Warping Harness is a mechanism which can periodically correct the low order surface errors of mirror. The main correction objects are the residual error of the mirror machining, the stress distortion caused by the coating, the surface error caused by the temperature load, even with the errors caused by the gravity change, and so on. In principle, the zero moment point of the Whiffletree structure can be adjusted by changing the deflection of the warping harness blade. Due to the closed force system, once the moment induced by the warping harness changes, the load distribution on the whiffletree structure varies too. In practice, the structure of Warping Harness is installed on each group of Whiffletree joints and works with the structure of Whiffletree. The servo stepping motor is employed to control the bending of the spring blade to change the distribution of the support force, and then the correction of the main mirror surface figure is completed. This paper mainly introduces the correction principle of Warping harness and its principle, and demonstrates the preliminary design of the system.
Large telescopes are developing, and promoted by new technological developments. In order to study the method of mirror seeing detection for large aperture optical system, the relationship between mirror seeing and slope information is derived first. In order to evaluate the results more comprehensively, the normalized point source sensitivity was introduced to evaluate the results. Finally, according to the previous analysis, the experiment was carried out. The change normalized point source sensitivity under different conditions is calculated. By comparing with RMS of wavefront, the better statistical characteristic of sensitivity of normalized point source was verified.
The Changchun Institute of Optics, Fine Mechanics and Physics (CIOMP) team is developing Giant Steerable Science Mirror (GSSM) for Thirty Meter Telescope (TMT). This paper will combine PSSn to analyze the error characteristics of GSSM. To evaluate the performance of the large telescope under different kinds of error source, the normalized point source sensitivity is introduced, which is firstly studied by the group of thirty meter telescope team to balance all the deviation of the telescope and also budget the error. First and foremost, the character of the normalized point source sensitivity is studied in the very first part and the advantage in the evaluation in all the frequency domain. Then the PSSn is compared with the traditional metric, such as RMS and the multiplication property is discussed. The experienced formula is used to show the relationship between the PSSn and the error sources, static and dynamic. Lastly, the method is applied to a large aperture telescope.
The Thirty Meter Telescope (TMT) project will design and build a thirty-meter diameter telescope for research in astronomy in visible and infrared wavelengths. The primary mirror of TMT is made up of 492 hexagonal mirror segments under active control. The highly segmented primary mirror will utilize edge sensors to align and stabilize the relative piston, tip, and tilt degrees of segments. The Support System Assembly (SSA) of segmented mirror utilizes a Guide Flexure to decouple the axial support and lateral support while its deformation will bring in measurement error of edge sensor. We have analyzed the theoretical relationship between the segment movement and the measurement value of edge sensor and proposed an error correction method with matrix. The correction process and the simulation results of the edge sensor will be described in this paper.
The Changchun Institute of Optics, Fine Mechanics and Physics (CIOMP) team is developing Giant Steerable Science Mirror (GSSM) for Thirty Meter Telescope (TMT) which has got into the preliminary design phase in 2017. To develop the passive support structure system for the largest elliptic-plane flat mirror and a smoothest tracking mechanism for the gravity-variant condition, CIOMP had developed a 1/4 scale, functionally accurate version of the GSSM prototype as the pre-construction of GSSM. The prototype incorporates the same optical-mechanical system and servo control system as GSSM. The size of the prototype mirror is 898.5mm×634mm×12.5 mm with elliptic-plane figure and is supported by 18 points whiffletree on axial and 12 points whiffletree on lateral. The main objective of the preconstruction includes validate the conceptual design of GSSM and increase more confidence when meet the challenge during the development of GSSM. The assembling, integration and verification of the prototype have been completed based on the test results. CIOMP has got the sufficient test results during the pre-construction phase and got into the preliminary design for GSSM.
The Changchun Institute of Optics, Fine Mechanics and Physics (CIOMP) team is developing the Giant Steerable Science Mirror (GSSM) for Thirty Meter Telescope (TMT) which will enter the preliminary design phase in 2016. The GSSM is the tertiary mirror of TMT and consists of the world’s largest flat telescope mirror (approximately 3.4m X 2.4 m X 100mm thick) having an elliptical perimeter positioned with an extremely smooth tracking and pointing mechanism in a gravity-varying environment. In order to prepare for developing this unique mirror system, CIOMP has been developing a 1/4 scale, functionally accurate version of the GSSM prototype during the pre-construction phase of GSSM. The prototype will incorporate the same optomechanical system and servo control system as the GSSM. The size of the prototype mirror is 898.5mm×634mm×12.5mm with an elliptical perimeter. The mirror will be supported axially by an 18 point whiffletree and laterally with a 12 point whiffletree. The main objective of the preconstruction phase includes requirement validation and risk reduction for GSSM and to increase confidence that the challenge of developing the GSSM can be met. The precision mechanism system and the optical mirror polishing and testing have made good progress. CIOMP has completed polishing the mirror, the prototype mechanism is nearly assembled, some testing has been performed, and additional testing is being planned and prepared. A dummy mirror is being integrated into the cell assembly prototype to verify the design, analysis and interface and will be used when testing the prototype positioner tilt and rotation motions. The prototype positioner tilt and rotator structures have been assembled and tested to measure each subsystem’s jitter and dynamic motion. The mirror prototype has been polished and tested to verify the polishing specification requirement and the mirror manufacturing process. The complete assembly, integration and verification of the prototype will be soon finished. Final testing will verify the prototype requirements including mounted mirror surface figure accuracy in 5 different orientations; rotation and tilt motion calibration and pointing precision; motion jitter; and internally generated vibrations. CIOMP has scheduled to complete the prototype by the end of July 2016. CIOMP will get the sufficient test results during the pre-construction phase to prepare to enter the preliminary design for GSSM.
The Changchun Institute of Optics, Fine Mechanics and Physics (CIOMP) team is developing the Giant Steerable Science Mirror (GSSM) for Thirty Meter Telescope (TMT) which will get into the preliminary design phase in 2016. To develop the passive support structure system for the largest elliptic-plan flat mirror and smoothest tracking mechanism for the gravity-invariant condition, CIOMP is designing and building a 1/4 scale, functionally accurate version of the GSSM prototype. The prototype will incorporate the same optical-mechanical system and electric control system as the GSSM. The size of the prototype mirror is 898.5mm×634mm×12.5mm with elliptic-plan figure and will be supported by 18 points whiffletree on axial and 12 points whiffletree on lateral. The mirror surface figure will be evaluated by SlopeRMS which is the final evaluation method used in the actual GSSM. The prototype allows the mirror point to and be tested in five specified gravity orientations and meet the requirements of SlopeRMS. The prototype testing platform will have the interfaces with direct drive systems. The jitter testing will be implemented on the prototype system to verify the bearing, the encoder, the servo control algorithm in the low speed up to 5 arcsecond per second. The total prototype system configured mirror surface figure will be better than 1 micro radian SlopeRMS in each tested orientation. The positioner jitter will be less than 0.1 arcsecond RMS for tilt and rotator axis respectively and will be analyzed with frequency domain to meet the requirements of the TMT adaptive optics system. The pre-construction will be completed at the beginning of 2016 and provide the technical support to the preliminary design of GSSM.
For large aperture telescope, we place the significance on the jitter of the wave front parameters when we make
effort to obtain better image. We investigate the power spectral density for charactering the optical jitter for large
telescope as stochastic sequence. Limited by frequency domian property, the universal used metric, and root mean square
of wave front error (RMS WFE) cannot provide adequate information .This paper provides a complete and easy-to-use
approach to the specification of mid-and-high frequency aberration of the wave front. Additionally, we apply welch
method to the calculation of the power spectral density to achieve the accuracy result without much noise involved.
Lastly, we verify this theory by the analysis of a laser system.
We investigate a new metric power spectral density (PSD),for characterizing the performance of seeing-limited large telescope such as thirty meter telescope(TMT ). As the PSD is directly related to the performance of the atmosphere which plays an important role in ground based facilities, it represents the efficiency lose due to mid and high-spatial frequency components in observing time. The metric also properly counts for the optic error of the mirror itself such as the deviations from a perfect surface, and metrology measurement errors .The metric can multiply all the errors which differentiates from the traditional ones, such as RMS. We also numerically confirm this feature for Karman model atmosphere error multiplied with the sample of our vendor and the TMT M3.Additonaly, we discuss other pertinent feature of the PSD, including its relationship to Zernike aberration ,and RMS of wave front errors.
With the aperture of large ground-based telescopes increasing, thermal issues appear more evidently. As a relatively large thermal expansion coefficient SiC (about 2.5x10-6 /K), it makes large aperture SiC lightweight primary mirror more sensitive to temperature gradient. Firstly, discuss thermal issue of the mirror seeing induced by the temperature difference between the mirror surface and ambient theoretically. Then analyze the mirror surface deformation under seven different steady-state temperature fields with a unit temperature load. A uniform axial gradient can cause a mirror surface deflection RMS which can reach 438.4 nm. According to the simulation results, it shows that the primary is most sensitive to a uniform axial gradient and least to uniform change. Lastly, the parameter of thermal control is determined through the above analysis with the error budget to get a better image quality.
The tertiary mirror positioned assembly (M3PA) of the thirty meters telescope (TMT) is the largest tertiary mirror pointing system in the world. The tracking and pointing performance of M3PA is better than any other telescopes which have been built, and the working condition is even worse, so the designers face an enormous challenge. The tracking system includes the bottom rotator shaft and the tilt shaft. The study of this paper focuses on the tilt shaft. There are mainly three forms. The first form is one end fixed with the other unrestrained in axial direction. The second form uses two pairs of angular contact ball bearing. The last form lays two tape roller bearings. All of them can meet the requirements when the M3PA is vertical. But the first one becomes invalid when the M3PA is horizontal. We pay our attention on the study for the second arrangement method.. This bearing arrangement can produce a good stiffness, and increase the first modal frequency to 15.1Hz. In addition, some analysis were down to study the load applied on the balls. The results show that the maximum load is up to 5000N with the stress of 2300MPa.
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