MUltiplexed Survey Telescope (MUST) proposed by Tsinghua University is a 6.5-meter widefield telescope for the ground-based spectroscopic survey. To realize the design target of large field of view of 7 square degrees, the effective aperture of the secondary mirror is preliminarily designed to be 2.4 meters, and the mass of the secondary mirror assembly is supposed to be about 3 tons. Under different zenith angles, the attitude variation of the secondary mirror assembly will affect the stability of the optical axis and result in the spot drift of the focus image on the focal plane. In this paper, a simulation model of the top end assembly is established. Finite element analysis is carried out to investigate the effects of different parameters of the top end assembly on the performance of the optical system, including the vane horizontal offset angle, the vane altitude offset angle, and different forms of ring assembly. Based on the simulation results, an optimized top end assembly is preliminarily obtained and the magnitude of spot drift on the focal plane could be effectively limited at different zenith angles and field of view (FOV).
The MUltiplexed Survey Telescope (MUST) is a 6.5-meter aperture wide field spectroscopic survey telescope built by Tsinghua University. In the optical system of MUST, the second mirror is designed as a hyperbolic flat-convex reflector with an effective aperture of 2.4 meters. In order to achieve high imaging quality under different zenith angles, lightweighted mirror structure is adopted to effectively reduce the weight of the secondary mirror and depress the deformation of the surface figure. In this paper, a preliminary finite element model of the second mirror with multi-point passive support is established and numerical simulation is utilized to investigate the effects of different light-weighted schemes. In the simulation, parameters of the mirror structure are taken into consideration, including the distribution and the structural forms of the light-weighted holes, the back plate and the rib, and the distribution of the passive supports. According to the optimization results, a light-weighted secondary mirror with 36-point axial support is finally achieved to significantly reduce the weight by more than 70% and effectively improve the surface accuracy to 20nm RMS value. To our best knowledge, this is one of the largest aperture light-weighted secondary mirror with passive supports and the presented light-weighted design could provide a reference for the future development of 2-meter class secondary mirror.
KEYWORDS: Telescopes, Mirrors, Active optics, Distortion, Design and modelling, Multiplexing, Wavefronts, Mirror surfaces, Image quality, Chemical elements
MUltiplexed Survey Telescope (MUST) proposed by Tsinghua University aims to build a 6.5-meter widefield telescope for the ground-based spectroscopic survey. MUST adopts the Ritchey-Chretien system with the Cassegrain focus, consisting of an active support primary mirror, a passive support secondary mirror and a multiple-element widefield corrector. In order to fulfill the needs of the widefield spectroscopic survey, the primary mirror is supported in a specific approach rather than traditional methods, which results in optical distortions in the center region of the beam. In this paper, we presented a self-compensation method using the corrector itself to compensate the optical distortion caused by the primary mirror. Based on the optical system of MUST, an optical model of the self-compensation is established, and numerical simulation is conducted to implement the optimization of the corrector and investigate the self-compensation ability. Simulation results indicate that the surface shapes of the elements inside the corrector could be evolved to realize the self-compensation through the optimization of the widefield corrector, including the materials, surface shapes and load conditions. By using the presented self-compensation method, the optical distortions are well compensated and the image quality at the focal plane could be effectively improved.
The LAMOST completed its first five years of operation in June 2017, and 9 million low resolution spectra are obtained. The spectrographs have been upgraded in 2017, and the resolution can reach up to 7500(with 2/3 slit). In the midresolution mode, the wavelength can cover 495nm-535nm(blue band) and 630nm-680nm(red band). The LAMOST will carry out the middle resolution spectroscopic survey in September 2018, and 3 million middle resolution spectra will be obtained. This paper describes the requirements, optical design and mechanical design of the LAMOST-MRS (the LAMOST middle resolution spectrograph)
The Next Generation Palomar Spectrograph (NGPS) is designed for Cassergrain focus of the Hale 200-inch telescope to replace the old Palomar Double Spectrograph (DBSP). NGPS have higher throughput, efficiency and realities spectrograph. NGPS is designed as three channels to cover the wavelength from 365nm to 1050nm with no spectral gap and delivers a resolving power with a 1.5” slit exceeding R=1800 overall the observable range. The peak efficiency of the whole throughput (from sky to detector) at the wavelength is 35.3% which is consistent with throughput achieved by some of the world’s most efficient spectrographs.
Infrared sky background level is an important parameter of grounded infrared astronomy observations, which should be firstly measured in a good infrared observatory site, and only the site with low background level is suitable for infrared observations. Infrared sky background level can provide background data for the design of related infrared instruments. However, there is no such data available for major sites in China. Based on the requirement, In order to supplement the current site survey data and guide the design of future infrared instruments, a multiband near-infrared sky brightness monitor (MNISBM) based on an InSb sensor is designed in this paper. The MNISBM consists of optical system, mechanical structure and control system, detector and cooler, high gain readout electronic system, operational software. It is completed and carried out an experimental measurement in the laboratory. The result shows that the sensitivity of the MNISBM meets the requirements of the measurement of near-infrared sky background level.
High accuracy radial velocity measurement isn’t only one of the most important methods for detecting earth-like
Exoplanets, but also one of the main developing fields of astronomical observation technologies in future. Externally
dispersed interferometry (EDI) generates a kind of particular interference spectrum through combining a fixed-delay
interferometer with a medium-resolution spectrograph. It effectively enhances radial velocity measuring accuracy by
several times. Another further study on multi-delay interferometry was gradually developed after observation success
with only a fixed-delay, and its relative instrumentation makes more impressive performance in near Infrared band.
Multi-delay is capable of giving wider coverage from low to high frequency in Fourier field so that gives a higher
accuracy in radial velocity measurement. To study on this new technology and verify its feasibility at Guo Shoujing
telescope (LAMOST), an experimental instrumentation with single fixed-delay named MESSI has been built and tested
at our lab. Another experimental study on multi-delay spectral interferometry given here is being done as well. Basically,
this multi-delay experimental system is designed in according to the similar instrument named TEDI at Palomar
observatory and the preliminary test result of MESSI. Due to existence of LAMOST spectrograph at lab, a multi-delay
interferometer design actually dominates our work. It’s generally composed of three parts, respectively science optics,
phase-stabilizing optics and delay-calibrating optics. To switch different fixed delays smoothly during observation, the
delay-calibrating optics is possibly useful to get high repeatability during switching motion through polychromatic
interferometry. Although this metrology is based on white light interferometry in theory, it’s different that integrates all
of interference signals independently obtained by different monochromatic light in order to avoid dispersion error caused
by broad band in big optical path difference (OPD).
Exoplanet detection, a highlight in the current astronomy, will be part of puzzle in astronomical and astrophysical future,
which contains dark energy, dark matter, early universe, black hole, galactic evolution and so on. At present, most of the
detected Exoplanets are confirmed through methods of radial velocity and transit. Guo shoujing Telescope well known
as LAMOST is an advanced multi-object spectral survey telescope equipped with 4000 fibers and 16 low resolution fiber
spectrographs. To explore its potential in different astronomical activities, a new radial velocity method named
Externally Dispersed Interferometry (EDI) is applied to serve Exoplanet detection through combining a fixed-delay
interferometer with the existing spectrograph in medium spectral resolution mode (R=5,000-10,000). This new
technology has an impressive feature to enhance radial velocity measuring accuracy of the existing spectrograph through
installing a fixed-delay interferometer in front of spectrograph. This way produces an interference spectrum with higher
sensitivity to Doppler Effect by interference phase and fixed delay. This relative system named Multi-object Exoplanet
Search Spectral Interferometer (MESSI) is composed of a few parts, including a pair of multi-fiber coupling sockets, a
remote control iodine subsystem, a multi-object fixed delay interferometer and the existing spectrograph. It covers from
500 to 550 nm and simultaneously observes up to 21 stars. Even if it’s an experimental instrument at present, it’s still
well demonstrated in paper that how MESSI does explore an effective way to build its own system under the existing
condition of LAMOST and get its expected performance for multi-object Exoplanet detection, especially instrument
stability and its special data reduction. As a result of test at lab, inside temperature of its instrumental chamber is stable
in a range of ±0.5degree Celsius within 12 hours, and the direct instrumental stability without further observation
correction is equivalent to be ±50m/s every 20mins.
The quality of the range image obtained by laser radar will directly influence the target profile reconstruction and the
target identification, and the quality of the range image is mainly determined by the parameters of laser radar system. As
a result, this paper concentrates on discussing the effect of laser radar's parameters on the quality of range image. To
evaluate the quality of range image quantitatively, two parameters, the mean squared error of range (R-MSE) and peak
signal noise ratio of range (R-PSNR), are introduced and a simulation program is developed to study the influence of
system's parameters on the range imaging quality. The results show that for a given pulse width, there has an optimal
bandwidth and threshold level, that make the range image has better image quality. Above results have important
significance to optimize the parameter design of laser radar.
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