jitter. To verify the tip-tilt performance at various orientations, we performed tiptilt tests using a conceptual prototype of the FSM (FSMP) which was developed at KASI for R&D of key technologies for FSM. In this paper, we present configuration, methodology, results, and lessons from the FSMP test which will be considered in the development of FSM.
The Fast Steering Secondary Mirror (FSM) for the Giant Magellan Telescope (GMT) will have seven 1.05 m diameter circular segments and rapid tip-tilt capability to stabilize images under wind loading. In this paper, we report on the assembly, integration, and test (AIT) plan for this complex opto-mechanical system. Each fast-steering mirror segment has optical, mechanical, and electrical components that support tip-tilt capability for fine coalignment and fast guiding to attenuate wind shake and jitter. The components include polished and lightweighted mirror, lateral support, axial support assembly, seismic restraints, and mirror cell. All components will be assembled, integrated and tested to the required mechanical and optical tolerances following a concrete plan. Prior to assembly, fiducial references on all components and subassemblies will be located by three-dimensional coordinate measurement machines to assist with assembly and initial alignment. All electronics components are also installed at designed locations. We will integrate subassemblies within the required tolerances using precision tooling and jigs. Performance tests of both static and dynamic properties will be conducted in different orientations, including facing down, horizontal pointing, and intermediate angles using custom tools. In addition, the FSM must be capable of being easily and safely removed from the top-end assemble and recoated during maintenance. In this paper, we describe preliminary AIT plan including our test approach, equipment list, and test configuration for the FSM segments.
KEYWORDS: Mirrors, Telescopes, Optical fabrication, Telescopes, Control systems, Prototyping, Control systems design, Space telescopes, Surface finishing, Manufacturing, Profilometers
The Giant Magellan Telescope (GMT) will be featured with two Gregorian secondary mirrors, an adaptive secondary mirror (ASM) and a fast-steering secondary mirror (FSM). The FSM has an effective diameter of 3.2 m and built as seven 1.1 m diameter circular segments, which are conjugated 1:1 to the seven 8.4m segments of the primary. Each FSM segment contains a tip-tilt capability for fine co-alignment of the telescope sub-apertures and fast guiding to attenuate telescope wind shake and mount control jitter. This tip-tilt capability thus enhances performance of the telescope in the seeing limited observation mode. As the first stage of the FSM development, Phase 0 study was conducted to develop a program plan detailing the design and manufacturing process for the seven FSM segments. The FSM development plan has been matured through an internal review by the GMTO-KASI team in May 2016 and fully assessed by an external review in June 2016. In this paper, we present the technical aspects of the FSM development plan.
The Giant Magellan Telescope (GMT) will be a 25m class telescope currently in the design and development phase. The
GMT will be a Gregorian telescope and equipped with a fast-steering secondary mirror (FSM). This secondary mirror is
3.2 m in diameter and built as seven 1.1 m diameter circular segments conjugated 1:1 to the seven 8.4m segments of the
primary. The prototype of FSM (FSMP) development effort is led by the Korea Astronomy and Space Science Institute
(KASI) with several collaborators in Korea, and the National Optical Astronomy Observatory (NOAO) in USA. The
FSM has a tip-tilt feature to compensate image motions from the telescope structure jitters and the wind buffeting. For
its dynamic performance, each of the FSM segments is designed in a lightweight mirror. Support system of the
lightweight mirror consists of three axial actuators, one lateral support at the center, and a vacuum system. A parametric
design study to optimize the FSM mirror configuration was performed. In this trade study, the optical image qualities
and structure functions for the axial and lateral gravity print-through cases, thermal gradient effects, and dynamic
performances will be discussed.
The Giant Magellan Telescope (GMT) will be a 25m class telescope which is one of the extremely large telescope
projects in the design and development phase. The GMT will have two Gregorian secondary mirrors, an adaptive
secondary mirror (ASM) and a fast-steering secondary mirror (FSM). Both secondary mirrors are 3.2 m in diameter and
built as seven 1.1 m diameter circular segments conjugated 1:1 to the seven 8.4m segments of the primary. The FSM has
a tip-tilt feature to compensate image motions from the telescope structure jitters and the wind buffeting. The support
system of the lightweight mirror consists of three axial actuators, one lateral support at the center, and a vacuum system.
A parametric study and optimization of the FSM mirror blank and central lateral flexure design were performed. This
paper reports the results of the trade study. The optical image qualities and structure functions for the axial and lateral
gravity print-through cases, thermal gradient effects, and dynamic performances will be discussed for the case of a lightweighted
segment with a center thickness of 140 mm weighing approximately 105 kg.
The Advanced Technology Solar Telescope (ATST) primary mirror is a 4.24-m diameter, 75-mm thick, off-axis
parabola solid meniscus mirror made out of a glass or glass ceramic material. Its baseline support system consists of 120
axial supports mounted at the mirror back surface and 24 lateral supports along the outer edge with an active optics
capability. This primary mirror support system was optimized for the telescope at a near horizon position to achieve the
best gravity and thermal effects. To fulfill the optical and mechanical performance requirements, extensive finite
element analyses using I-DEAS and optical analyses with PCFRINGE have been conducted for the support optimization.
Analyses include static deformation (gravity and thermal), frequency calculations, and support system sensitivity
evaluations. An influence matrix was established to compensate potential errors using an active optics system.
Performances of the primary mirror support system were evaluated from mechanical deformation calculations and the
optical analyses before and after active optics corrections. The performance of the mirror cell structure was also
discussed.
The design and development of a beam launch telescope (BLT) was addressed herein. The BLT optical instruments have been commonly used for the applications of adaptive optics (laser guide star), optical communications, and other laser powered optical systems. In this study, a BLT with a primary mirror of 700 mm was investigated as a prototype optical system. The BLT optical system includes a lightweight primary mirror of 700 mm in daimeter, a secondary mirror of 110 mm, a fast steering mirror of 200 mm, and three flat mirrors (array/relay mirrors) of 200 mm. As a test bed, the BLT system was optimized for a spot size of 100mm at a far field (departed by 1km from the telescope). In this design and development study, a wide range of the opto-mechanical and structural analyses have been performed including: static (gravity and thermal), frequency, dynamic and response analysis, and optical evaluations for minimum optical deformation. The EDS I-DEAS Finite Element program and the PCFRINGE optical program are mainly used to fulfill this analysis. Image motion is also calculated based on line of sight (LOS) sensitivity equations integrated in finite element models.
This paper describes a design study of the KAO (Korea Astronomy Observatory) 1m telescope. The telescope uses an F/2.7 zerodur primary mirror which has a double arch back contour shape. For the zenith pointing, the primary mirror is to be held by a 6-point axial support system at the back surface. For Horizon, a 3-lateral support system is to be designed and located at the center of gravity of the mirror. In this paper, a parametric design study of a double arch back contour shape is to be performed to meet an optical surface deflection requirement, a surface RMS wavefront error of (lambda) divided by 10, using the finite element program, ANSYS, for the mechanical surface deformation, and the PCFRINGE program for the evaluation of the optical performance. Additionally, the static and modal frequency analysis of the truss structure and yoke were performed.
We developed formulae and numerical techniques for the corrutations of the point spread
function (PSF) and optical transfer function (GrF) in the general case of unrestricted
aberration and with the following di fferent forms of non-uniform real ariplitude : ( i ) when
the real airplitude is described by a polynomial, (ii) a Gaussian distribution of real amplitude
which corresponds to the intensity distribution of laser beam, and ( iii ) a pupil
with a central obstruction. The developed coriputer programs
were tested and used to study the influence of non-uniform
anplitude on the PSF and CITF .
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