To address the installation challenges of a 2-m ring Gregorian telescope system,and similar optical systems with a small width-to-radius ratio,we propose a detection method combining local interferometry with a compar...To address the installation challenges of a 2-m ring Gregorian telescope system,and similar optical systems with a small width-to-radius ratio,we propose a detection method combining local interferometry with a comparison model.This method enhances the precision of system calibration by establishing a dataset that delineates the relationship between secondary mirror misalignment and wavefront aberration,subsequently inferring the misalignment from interferometric detection results during the calibration process.For the 2-m ring telescope,we develop a detection model using five local sub-apertures,enabling a root-mean-square detection accuracy of 0:0225λ(λ=632:8 nm)for full-aperture wavefront aberration.The calibration results for the 2-m Ring Solar Telescope system indicate that the root-mean-square value of sub-aperture wavefront aberration reaches 0.104λ,and the root-mean-square value of spliced full-aperture measurement yields reaches 0.112λ.This method offers a novel approach for calibrating small width-toradius ratio telescope systems and can be applied to the calibration of other irregular-aperture optical systems.展开更多
The National Solar Observatory is currently developing the Accurate Infrared Magnetic Field Measurements of the Sun(AIMS). The primary mirror of the AIMS solar telescope is an off-axis parabolic with a diameter of 1 m...The National Solar Observatory is currently developing the Accurate Infrared Magnetic Field Measurements of the Sun(AIMS). The primary mirror of the AIMS solar telescope is an off-axis parabolic with a diameter of 1 m and with a large off-axis amount of 1 m. Due to the surface figure of the primary mirror under the used state is directly related to image quality of the whole system, a computer-generated hologram(CGH) is carried out to test the primary mirror, and the test results are used to polish the mirror to a higher surface accuracy. However, the fact that the distortion exists in the testing results leads to the failure of a further guide to deterministic optical processing. In this paper, a distortion correction method is proposed, which uses an orthogonal set of vector polynomials to mapping the coordinates of the mirror and the pixels of fringes, and then an interpolation method is adopted to obtain the corrected results. The testing accuracy by using CGH is also verified by an auto-collimate test experiment. According to the distorted corrected results, the root-mean-square of the surface figure is about 1/50λ(λ=632.8 nm) after polishing.展开更多
The impact of structural stiffness on optical axis deviation poses a significant challenge in the design of equatorial telescope structures.A comprehensive analysis during the design process can reduce the reliance of...The impact of structural stiffness on optical axis deviation poses a significant challenge in the design of equatorial telescope structures.A comprehensive analysis during the design process can reduce the reliance of a telescope on advanced control technologies,thereby improving its economic feasibility.Although full-system finite element analyses are reliable,they are encumbered by significant time requirements and limitations in covering all possible telescope orientations.Therefore,we propose an efficient and comprehensive analytical method to evaluate the optical axis deviation of equatorial telescopes across a full range of angles.To address the challenge of ensuring that the analysis covers all possible positions of an equatorial telescope,based on a model from SiTian project,we analyze the optical axis deviations caused by the fork arm at 25 different angles and then use fitting methods to obtain results for all angles.Based on the analysis results of the optical axis deviation caused by the stiffness of the optical tube in the horizontal position,we derive the results for the tube at any position using geometric relationships.Finally,we calculate the coupling factors and combine these impacts.Furthermore,we identify six discrete feature points to reflect possible telescope orientations and conduct comprehensive finite element analyses.The results are in alignment with those acquired through a comprehensive computational approach.展开更多
The photoelectric properties of conductive films are improved by doping Ag on aluminum-doped zinc oxide(AZO)films by laser induced forward transfer(LIFT).Firstly,the picosecond laser induced transfer mechanism of Ag f...The photoelectric properties of conductive films are improved by doping Ag on aluminum-doped zinc oxide(AZO)films by laser induced forward transfer(LIFT).Firstly,the picosecond laser induced transfer mechanism of Ag films was revealed by numerical simulation;then,different-thickness Ag films were deposited on the AZO films by picosecond LIFT.When the film thickness is 30 nm and,50 nm,we have successfully obtained some Ag-AZO films with better optoelectronic properties by adjusting the laser parameters.展开更多
This paper introduces configuration of the main optical system of China’s 2.16-m telescope and the results of its optical design. There are three foci in this telescope: the Cassegrain, the coude and the prime foci. ...This paper introduces configuration of the main optical system of China’s 2.16-m telescope and the results of its optical design. There are three foci in this telescope: the Cassegrain, the coude and the prime foci. Ritchey-Chretien (R-C) system is used as the Cassegrain system. The 2-lens and 3-lens correctors are prepared for the Cassegrain and the prime foci respectively. The most significant characteristic of this optical system is that the coude and Cassegrain systems share one secondary mirror. A relay mirror is added to the coude system. When the two systems exchange, the secondary mirror moves slightly, and the coude system obtained is free from both spherical aberration and coma simultaneously. Some other coude configurations and a special configuration for setting the focal reducer are also introduced in this paper.展开更多
基金supported by the Jiangsu Provincial Key Research and Development Program(BE2022072)the National Natural Science Foundation of China(12141304)the Natural Science Foundation of Jiangsu Province(BK20231134).
文摘To address the installation challenges of a 2-m ring Gregorian telescope system,and similar optical systems with a small width-to-radius ratio,we propose a detection method combining local interferometry with a comparison model.This method enhances the precision of system calibration by establishing a dataset that delineates the relationship between secondary mirror misalignment and wavefront aberration,subsequently inferring the misalignment from interferometric detection results during the calibration process.For the 2-m ring telescope,we develop a detection model using five local sub-apertures,enabling a root-mean-square detection accuracy of 0:0225λ(λ=632:8 nm)for full-aperture wavefront aberration.The calibration results for the 2-m Ring Solar Telescope system indicate that the root-mean-square value of sub-aperture wavefront aberration reaches 0.104λ,and the root-mean-square value of spliced full-aperture measurement yields reaches 0.112λ.This method offers a novel approach for calibrating small width-toradius ratio telescope systems and can be applied to the calibration of other irregular-aperture optical systems.
基金funded by the West Light Foundation of the Chinese Academy of Sciences(Grant No.XAB2017B13)the National Natural Science Foundation of China(Grant No.11703072)。
文摘The National Solar Observatory is currently developing the Accurate Infrared Magnetic Field Measurements of the Sun(AIMS). The primary mirror of the AIMS solar telescope is an off-axis parabolic with a diameter of 1 m and with a large off-axis amount of 1 m. Due to the surface figure of the primary mirror under the used state is directly related to image quality of the whole system, a computer-generated hologram(CGH) is carried out to test the primary mirror, and the test results are used to polish the mirror to a higher surface accuracy. However, the fact that the distortion exists in the testing results leads to the failure of a further guide to deterministic optical processing. In this paper, a distortion correction method is proposed, which uses an orthogonal set of vector polynomials to mapping the coordinates of the mirror and the pixels of fringes, and then an interpolation method is adopted to obtain the corrected results. The testing accuracy by using CGH is also verified by an auto-collimate test experiment. According to the distorted corrected results, the root-mean-square of the surface figure is about 1/50λ(λ=632.8 nm) after polishing.
文摘The impact of structural stiffness on optical axis deviation poses a significant challenge in the design of equatorial telescope structures.A comprehensive analysis during the design process can reduce the reliance of a telescope on advanced control technologies,thereby improving its economic feasibility.Although full-system finite element analyses are reliable,they are encumbered by significant time requirements and limitations in covering all possible telescope orientations.Therefore,we propose an efficient and comprehensive analytical method to evaluate the optical axis deviation of equatorial telescopes across a full range of angles.To address the challenge of ensuring that the analysis covers all possible positions of an equatorial telescope,based on a model from SiTian project,we analyze the optical axis deviations caused by the fork arm at 25 different angles and then use fitting methods to obtain results for all angles.Based on the analysis results of the optical axis deviation caused by the stiffness of the optical tube in the horizontal position,we derive the results for the tube at any position using geometric relationships.Finally,we calculate the coupling factors and combine these impacts.Furthermore,we identify six discrete feature points to reflect possible telescope orientations and conduct comprehensive finite element analyses.The results are in alignment with those acquired through a comprehensive computational approach.
基金partially supported by the Jiangsu Government Scholarship for Overseas Studies(No.JS-2018-253)the Jiangsu Natural Science Foundation Youth Fund(No.BK20150529)the National Science Foundation for Post-doctoral Scientists of China(No.2015M571678)。
文摘The photoelectric properties of conductive films are improved by doping Ag on aluminum-doped zinc oxide(AZO)films by laser induced forward transfer(LIFT).Firstly,the picosecond laser induced transfer mechanism of Ag films was revealed by numerical simulation;then,different-thickness Ag films were deposited on the AZO films by picosecond LIFT.When the film thickness is 30 nm and,50 nm,we have successfully obtained some Ag-AZO films with better optoelectronic properties by adjusting the laser parameters.
文摘This paper introduces configuration of the main optical system of China’s 2.16-m telescope and the results of its optical design. There are three foci in this telescope: the Cassegrain, the coude and the prime foci. Ritchey-Chretien (R-C) system is used as the Cassegrain system. The 2-lens and 3-lens correctors are prepared for the Cassegrain and the prime foci respectively. The most significant characteristic of this optical system is that the coude and Cassegrain systems share one secondary mirror. A relay mirror is added to the coude system. When the two systems exchange, the secondary mirror moves slightly, and the coude system obtained is free from both spherical aberration and coma simultaneously. Some other coude configurations and a special configuration for setting the focal reducer are also introduced in this paper.
