Guo Shoujing Telescope

Large sky area multi-target optical fiber spectroscopic telescope

Collection

zero Useful+1

zero

synonym lamost (most) generally refers to Guo Shoujing's telescope

The large sky area multi-target optical fiber spectroscopic astronomical telescope (LAMOST for short) is a large field of view and large aperture telescope with the largest aperture in the world, independently innovated in China and developed by the National Astronomical Observatory of the Chinese Academy of Sciences Telescope with the most spectrum by 2023^[15] 。 yes Chinese Academy of Sciences National Astronomical Observatory National major scientific and technological infrastructure field It is the ritual reflection of the Midstar lying 5 degrees in the north-south direction Schmidt telescope 。^[1]

LAMOST was established in 1997, started construction in 2001, passed national acceptance in June 2009, and was named“ Guo Shoujing Telescope ". In September 2012, the official sky patrol was launched. In August 2021, based on the observation data of LAMOST, researchers found a very rare new type of cataclysmic variable star.^[4]

Based on the massive spectral data of LAMOST, researchers from the National Astronomical Observatory of the Chinese Academy of Sciences and other units have discovered 1417 compact galaxies.^[5] By September 2022, the Guo Shoujing telescope has been in operation for 11 years, About 20 million spectral data were released.^[8] In March 2023, the total number of spectra released by Guo Shoujing Telescope will exceed 20 million, reaching 22.29 million. LAMOST, a large scientific device in China with the largest number of spectra in the world, has been obtained for ten consecutive years, making it the first sky survey project in the world to release more than 20 million spectra.^[16]

In March 2024, LAMOST has released more than 25.12 million spectral data, LAMOST is still the only spectral survey project in the world that releases tens of millions of spectra^[17] 。

Chinese name: Guo Shoujing Telescope (large sky area multi-target optical fiber spectrum telescope)
Foreign name: Large Sky Area Multi-Object Fiber Spectroscopy Telescope

Recumbent degree: 5 degrees
project investment: RMB 235 million
First proposed construction: April 1993
Location: Xinglong County, Hebei Province

catalog

brief introduction

Announce

edit

Figure 1 LAMOST

Large sky area multi-target optical fiber spectroscopic telescope LAMOST is a horizontal north-south Transit Type reflex Schmidt telescope 。 The active optical technology is applied to control the reflection correction plate, so that it becomes both large aperture and large field Optical telescope The best in the world. Because its aperture is up to 4 meters, objects of 20.5 degrees of darkness can be observed within 1.5 hours of exposure. Since its field of view is up to 5 °, 4000 optical fibers can be placed on the focal plane to transmit the light of distant celestial bodies to multiple stations a spectrometer And get their spectrum And become the telescope with the highest spectral acquisition rate in the world. It will be placed at Xinglong Observatory of the National Astronomical Observatory (Figure 1 is the effect picture), making it the largest optical spectral observation in China field In astronomical research Large scientific device 。

Over the years, China's astronomical community has built a space of 2.16 meters and 1.56 meters Optical telescope 1.26m Infrared telescope , solar magnetic field and multi-channel telescope, 13.7m Millimeter wave , Mibo Synthetic aperture , and very long baseline interference radio telescope Represented by the astronomical measurement infrastructure Astronomical research The development of China's astronomy has improved its position in the world. LAMOST aimed at astronomy and Astrophysics The large field of view astronomy, which has many cutting-edge issues, seized the valuable opportunity of large-scale optical spectrum development, and realized the large aperture and large size of optical telescopes with novel ideas and ingenious designs field Breakthrough. LAMOST telescope reflected from the north end Schmidt correction plate MA、 The spherical primary mirror MB at the south end is composed of the focal plane in the middle. sphere Primary mirror And the focal plane is fixed on the foundation, and the reflection Schmidt correction plate is used as Heliostat Tracking the movement of celestial bodies, telescopes observe celestial bodies before and after they pass through the midheaven. The light of the celestial body is reflected to MB by MA, and then imaged on the focal plane after being reflected by MB. The optical fiber placed on the focal plane transmits the light of celestial bodies to a spectrometer Through the slit of the spectrometer CCD detector At the same time, the spectra of a large number of celestial bodies are obtained (Fig. 2 is the schematic diagram of light path).

Figure 2

The optical spectrum contains abundant physical information of distant objects. The acquisition of a large number of optical spectra of objects involves astronomy and Astrophysics The key to the large field of view and large sample astronomy research of many frontier problems. However, up to now, only a small part (about one in ten thousand) of the tens of billions of various celestial bodies recorded by imaging surveys have undergone spectral observations. LAMOST, as the telescope with the highest acquisition rate of celestial spectrum, will break through Astronomical research This "bottleneck" of mid spectral observation has become the most powerful spectral survey telescope field A powerful tool for large sample astronomical research. LAMOST a quasar The spectral surveys of extragalactic objects such as galaxies, quasars and Large scale structure of the universe And made significant contributions to the research. Spectral surveys of a large number of stars and other Hanoi objects will be carried out in Hanoi astrophysics and Galaxy In research, such as stars Astral family And the structure of the Milky Way kinematics And chemistry. Combined with infrared radio 、 X-ray 、 Gamma ray The spectral observation of a large number of celestial bodies in the sky survey will make a significant contribution to the multi band cross identification of various celestial bodies.

LAMOST project is divided into seven subsystems: optical system; Active optics and support system; Rack and tracking device; Telescope control system; Focal plane instrument; Dome; Data processing and computer integration. The telescope is placed on Chinese Beijing Astronomical Observatory Xinglong Observatory, with a total investment of about 235 million yuan, will be opened to the national astronomical community as a national equipment and actively carry out international cooperation.

LAMOST passed the national acceptance on June 4, 2009, becoming the largest in the world field The telescope with the highest acquisition rate of spectral observation provides high-level observation means and research platform for astronomical research in China and even the world, and has been highly praised by the international astronomical community.

By September 2022, the Guo Shoujing telescope has been in operation for 11 years, A total of about 20 million spectral data were released, about twice the total spectral data released by all other international optical survey projects.^[8]

Technical achievements

Announce

edit

survey

Technically, LAMOST in its reflection Schmidt corrector At the same time, thin mirror active optics and splicing mirror active optics technology are used in the Optical telescope large field At the same time, it also has a breakthrough in large caliber. The parallel controllable optical fiber positioning technology solves the problem of accurately positioning 4000 observation targets at the same time, which is also an international leading technological innovation.

LAMOST has exceeded the internationally completed or ongoing large field of view multi celestial body spectral survey plan in terms of aperture, field of view and number of optical fibers, and its scientific objectives focus on Extragalactic galaxy Observation of, Galaxy structure And evolution, as well as multi band target identification. It affects nearly ten million galaxies a quasar Spectral observations of extragalactic objects, such as cosmological models 、 Large scale structure of the universe And galaxy formation and evolution. Spectral surveys of a large number of stars will make significant contributions to the study of the structure and evolution of the Milky Way Galaxy and stellar physics. Combined with infrared radio 、 X-ray 、 Gamma ray The spectral observation of a large number of celestial bodies in the sky survey will make a significant contribution to the multi band cross identification of various celestial bodies.

LAMOST telescope is located in Xinglong Observatory of the National Astronomical Observatory. As a national equipment, LAMOST telescope is open to the national astronomical community and actively carries out international cooperation. LAMOST will enable Chinese astronomy to field In astronomy research, it is in the leading position in the world.

characteristic

The most prominent feature of LAMOST telescope is large aperture (4m) and large field (5 degrees) and 4000 optical fibers. It is the same type of international sky patrols, such as the United States Sloan Digital Sky Survey Program (SDSS) and Australia British Australian Observatory 2dF sky survey comparison, LAMOST has made great strides in both telescope aperture and observation efficiency.

Subsystem

Figure 3 LAMOST Working Principle

LAMOST telescope consists of eight subsystems, namely optical system , active optics and support system, gantry and tracking system, telescope control system, focal plane instrument, dome, observation control and data processing system, input catalog and sky survey strategy.

The optical system consists of a spherical primary mirror MB at the south end and a reflective Schmidt corrector MA at the north end, with the focal plane in the middle. The optical axis is high in the south and low in the north to adapt to the latitude of the station site and expand the observation area. The spherical primary mirror MB is 6.5 m × 6 m in size and consists of 37 hexagonal shapes with 1.1 m diagonal diameter Spherical mirror It is spliced together. The reflective Schmidt corrector MA is 5.7m × 4.4m in size, and is composed of 24 hexagonal active aspherical mirrors with a diagonal diameter of 1.1m. The spherical primary mirror MB is fixed, and the pointing and tracking movement of the celestial body is completely undertaken by MA. As Heliostat The MA adopts the horizontal frame, and its pointing and tracking are realized by the rotation of azimuth and altitude. The telescope makes observations before and after the celestial body passes through the middle sky.

key technology

Figure 4 LAMOST focal plane

Active optics technology is the most challenging and core key technology of LAMOST project. In order to correct the spherical aberration of spherical primary mirror MB, real-time changes are required during observation Corrector Aspherical surface shape of MA, Active optics The system deforms 24 thin flat sub mirrors as required by combining thin mirror surface and splicing mirror surface active optical technology, and makes all sub mirrors confocal. Thousands of force actuators control each sub mirror of MA in real time to achieve the required shape. The 37 sub mirrors of MB are directly connected to the main truss through the adjustment mechanism of the active displacement actuator, and confocal is achieved by using the active optical technology of the spliced mirror surface.

LAMOST system has applied thin mirror active optical technology and mosaic mirror active optical technology on the same large mirror for the first time in the world, and also used two large mosaic mirrors in one optical system for the first time. The splicing of spherical primary mirror is an important part of the key technology of the project, and also one of the keys to greatly reduce the project cost.

The telescope collects the weak radiation from the celestial body, images it on the focal plane, and then uses the focal plane instruments for light splitting, detection and recording. The focal plane instrument is the part of LAMOST to directly obtain celestial spectral information, including optical fiber positioning device, optical fiber a spectrometer and CCD detector And so on.

"Parallel controllable optical fiber positioning technology" is another independent innovation and key technology of LAMOST. Different from the drilling aluminum plate used by SDSS and the magnetic buckle used by 2dF, LAMOST optical fiber positioning adopts the double rotation optical fiber positioning unit scheme. The diameter of LAMOST focal plane is 1.75 meters, which is similar to the size of the round table we use for dinner, as shown in Figure 4. The positioning system can accurately position the 4000 optical fibers on the focal plane according to the star position in a few minutes, and provide fine adjustment of the optical fiber position. 4000 optical fiber positioning units are arranged at an equal distance of 25.6 mm on the focal plane, and each unit drives the optical fiber to work within the range of 33 mm in diameter. The advantage of LAMOST positioning system is that 4000 positioning units work in parallel, greatly reducing the positioning time. It also avoids the trouble of replacing the optical fiber aluminum plate for every observation like SDSS. On a dining table size focal panel, 8000 motors drive 4000 optical fiber positioning units to rotate, which is also a shocking scene.

structure

Figure 5 LAMOST's hexagonal spherical mirror

Due to LAMOST's original structure, its telescope building is also different from the general Astronomical telescope Dome. It consists of MA building MB building and focal plane instrument building are composed of three parts, as shown in the title drawing. The dome enclosure of MA is cylindrical with a spherical cap, and the upper part can be moved to the east and west. The enclosure from the focal plane to the MB is a horizontal long channel with louvers to reduce the impact of wind on MA, and make the temperature in the optical path uniform to avoid deterioration of natural Atmospheric visual acuity 。

engineering

Announce

edit

April May 1992, Chinese Astronomical Society And the Department of Mathematics and Physics of the Chinese Academy of Sciences to solicit suggestions from the national astronomical community on major astronomical observation equipment for the next stage. with Wang Shouguan The research group led by Academician Su Dingqiang put forward the proposal of building LAMOST in view of the current situation and development opportunities at home and abroad, which has been widely supported by the astronomical community. The implementation of LAMOST project will enable China's astronomy to make large-scale optical spectral observations and field In astronomical research, it ranks among the international leaders.

From January to February 1995, the National Science and Technology Commission organized a review of the proposed projects of scientific engineering in various disciplines, LAMOST is at the forefront.

In June 1996, the National Planning Commission and the National Science and Technology Commission organized academicians of the Chinese Academy of Sciences and the Chinese Academy of Sciences to review major national scientific projects, LAMOST is at the forefront.

In July 1996, the National Leading Group for Science and Technology launched the National Major Scientific Project Plan.

In April 1997, the State Planning Commission approved the LAMOST project proposal.

On August 29, 1997, the State Planning Commission approved the feasibility study report of LAMOST project, marking the formal establishment of LAMOST project.

On 12 February 1999, The preliminary design report of LAMOST project has been prepared.

On June 9, 1999, the National Planning Commission entrusted the Chinese Academy of Sciences to approve the preliminary design and budget estimate of LAMOST project.

On February 20, 2000, the data processing and research center project started.

In August 2001, LAMOST project commencement report was approved by the National Planning Commission, and the project entered the formal construction stage.

On the evening of December 3 and 4, 2002, 1 to 1 outdoor active optical test closed loop correction optical system aberration The accuracy research was initially successful, and the accuracy of off-axis aspherical surface on the hexagonal test sub mirror with a diagonal diameter of 1.1 meters and a thickness of 25 mm reached the root mean square value of 42 nanometer 。 This is a research on the most important key technology of LAMOST.

On January 22, 2003, a discussion on LAMOST's "OCS and TCS" 0-cascade debugging system scheme was held in the TCS General Control Development Laboratory of Nanjing Tianguang Institute, and the "Technical Draft for Achieving 0-level OCS and TCS System Joint Debugging" scheme of TCS research team was finally confirmed, and the first successful demonstration of LAMOST's Nanjing Hefei system joint debugging was realized through actual measurement.

In July 2003, LAMOST mass spectrum automatic identification and analysis system has completed the technical and theoretical research work through the joint research of astronomers from the National Astronomical Observatory of the Chinese Academy of Sciences and technical experts from the Institute of Automation, The framework design scheme of LAMOST's most important practical system is thus determined. When LAMOST is completed, it will observe 4000 celestial bodies at a time, supporting a huge astronomical observation database for astronomers to carry out cutting-edge research on this basis. Experts in the field of automation assisted astronomers in finding effective algorithms for automatic identification, classification and parameter measurement of celestial spectra, developed software packages for automatic identification and classification of spectra for LAMOST, and successfully established various types of Spectral library 。

On October 13, 2003, Department of Modern Physics, University of Science and Technology of China The LAMOST-1 observation and control system (OCS-1.20) and the Level 1 sky patrol strategic system (SSS-1.00) undertaken by the OCS research team passed the acceptance. From LAMOST Engineering Headquarters, National Astronomical Observatory Nanjing Institute of Astronomical Optics Technology and University of Science and Technology of China 16 experts and professors form the acceptance expert group.

On October 14, 2003, the LAMOST "Multi unit Intermediate Test System for Optical Fiber Positioning" undertaken by the University of Science and Technology of China passed the expert acceptance, and the test system met the contract requirements. The success of the test shows that the development of LAMOST optical fiber positioning system has made breakthrough progress. The optical fiber positioning system is one of the two key technologies of LAMOST, which requires that 4000 optical fibers be accurately aligned with their respective observation targets in a short time. More mature optical fiber positioning technology is used abroad, including fixed positioning holes, magnetic buttons, etc. Due to the large diameter of LAMOST focal plane (up to 1.75 meters), the number of optical fibers is up to 4000 (up to 640 fibers are practical abroad at present), the existing scheme is difficult to apply directly. University of Science and Technology of China Xing Xiaozheng The "parallel controllable optical fiber positioning" scheme proposed by the professor was finally adopted. The scheme has fast positioning speed and high accuracy, and can real-time compensate the errors caused by temperature and poor atmospheric refraction normal Small deflection angle, direct alignment with stars, small light energy loss, no blind area in observation, 4000 controllable units are composed of the same components, with low processing cost, high reliability and low operating cost. this University of Science and Technology of China The 19 unit prototypes developed successfully passed the acceptance after one and a half years of successful operation, indicating that this key technology has made breakthrough progress.

On January 7, 2004, The prototype experiment of the sub mirror room of the spherical primary mirror part of LAMOST was successfully completed. The main mirror of LAMOST is a large thin mirror using the splicing mirror active optical technology. The diagonal diameter of a single hexagonal sub mirror is 1.1 meters, and the thickness is only 75 mm. Since the beginning of scheme design in 2001, Nanjing Tianguang Institute has gone through several stages, including structural optimization analysis, detail design, several principle and process reviews, outsourcing processing, part modification, aluminum sub mirror test and glass sub mirror test, and finally obtained preliminary conclusions. The spherical primary mirror is the first in China to adopt an inverted rocker mechanism (WHIFFLETREE) and a middle hole membrane mechanism to solve the axial and lateral support problems of the sub mirror, respectively. All the mechanisms are hidden behind the sub mirror, and the structure is compact, avoiding the possible interference of the support system in the splicing mirror surface.

On June 15, 2004, LAMOST observation building is under construction at Xinglong Observation Station of the National Astronomical Observatory. Vice President of the Chinese Academy of Sciences attended the foundation laying ceremony of the observation building Bai Chunli Basic Department of the Ministry of Science and Technology, Department of Science and Technology of Hebei Province, Chengde City Xinglong County , relevant leaders of the National Astronomical Observatory and the construction unit Some members of LAMOST Project Management Committee and Science and Technology Committee, as well as major members of the project headquarters.

In September 2004, the design scheme of 4000 optical fiber focal plane positioning system passed the review and began processing and manufacturing.

On 25 November 2004, Department of Modern Physics, University of Science and Technology of China The LAMOST observation and control system (OCS-2.10) and the sky patrol strategy system (SSS-1.10) that we undertook passed the acceptance. The review expert group is composed of the project headquarters University of Science and Technology of China 18 experts and scholars from the National Astronomical Observatory and the Nanjing Institute of Astronomical Optics and Technology.

On December 30, 2004, the key technology pre research project of LAMOST undertaken by Nanjing Institute of Astronomical Optics“ Large aperture active optical experimental telescope ”Passed acceptance and achievement appraisal in Nanjing. Experts believe that this device is the first one adopted internationally Active optics Reflection of technology Schmidt telescope High precision test results are obtained through field test. The device uses a hexagonal thin mirror as an active optical Deformable mirror , developed relevant calibration calculation method of active correction force, and adopted active optics Open loop control The technology successfully produces off-axis aspherical surfaces on thin mirrors, which compensates the aberration , solved the problem of large diameter and field One of the key technologies of the reflecting Schmidt telescope is an international initiative. The successful experiment of this device shows that China has mastered the key technology of active optics with large aperture and thin mirror, and has created a new situation of large aperture and large field of view observation in astronomical optics, which has great application prospects in astronomy and national defense.

On January 14, 2005, The first batch of four MB sub mirrors processed by Russia Lytkarino Optical Glass Factory (JSC LZOS) entrusted by LAMOST project arrived at Nanjing Institute of Astronomical Optics and Technology safely (accepted in Russia in November 2004). LAMOST's spherical primary mirror (MB for short) has a size of 6.67m × 6.05m, a radius of curvature of 40m, and is composed of 37 hexagonal spherical sub mirrors with a diagonal length of 1.1m and a thickness of 75mm, which is difficult to process. The technical indicators of the four sub mirrors in this acceptance fully meet the requirements of LAMOST project. On January 18, 2005, LAMOST Engineering Headquarters and University of Science and Technology of China The "LAMOST focal plane optical fiber positioning device development contract" was signed in Hefei.

On April 15, 2005, LAMOST low resolution a spectrometer The prototype passed the expert evaluation. LAMOST needs to be configured with 16 sets of medium and low resolution multi-target ocean optics And a high resolution Step grating Spectrometer and low resolution spectrometer prototype have been completed. The expert group listened to the prototype development report and test report, and inspected the site. The expert group believes that the main indicators of the spectrometer are as follows spectral resolution Etc., which can be covered by the CCD used for detection Spectral range It has reached the design index requirements and is consistent with the optical calculation results. Due to the limited experimental conditions, some performance indicators cannot be detected. The next step will be to improve the detection equipment to ensure that the sample spectrometer has complete detection results.

On April 20, 2005, Nanjing Institute of Astronomical Optics Technology Undertaken by the hospital Device update Special fund support project - 3.6m Circular throwing machine It passed the on-site acceptance of the expert group in Nanjing. LAMOST is used for 3.6m ring polishing machine Schmidt corrector It has been configured as required by development and has completed trial operation. After strict acceptance procedures, the expert group agreed that: various quantitative items of the 3.6m ring throwing machine Qualitative indicators They have all met the requirements of the LAMOST project Ma sub mirror optics. They are in normal operation and can meet the requirements of the intended objectives of the LAMOST project Ma sub mirror optics. We agree to accept them. On May 18, 2005, LAMOST horizontal rack completed the electromechanical preliminary joint commissioning in Nanjing, after tracking accuracy and pointing Repeated positioning accuracy The preliminary test shows that all indicators meet the design requirements. This means that the LAMOST horizontal rack has reached the requirements before it was disassembled for shipment, which is another milestone in the development process of LAMOST. From May 30 to June 2, 2005, the "International Mid term Assessment of LAMOST Project" was held in Nanjing and Beijing. Nine internationally renowned astronomical instrument experts and astronomers from Britain, the United States, Australia, France and Germany served as judges. Experts visited LAMOST's 8-meter MA horizontal rack On site installation and adjustment of MB truss and outdoor experiment of active optics Telescope device Active optics laboratory, force actuator laboratory, multi-target ocean optics Prototype MA/MB sub mirror prototype, friction drive test MB sub mirror and MA sub mirror being ground in the institute, and discussed the four reports submitted at the meeting and the problems and difficulties existing during the project construction.

On June 3-4, 2005, the "Antarctic DOME C/A University" held in Beijing field Seminar on Sky Survey Telescope ". Foreign astronomers proposed to build a larger LAMOST telescope in the South Pole. Echoing the LAMOST of the National Astronomical Observatory from afar, complete depth spectral observation of the whole sky is carried out.

On June 16, 2005, The first batch (4 pieces in total) of MA sub mirrors developed by Nanjing Institute of Astronomical Optics and Technology entrusted by LAMOST successfully passed the acceptance in Nanjing. Reflective type of LAMOST project Schmidt correction plate (referred to as MA mirror for short) is 5.7 meters long and 4.4 meters wide, and is composed of 24 MA sub mirrors. The shape of the sub mirror is Regular hexagon The diagonal dimension is 1.1 m and the thickness is 25 mm. It is characterized by large diameter, small thickness and high surface accuracy. The acceptance team listened to the development report and test report and carried out spot inspection on the site. The acceptance team believed that the four sub mirrors have all met the technical requirements of the contract, their process flow is reasonable, and the development of large aperture high-precision thin plane optical mirrors has reached the leading level in China.

In September 2005, LAMOST and SDSS signed a memorandum on LAMOST's participation in the "SLOAN Digital Sky Survey II". On September 20, 2005, LAMOST's first large equipment MA rack Nanjing Institute of Astronomical Optics Technology It was launched and transported to Xinglong Observatory of the National Astronomical Observatory, marking that the development of LAMOST has achieved phased results, which is a milestone in LAMOST project construction.

On November 18, 2005, Department of Modern Physics, University of Science and Technology of China The observation control system (OCS-2.20) and observation strategy system SSS-2.00, the sub project of LAMOST, were accepted. The expert review team is composed of LAMOST project headquarters University of Science and Technology of China 21 experts from National Astronomical Observatory and Nanjing Institute of Astronomical Optics Technology.

On December 24, 2005, the reflection of LAMOST body was formed Schmidt corrector The installation of (MA) frame, spherical mirror (MB) truss and focal plane mechanism in Xinglong Observation Station was successfully completed, and all indicators met the design requirements, marking that LAMOST project has entered the field installation and commissioning stage.

On April 12, 2006, three hexagonal spherical MB sub mirrors with a diagonal diameter of 1.1 m Nanjing Institute of Astronomical Optics Technology The successful splicing is another major progress of LAMOST project. It is the first time in the world that thin mirror (deformable mirror) active optical technology and mosaic mirror active optical technology are simultaneously applied on the same large mirror. It is also the first time that two large mosaic mirrors are simultaneously used in one optical system. The splicing of spherical primary mirror is an important part of this key technology, and also one of the keys to greatly reduce the project cost. In addition, the mosaic mirror active optical technology is also the future giant ground optics Infrared telescope It is of great significance to master this technology.

In November 2006, 40 MB sub mirrors (including 3 spare sub mirrors) developed by Russia were accepted. On December 27, 2006, 30 LAMOST sub mirrors (including 6 spare sub mirrors) undertaken and developed by Nanjing Institute of Astronomical Optics and Technology passed the acceptance successfully. The acceptance expert group listened to the development report and the acceptance test report, reviewed the relevant technical data and conducted a site visit. The expert group believes that the technical indicators of the 30 MA sub mirrors meet the contract requirements and agree to pass the acceptance, which is another important milestone in the construction process of LAMOST. This work takes the lead in the development of large aperture high-precision non-circular ultra-thin plane in China and reaches the international advanced level Optical Engineering It is of great significance.

On February 4, 2007, LAMOST's first three 1.1 meter hexagonal main mirrors were successfully installed at Xinglong Observatory of the National Astronomical Observatory. LAMOST Primary mirror The installation of LAMOST is very difficult. After repeated preparation of actual combat simulation, the first three sub mirrors were finally installed safely and successfully, marking that LAMOST project has successfully entered the stage of optical installation and adjustment.

On February 27, 2007, LAMOST "Focus optical fiber positioning system (small system) acceptance meeting" Hefei University of Science and Technology of China Held. From the National Astronomical Observatory, Shanghai Astronomical Observatory Nanjing Institute of Astronomical Optics Technology 、 University of Science and Technology of China Acceptance experts and relevant leaders from other units attended the acceptance meeting. The focal plane optical fiber positioning small system includes a small focal panel with a diameter of 600mm, 250 optical fiber positioning units, 250 unit drive control circuit, positioning control software and positioning accuracy Detection system. The experts attending the meeting listened to the development report, the test team checked the detailed test data provided by the project team, and the acceptance team inspected and inspected the site. The acceptance team believes that the small focal panel, optical fiber unit, control system hardware and software and optical fiber position detection system meet the technical requirements, and the small system can pass the laboratory acceptance and be installed on the site in Xinglong Observation Station.

On February 28, 2007, The electromechanical joint commissioning of LAMOST's horizontal frame and focal plane mechanism was successfully completed, and the measured technical indicators were better than the design indicators. The horizontal rack is the largest and most complex precision mechanical system of LAMOST, and it is also the largest and the highest precision required in China Optical telescope Track racks. The focal plane mechanism is used to support the focal plane with a diameter of 1.8 meters and installed with 4000 optical fibers and their positioning mechanism, and plays an important role in eliminating image field rotation, accurately positioning the focal plane and accurately tracking the star image in the observation process. Due to the need for field rotation, attitude adjustment, focusing, and lateral displacement of the space five dimensional accurate movement, the technology is very difficult. The completion of electromechanical joint commissioning is another phased achievement of LAMOST, which has laid a solid foundation for the optical electromechanical joint commissioning and small system to produce light on time.

At 3:00 a.m. on May 28, 2007, LAMOST, which was being debugged, won the first celestial spectrum. With the progress of debugging, LAMOST has continuously obtained more and more celestial spectra in the following two days, marking its various subsystems (telescope optics and active optics, tracking control, optical fiber a spectrometer ）All have been connected and meet the required technical indicators. LAMOST is in the stage of "small system" joint commissioning. After the "small system" is commissioned, the number of mirror sub mirrors will be expanded to 24/37, the number of optical fibers to 4000 and the number of spectrometers to 16.

On June 29, 2007, the "LAMOST Small System Acceptance Meeting" was held in Beijing. LAMOST "small system" consists of a 3-meter aperture mirror, 250 optical fibers and a spectrometer, as well as LAMOST's complete rack, tracking and control system. The Basic Bureau of the Chinese Academy of Sciences organized more than 20 famous experts and scholars in the fields of astronomy, astronomical instruments, optics, precision machinery, electronics and management science to conduct a comprehensive assessment of LAMOST's "small system". The test expert group went to Xinglong Observation Base for field test and inspection on June 18 and 28. The acceptance expert group listened to the development report and the test report of the test expert group, and reviewed the relevant technical data. The expert group believes that "the optical quality of LAMOST small system has fully met the index requirements, and the multi-target optical fiber spectrum system has basically reached the intended goal. Telescope, optical fiber a spectrometer and CCD camera The observation system is well integrated. The successful development of LAMOST small system proves that the overall scheme of the project is correct and the technology and process are feasible. Agree to pass the acceptance. " The success of LAMOST small system is an important milestone in the project construction, which marks that all key technical difficulties in the project construction have been overcome, especially the success of two new technologies, namely, the internationally leading active optical technology of thin mirror and splicing mirror and parallel controllable optical fiber, paving the way for the overall success of the project construction.

1.6 meter box ordered by Nanjing Tianguang in August 2007 Vacuum coating Reliable process parameters have been obtained through equipment commissioning and process experiment, and the reliability of process parameters has been improved for LAMOST project MA The MB sub mirror has been equipped with special tooling, and the coating of three MA sub mirrors and one MB sub mirror of LAMOST has been successfully completed. Through testing, the film quality of these four sub mirrors is excellent, and the mechanical strength of the film is reflectivity All the indexes meet the design requirements.

In mid December 2007, Shanghai Observatory, Chinese Academy of Sciences Astrometry The "LAMOST astrometry support system" undertaken by the group has completed the debugging on the LAMOST small system, and more than 97% of the effective optical fibers have obtained the star light spectrum of the target, laying the foundation for the next step of scientific target test and observation. The astrometric support system is responsible for providing real-time pointing parameters and motion parameters for each moving part of the LAMOST telescope, including Schmidt corrector normal Instantaneous pointing parameters, instantaneous position, attitude and Rotation angle Parameters, positioning parameters of each optical fiber unit. Due to LAMOST field Large (20 Square degree ）, focal length (20m), discrete distribution of receiving units, special working principle Astrometry Support the system to put forward high precision requirements (allowed on the focal plane positioning error 50 microns).

At the end of 2007, The repeatable spectral luminous yield of LAMOST optical fiber positioning system reaches 97% on average, and about two-thirds of the optical mirrors (24 primary mirrors and 16 Schmidt correction mirrors) and 8 multi targets have been installed and debugged ocean optics This ensures that the project will be fully completed in 2008, and lays a good foundation for scientific trial observation.

In January 2008, the National Astronomical Observatory established the "LAMOST Celestial survey Plan Selection and Design Committee ". The committee issued the "LAMOST Data Policy (Exposure Draft)" to promote the enthusiasm of astronomers at home and abroad to use LAMOST observation data for scientific research. The draft for comments has been publicly released to the domestic astronomical community and published on the LAMOST website. The Committee also sent the first notice to astronomers at domestic observatories and other universities to ask for LAMOST scientific observation plans and research topics. The deadline for asking for topics was the end of April 2008, and the first batch of proposed observation plans would be reviewed in May. On the basis of the review, select the best subjects and organize corresponding working groups to promote the comprehensive preparation of LAMOST scientific research.

In March 2008, LAMOST removed the small focal panel for small system, and installed and debugged the LAMOST focal panel. In order to ensure the quality of products, the project headquarters has organized personnel to University of Science and Technology of China The mechanical processing of the developed coke panel has been tested and accepted before delivery and after on-site installation. The results show that the mechanical processing, installation and commissioning of the coke panel meet the design requirements.

On April 4, 2008, Science (Page 34-35, VOL 320) reported the latest progress of LAMOST project. The article, entitled "LAMOST in China is preparing for the final test", introduces the technological innovation, construction process and recent situation of LAMOST, as well as three major scientific goals in detail. Link: original

On April 10, 2008, LAMOST successfully completed the 2/3 mirror assembly and adjustment goal. 16 MA sub mirrors (24 in total) and 24 MB sub mirrors (37 in total) and their supporting systems have been installed and adjusted on site. The test result of the common spherical center of 24 MB sub mirrors shows that 80% of the light energy is concentrated in a circle with a diameter of 0.4 angular seconds, which meets the design technical requirements; The imaging quality of the telescope optical system has reached 80% of the light energy is concentrated in a circle with a diameter of 1.2 angular seconds (the design index is that 80% of the light energy is concentrated in a circle with a diameter of 2.0 angular seconds) through autocollimation correction; The test results fully show that the imaging quality of the telescope optical system is better than the design index. 16 sets equipped a spectrometer Eight sets have completed optical, mechanical and electrical joint commissioning. So far, more than half of the development task of the spectrometer has been completed, and the predetermined goal has been achieved. The comprehensive precision of the telescope star guide tracking can reach 0.42 angular seconds, and the average repeatable spectral luminous yield of the optical fiber positioning system can reach 97%, which ensures the stable and comprehensive luminous output of the entire system, and lays a solid foundation for the next step of scientific target test and observation.

On May 13, 2008“ Astrometry The "Application of Support System in LAMOST Small System" acceptance meeting was held at Shanghai Astronomical Observatory, and the acceptance team was composed of Nanjing Institute of Optical Astronomical Instruments, National Astronomical Observatory University of Science and Technology of China And director of Nanjing Institute of Optical Astronomical Instruments Cui Xiangqun The researcher serves as the leader of the acceptance team. After listening to the summary report of the scientific researchers of the Shanghai Astronomical Observatory Astrometry Research Group, the participating experts evaluated the work of the astrometry support system in the commissioning of the LAMOST project small system. The support system is responsible for providing real-time pointing parameters, motion parameters and guide star corrections for each moving part of LAMOST telescope, mainly including Schmidt corrector normal Instantaneous pointing parameters, instantaneous position, attitude and Rotation angle Parameters, positioning parameters of each optical fiber unit. During the debugging of LAMOST small system, Astrometry Support system and optical, mechanical, electronic control, optical fiber positioning a spectrometer With the close cooperation of all subsystems, under the condition of good weather conditions and instrument status, the comprehensive fluctuation mean square deviation of the telescope's guide and tracking for 1 hour reached 0 ". 42, and the spectral effective luminous yield reached more than 97%, which can be repeated, laying a solid foundation for the next step of LAMOST large-scale system debugging. The acceptance team believes that the design scheme of the support system is effective, and the performance of the hardware and software parts has reached the required indicators, can normally support the realization of the observation process, and has played an important role in the overall commissioning of the small system, and agrees to pass the acceptance.

On June 21, 2008, LAMOST completed 24 reflections at Xinglong Observation Station Schmidt corrector (MA), 37 spherical surfaces Primary mirror (MB) installation. This is an important milestone in the development process of the LAMOST project, marking that the LAMOST project has entered the final stage of on-site commissioning.

On the night of September 27, 2008, During the commissioning of LAMOST telescope, more than 1000 celestial spectra were observed at one time. As of press release, during each commissioning observation, LAMOST continuously obtains the spectra of more than 1000 to 2000 celestial bodies. The celestial body used for debugging observation is generally brighter than 17, and the spectrum is obtained after 5 minutes of cloudless observation night exposure. Compared with the spectrum of more than 600 celestial bodies that can only be observed once in the world, LAMOST has become the telescope with the highest spectral observation rate in the world.

On October 16, 2008, The inauguration ceremony of LAMOST was held at the Xinglong Observation Base of the National Astronomical Observatory. LAMOST completed all hardware installation at the end of August 2008, and began to conduct trial observation. Each index of the telescope has reached or even exceeded the design requirements. During the commissioning process, a single observation can simultaneously obtain more than 3000 celestial spectra. LAMOST has become the largest Optical telescope The largest caliber in the world field The telescope is also the telescope with the highest spectral acquisition rate in the world. Its successful development has made China's large-scale spectral observation in the leading position in the world.

From December 15 to 18, 2008, the Bureau of Basic Science and the Bureau of Planning and Finance of the Chinese Academy of Sciences organized experts to conduct a field test on LAMOST (the equipment part of the project - telescopes and instruments). On December 19, the identification and acceptance expert group carried out the process identification and acceptance. The expert group believes that LAMOST has overcome the difficulty of having both large aperture and large field of view of optical telescopes Primary mirror and Corrector Simultaneous implementation on Active optics Technology, dozens of thin mirrors, real-time adjustment, perfect integration; And 4000 optical fibers are installed in the field of view, which can simultaneously measure the spectrum of 4000 targets. LAMOST has the largest aperture, the widest field of view and the highest spectral acquisition rate in the world Schmidt telescope , praised by international peers. In the development process, there are many technological innovations Large telescope The development lays a solid foundation.

On June 4, 2009, LAMOST in Xinglong Observation Base of National Astronomical Observatory, Chinese Academy of Sciences smoothly

It passed the national completion acceptance organized by the National Development and Reform Commission. The National Development and Reform Commission, the Ministry of Science and Technology State Archives Administration , Foundation Committee, Hebei Province Chinese Academy of Sciences And other relevant departments and experts in relevant fields. Zhang Xiaoqiang, Deputy Director of the National Development and Reform Commission, Executive Vice President of the Chinese Academy of Sciences Leader of LAMOST Engineering Construction Leading Group Bai Chunli Chairman of the committee attended the acceptance ceremony.

In order to promote the smooth implementation of project commissioning and scientific test observation after the completion of LAMOST, a major national scientific project, on May 31, 2010, National Astronomical Observatory, Chinese Academy of Sciences LAMOST Operation and Development Center (now renamed as“ Guo Shoujing Telescope Operation and Development Center (hereinafter referred to as "the Center") consists of the Office, Observation Operation Department, Technical Maintenance and Development Department and Sky Survey and Data Department. Zhao Gang was appointed as the Director of the Center and Zhao Yongheng as the Executive Deputy Director of the Center, Cui Xiangqun As the chief engineer of the Center, Chu Yaoquan 、 Li Guoping Deputy Director of the Center.

On December 15, 2010, the LAMOST Operation and Development Center carried out the Xinglong on-site installation, commissioning and acceptance of the LAMOST coating machine. LAMOST coating machine includes a 1.6m box type coating machine and a 1.4m special coating machine, innovated by Beiyi Vacuum technology Ltd. The two equipment were accepted on the production site in October 2008 and March 2009 respectively. As of December 31, 2010, the optical maintenance team of the Technical Maintenance and Development Department has completed the coating of five MA sub mirrors. After testing, the mirror surface after coating reflectivity It reaches 92%, which is about 10% higher than that before coating.

From December 17 to 18, 2010, Guo Shoujing The International Assessment Meeting of Telescope (LAMOST) Software was held at the National Astronomical Observatory. The successful holding of the evaluation meeting is an important link before the official sky survey of LAMOST telescope, which provides a software guarantee for the star catalog preparation, observation control and data processing required for the sky survey.

In order to better provide LAMOST with astronomical and meteorological environment information for observation, at the end of May 2011, LAMOST environmental monitoring room instruments were installed and debugged in place, and officially put into use.

In May 2011, Important progress has been made in LAMOST optical fiber positioning improvement, 90% of optical fibers positioning accuracy Within one quarter of a second, The overall optical efficiency of LAMOST is about 5% at the blue end and about 10% at the red end, basically reaching the spectrum Celestial survey Requirements.

Technological innovation

Announce

edit

LAMOST is China's independent innovation, which is very challenging in technology Large optical telescope 。 It will be the largest Optical telescope （ Primary mirror 6 meters) and the largest caliber in the world field Optical telescope. LAMOST has a number of international cutting-edge technological innovations, such as:

1. Splicing mirror active optical technology and the simultaneous use of two large splicing mirrors in one optical system (37 1.1m hexagonal sub mirrors are spliced into a 6.67m × 6.58m main mirror, and 24 1.1m hexagonal sub mirrors are spliced into a 5.72m × 4.4m reflective Schmidt corrector);

2. Realize application splicing and deformable mirror on a large mirror in real time during observation Active optics Technology;

3. Hexagonal deformable mirror active control And wavefront detection technology;

4. Accurate positioning of 4000 optical fiber units on the focal plane;

5. Multi target optical fiber spectroscopy technology;

6. Massive data processing technology;

7. Large field Both with large diameter.

three major tasks

Announce

edit

In the early morning of May 28, 2007, LAMOST, which was being debugged at that time, won the first celestial spectrum. With the commissioning, LAMOST obtained more and more celestial spectra in the following days. On the morning of June 18, 2007, more than 120 celestial spectra were obtained from a single observation. On the night of September 27, 2008, LAMOST observed more than 1000 spectra at one time, breaking the "world record" of 640 spectra held by the SDSS project, LAMOST has officially become the world's highest acquisition rate of celestial spectra Astronomical telescope 。 At most 4000 celestial spectra can be taken at one time. Its completion has made China a world leader in large-scale astronomical spectral observation and research Astrophysics Significant scientific research achievements in many research fields have laid the foundation. In order to give full play to LAMOST's power and obtain the greatest scientific returns, astronomers have developed a series of observation plans and designed three core research topics for the telescope in combination with its functions and characteristics.

The first celestial spectrum obtained by LAMOST telescope

Task 1

The first is to study the universe and galaxies. One is Galaxy redshift The other is to further study the physical properties of galaxies through the obtained data. Galaxy physics is a hot topic in the international astronomical community. The birth of the universe, the formation of galaxies, stars and Galaxy structure And other frontier problems are based on the study of galactic physics. Research Large scale structure of the universe Depends on the work of galaxy redshift survey. Get the spectrum of the galaxy, and you can get the red shift With redshift, you can know its distance, and with distance, you can know its three-dimensional distribution, so you can understand the whole Cosmic space Structure of. At the same time, we can study the large-scale structure of the universe and galactic physics, including the formation and evolution of galaxies. This is an interlocking project, and obtaining the spectra of galaxies is the most basic part.

Task 2

The second core topic is to study stars and Galaxy The structural characteristics of. Mainly aim at darker stars, and observe more, so that we can learn more about the distribution and movement of stars farther away from the Milky Way, and make clear Galaxy structure 。 Since LAMOST can sample a large number of stars, more and darker stars can be selected for large-scale research. Stars are an important part of many galaxies. Through the spectrum of a star, astronomers can analyze its physical conditions such as density and temperature, analyze its chemical composition such as element composition and content, and measure its movement speed and trajectory. By studying the distribution of different kinds of stars, we can study the structure and formation of the Milky Way.

Task 3

The third core topic of LAMOST is“ Multiband It is a common practice in the astronomical community to verify that radio , infrared X-ray 、 Gamma ray The discovered objects should be analyzed in the spectrum. Because the spectral theory is full and there are many experiences, the data about celestial bodies collected by other means should finally be confirmed by spectra. As the highest spectral acquisition rate Astronomical telescope ， LAMOST pair Optical astronomy It is self-evident that. Multi band identification itself is one of the three major topics of LAMOST. By combining with other band sky survey telescopes, such as X-rays and telescopes, it can play a considerable role in solving many frontiers of astronomy.

Chronicle of Events

Announce

edit

1990s

In April 1993 Wang Shouguan 、 Su Dingqiang The research group led by LAMOST proposed the LAMOST project as a major astronomical observation equipment in China.

From December 1994 to June 1995 Chinese Astronomical Society 、 Chinese Academy of Sciences LAMOST project has always been in the forefront of many evaluations and reviews organized by the Ministry of Mathematics and Physics, the Chinese Academy of Sciences, the National Science and Technology Commission and the National Planning Commission.

In July 1996, the National Science and Technology Leading Group decided to launch the National Major Science and Technology Project Plan, LAMOST was listed in the first batch of startup projects.

In October 1996, the Chinese Academy of Sciences established the National Major Science Project“ Large sky area multi-target optical fiber spectroscopic telescope ”Project Headquarters, Project Science and Technology Committee Project Management Committee. The project management committee is headed by Xu Zhihong, the vice president in charge. Su Hongjun is the general manager of the project headquarters, and Cui Xiangqun, Chu Yaoquan and Zhao Yongheng are members of the project headquarters. The director of the project science and technology committee is academician Wang Shouguan, and the members are academician Wang Daheng, academician Su Dingqiang, academician Chen Jiansheng, and academician Lei Tianjue.

In April 1997, the National Planning Commission approved the LAMOST Project Proposal.

In August 1997, the National Planning Commission approved the Feasibility Study Report of LAMOST Project.

In June 1999, the Chinese Academy of Sciences was entrusted by the National Development Planning Commission to approve the Preliminary Design and Estimate of LAMOST Project.

twenty-first century

In August 2001, the National Development Planning Commission approved the commencement report of LAMOST project, and the project officially entered the construction phase.

In June 2004, LAMOST observation building is under construction at Xinglong Observation Station of the National Astronomical Observatory.

In December 2004, the key technology pre research project -“ Large aperture active optical experimental telescope ”Pass acceptance and appraisal.

In June 2005, the Chinese Academy of Sciences organized internationally renowned experts to conduct a mid-term evaluation of the LAMOST project.

In September 2005, The first large equipment (8m rack base) of LAMOST project was successfully hoisted at Xinglong Observation Station, and the installation of main equipment of the project began.

In December 2005, the reflection was successfully completed at Xinglong Observatory of the National Astronomical Observatory Schmidt corrector The installation of three major assemblies (MA) frame, focal plane mechanism and spherical master mirror (MB) truss has fully entered the field installation and commissioning.

In June 2007, LAMOST completes a 3m diameter mirror, 250 optical fiber positioning system, 1 set a spectrometer And 2 sets CCD camera (referred to as "small system"), as well as the installation and adjustment of the complete telescope horizon frame, focal plane frame, tracking and control system, to achieve the optical indicators of the telescope design, and obtain the celestial spectrum.

In August 2008, all hardware of the telescope (24 Ma sub mirrors, 37 Mb sub mirrors, 4000 optical fiber positioning units, 4000 optical fibers, 16 spectrometers, 32 CCD cameras) was installed in place.

In October 2008, The inauguration ceremony of LAMOST was held at the Xinglong Observation Base of the National Astronomical Observatory.

On June 4, 2009, LAMOST successfully passed the national acceptance.

On April 17, 2010, LAMOST is named“ Guo Shoujing Telescope ".

In August 2018 National Astronomical Observatory, Chinese Academy of Sciences The scientific research team led by the team found a strange celestial body relying on the large scientific device LAMOST. Its lithium content is about 3000 times that of similar celestial bodies, and it is the star with the highest lithium content known to mankind. The international academic journal Nature Astronomy published this scientific discovery online on the 7th^[1] 。

In the early morning of November 28, 2019, National Astronomical Observatory, Chinese Academy of Sciences The research team of Liu Jifeng and Zhang Haotong, relying on China's self-developed LAMOST, a major national science and technology infrastructure, has discovered the largest Stellar black hole And provides a way to search for black hole New method of^[2] 。

On May 24, 2021, the research team of the National Astronomical Observatory of the Chinese Academy of Sciences screened 209 type O stars from LAMOST (Guo Shoujing Telescope) spectral data, 135 of which were newly discovered. This is the research work that has discovered the largest number of O stars in the Milky Way at one time by using a single spectral database so far. Before that, the largest O star list of the Milky Way with spectral information had only 590 O stars. This achievement was recently published in the international academic journal Astrophysical Journal Supplement.^[3]

In August 2021, based on the observation data of LAMOST, researchers found a very rare new type of cataclysmic variable star. This rare type of cataclysmic variable successfully captured by Guo Shoujing's telescope confirmed the existence of this transitional type of cataclysmic variable; At the same time, it provides substantial evidence for further understanding the formation and evolution history of cataclysmic variable stars. Relevant research results were published online in the international academic journal Monthly Journal of the Royal Astronomical Society.^[4]

In April 2022, based on the seventh batch of low resolution spectral data released by Guo Shoujing's telescope, Chinese researchers found 734 extremely cold dwarfs, all of which are candidates for brown dwarfs. Relevant research results were published in the journal Astronomy and Astrophysics.^[6]

In July 2022, the Astrophysical Journal Express recently published an important research result on super lithium rich dwarfs. Based on the medium resolution spectral data of Guo Shoujing Telescope (LAMOST), Chinese astronomers found nine unexvoluted stars with very high lithium content at one time, namely super lithium rich dwarfs. One of the super lithium rich dwarfs has a lithium content 31 times that of the sun, breaking the record for such stars.^[7]

In March 2023, Peking University and the National Astronomical Observatory of the Chinese Academy of Sciences cooperated to use LAMOST (Guo Shoujing Telescope) spectral data and the photometric data of the Nanshan Optical Telescope of the Xinjiang Astronomical Observatory to discover a binary star system composed of a compact star with a mass of about 0.98 times the solar mass and a late main sequence star.^[9]

On March 31, 2023, the National Astronomical Observatory of the Chinese Academy of Sciences released the data set DR10 (v1.0 version) of Guo Shoujing Telescope (LAMOST), a major national science and technology infrastructure, to domestic astronomers and international collaborators. The data set contains more than 22.29 million spectra, 2.9 times the sum of the spectra published by other international sky survey telescopes 。^[10]

April 2023 news, based on China's Guo Shoujing Telescope and the United States Apache Observatory According to the observation data of the Galaxy Evolution Experiment (APOGEE) sky survey, the research team of Huang Yang, an associate professor of the University of Chinese Academy of Sciences, used machine learning methods to obtain the most accurate rotation curve of the Milky Way within the range of 16000 light-years to 81000 light-years from the center of the Milky Way, and based on the rotation curve, the mass of the Milky Way was estimated to be about 805 billion solar masses. Relevant research results were published online in the Journal of Astrophysics.^[12]

significance

Announce

edit

LAMOST is an innovative design in China, which is very challenging in technology Large optical telescope It is a national major scientific project that is expected to obtain world famous scientific achievements. It is also the largest caliber in China Infrared telescope 。

LAMOST also created a new type of telescope, LAMOST type Schmidt telescope , broke the big field The telescope cannot have the bottleneck of large aperture at the same time. It is internationally known as "the best solution for building a large aperture telescope with high efficiency on the ground".

LAMOST project has attracted extensive attention of astronomers at home and abroad LAMOST Great scientific potential is expected. United States《 Science 》The magazine has published articles twice. The famous astronomical science magazine Sky&Telescope mentioned in the 7th issue of 2000:

"The telescope related to spectrum is LAMOST, an unusual telescope in China, which will be built near the Great Wall in northern China Beijing Astronomical Observatory Xinglong Station. LAMOST with 30 million dollars has a fixed 4m Primary mirror And 5 degrees field A deformable mirror guides the starlight to the fixed primary mirror. When LAMOST is completed, it will be the most productive spectral survey tool so far: using optical fiber, automatic optical fiber positioning device and 20 sets a spectrometer Each time, the spectrum of 4000 celestial bodies will be obtained. "

At the turn of spring and summer in 2005, the Chinese Academy of Sciences and LAMOST The headquarters invited many internationally renowned astronomical instrument experts and astronomers to evaluate the functions and potential scientific significance of LAMOST telescope. These include Paloma Observatory Former director of Keck Observatory, USA Yerkes Observatory Front director, SDSS project leader, 2dF project leader. After careful on-site investigation and in-depth exchanges with project members, these international giants believe that LAMOST will be a world-class sky survey equipment suitable for studying major astrophysical problems in a wide range of fields. In view of its light collection area and number of optical fibers, The potential function of LAMOST will be 10-15 times higher than SDSS digital sky survey and 2dF. If such a high target can be reached, it will be a huge leap and open a wide 'exploration space'. LAMOST will have a very good scientific output and will be able to Extragalactic astronomy And the astronomy of the Milky Way. "

LAMOST's unique design idea also has a great impact on the international Astronomical telescope The design of has had an important impact. In early June 2005, some foreign astronomers proposed to build a large caliber LAMOST telescope in the Antarctic. The LAMOST telescope of the National Astronomical Observatory echoes the LAMOST telescope in the Antarctic from the south to the north, and makes complete depth spectral observations of the entire sky.

With the completion of LAMOST, many international research projects and astronomers have shown great interest and enthusiasm in it, hoping to participate in LAMOST's Celestial survey And scientific research. This includes SDSS in the United States, GAIA in Europe, University of Cambridge Astronomers and so on.

There were too many events around the Chinese people in 2008, but for Chinese astronomers and friends who care about astronomy, The completion of LAMOST will undoubtedly be an exciting achievement for many years.

On March 31, 2023, the National Astronomical Observatory of the Chinese Academy of Sciences released the data set of Guo Shoujing Telescope (LAMOST) DR10 (v1.0 version). This data set contains more than 22.29 million spectral data, 2.9 times the sum of the spectra published by other astronomical survey telescopes in the world. LAMOST became the first sky survey project in the world to release more than 20 million spectra.^[11]

The international team led by researcher Zhao Gang of the National Astronomical Observatory of the Chinese Academy of Sciences took the lead in discovering the pair instability supernova formed by the collapse of the first generation of super massive stars after evolution in the Milky Way, PISN). Before that, theoretical studies had predicted the existence of this special supernova, but it was never observed. This achievement confirmed that this supernova originated from a first generation star with a mass up to 260 times the mass of the sun, refreshing people's understanding of the mass distribution of the first generation stars. At 17:00 on June 7, 2023, the international academic journal Nature published this important research achievement online.^[13]

In February 2024, Chinese astronomers calculated that the mass of Andromeda Galaxy (M31) is about 1.14 trillion times of the sun, using the spectral data of LAMOST and the existing observation results of Andromeda Galaxy (M31) Quality.^[14]

Novice on the road

Growth task Getting Started with Editing Edit Rule Edit by myself

I have questions

Content query Online Service Official post bar Feedback

Complaints and suggestions

Report bad information Failed to appeal through entries Complaint of infringement information Blocking query and unblocking

Jinggong Network Anbei No. 1100000200001