In order to achieve the optimized design of a cased telescoped ammunition(CTA) interior ballistic design,a genetic algorithm was introduced into the optimal design of CTA interior ballistics with coupling the CTA inte...In order to achieve the optimized design of a cased telescoped ammunition(CTA) interior ballistic design,a genetic algorithm was introduced into the optimal design of CTA interior ballistics with coupling the CTA interior ballistic model. Aiming at the interior ballistic characteristics of a CTA gun, the goal of CTA interior ballistic design is to obtain a projectile velocity as large as possible. The optimal design of CTA interior ballistic is carried out using a genetic algorithm by setting peak pressure, changing the chamber volume and gun powder charge density. A numerical simulation of interior ballistics based on a 35 mm CTA firing experimental scheme was conducted and then the genetic algorithm was used for numerical optimization. The projectile muzzle velocity of the optimized scheme is increased from 1168 m/s for the initial experimental scheme to 1182 m/s. Then four optimization schemes were obtained with several independent optimization processes. The schemes were compared with each other and the difference between these schemes is small. The peak pressure and muzzle velocity of these schemes are almost the same. The result shows that the genetic algorithm is effective in the optimal design of the CTA interior ballistics. This work will be lay the foundation for further CTA interior ballistic design.展开更多
The Si Tian project,designed to utilize 60 telescopes distributed across multiple sites in China,is a next-generation timedomain survey initiative.As a pathfinder for the Si Tian project,the Mini-Si Tian(MST)has been ...The Si Tian project,designed to utilize 60 telescopes distributed across multiple sites in China,is a next-generation timedomain survey initiative.As a pathfinder for the Si Tian project,the Mini-Si Tian(MST)has been proposed and implemented to test the Si Tian’s brain and data pipeline,and to evaluate the feasibility of its technology and science cases.Mounted at the Xinglong Observatory,the MST project comprises three 30 cm telescopes and has been operated since 2022 November.Each telescope of the MST possesses a large field of view,covering 2°.29×1°.53 FOV,and is equipped withg',r'andi'filters,respectively.Acting as the pioneer of the forthcoming Si Tian project,the MST is dedicated to the discovery of variable stars,transients,and outburst events,and has already obtained some interesting scientific results.In this paper,we will summarize the first-two-year operation of the MST project.展开更多
This paper outlines the scientific goals and observational strategies of the Mini-SiTian Array.Mounted at Xinglong Observatory,the Mini-SiTian Array consists of three 30 cm telescopes and has been in operation since 2...This paper outlines the scientific goals and observational strategies of the Mini-SiTian Array.Mounted at Xinglong Observatory,the Mini-SiTian Array consists of three 30 cm telescopes and has been in operation since 2022.The large field of view,combined with the capability for multi-band photometric observations,enables the Mini-SiTian Array to perform rapid follow-up observations to identify optical counterparts of gravitational waves,capture the early light curves of tidal disruption events and supernovae,and monitor stellar flares,Be star outbursts,and cataclysmic variable stars,although its limiting magnitude is not very deep.By collaborating with the Xinglong2.16 m telescope and leveraging a real-time image processing pipeline,simultaneous photometric and spectroscopic observations could be performed to reveal their underlying physical mechanisms.The observational and research experience provides critical guidance for the implementation of the full-scale SiTian project in the future.展开更多
To realize effective co-phasing adjustment in large-aperture sparse-aperture telescopes,a multichannel stripe tracking approach is employed,allowing simultaneous interferometric measurements of multiple optical paths ...To realize effective co-phasing adjustment in large-aperture sparse-aperture telescopes,a multichannel stripe tracking approach is employed,allowing simultaneous interferometric measurements of multiple optical paths and circumventing the need for pairwise measurements along the mirror boundaries in traditional interferometric methods.This approach enhances detection efficiency and reduces system complexity.Here,the principles of the multibeam interference process and construction of a co-phasing detection module based on direct optical fiber connections were analyzed using wavefront optics theory.Error analysis was conducted on the system surface obtained through multipath interference.Potential applications of the interferometric method were explored.Finally,the principle was verified by experiment,an interferometric fringe contrast better than 0.4 is achieved through flat field calibration and incoherent digital synthesis.The dynamic range of the measurement exceeds 10 times of the center wavelength of the working band(1550 nm).Moreover,a resolution better than one-tenth of the working center wavelength(1550 nm)was achieved.Simultaneous three-beam interference can be achieved,leading to a 50%improvement in detection efficiency.This method can effectively enhance the efficiency of sparse aperture telescope co-phasing,meeting the requirements for observations of 8-10 m telescopes.This study provides a technological foundation for observing distant and faint celestial objects.展开更多
For segmented detectors,surface flatness is critical as it directly influences both energy resolution and image clarity.Additionally,the limited adjustment range of the segmented detectors necessitates precise benchma...For segmented detectors,surface flatness is critical as it directly influences both energy resolution and image clarity.Additionally,the limited adjustment range of the segmented detectors necessitates precise benchmark construction.This paper proposes an architecture for detecting detector flatness based on channel spectral dispersion.By measuring the dispersion fringes for coplanar adjustment,the final adjustment residual is improved to better than 300 nm.This result validates the feasibility of the proposed technology and provides significant technical support for the development of next-generation large-aperture sky survey equipment.展开更多
The FAST radio telescope has significantly better sensitivity than any other current radio telescope.Consequently,FAST has discovered over a thousand new pulsars in sky regions already searched for 50 yr.The Galactic ...The FAST radio telescope has significantly better sensitivity than any other current radio telescope.Consequently,FAST has discovered over a thousand new pulsars in sky regions already searched for 50 yr.The Galactic Plane Pulsar Snapshot(GPPS)survey found three-quarters of these new pulsars.The article by Han et al.(2025)details the latest batch of 473 discoveries,bringing the total to 751.展开更多
Earth-based deep space radar studies celestial bodies by both transmitting and receiving radio waves,whereas radio telescopes only work passively.On the operational level,radar missions use only short observation time...Earth-based deep space radar studies celestial bodies by both transmitting and receiving radio waves,whereas radio telescopes only work passively.On the operational level,radar missions use only short observation times,which leaves a large portion of the time available for astronomical observations.However,the design principles used for radar and radio telescopes differ.Technical challenges are involved in making the instruments required to meet the requirements of these two applications simultaneously.In this study,we have attempted to tune a deep space radar system for use in radio astronomical applications and conducted a successful pulsar observation,thus demonstrating the feasibility of using radar systems,particularly distributed deep space radar,to perform astronomical research.Additionally,given the limited astronomical capacity available within the observed frequency range,this system has the potential to contribute to the long-term monitoring of specific radio sources.This work represents the first successful attempt to use an Earth-based deep space radar system to perform radio astronomy in China.We also discuss the challenges of tuning a built radar system for astronomical observation applications and propose recommendations for the design of future large-scale distributed deep space radar systems with innate astronomical capabilities.展开更多
This paper presents a comprehensive analysis of the photometric system of the University of Chinese Academy of Sciences 70 cm Telescope located at the Yan-qi Lake campus of the University of Chinese Academy of Science...This paper presents a comprehensive analysis of the photometric system of the University of Chinese Academy of Sciences 70 cm Telescope located at the Yan-qi Lake campus of the University of Chinese Academy of Sciences.We evaluated the linearity,bias stability,and dark current of the camera.Utilizing the Johnson-Cousins Blue-Visible-Red-Infrared filter system and an Andor DZ936 charge-coupled device camera,we conducted extensive observations of Landolt standard stars to determine the color terms,atmospheric extinction coefficients,photometric zero-points,and the sky background brightness.The results indicate that this telescope demonstrates excellent performance in photometric calibration and good system performance overall,meeting the requirements for limited scientific research and teaching purposes.展开更多
Antarctic telescopes,especially those located at Dome A,face significant reliability challenges owing to the extremely harsh working environment,among which the reliability of the control system is critical in ensurin...Antarctic telescopes,especially those located at Dome A,face significant reliability challenges owing to the extremely harsh working environment,among which the reliability of the control system is critical in ensuring stable operation.This paper describes various factors affecting the reliability of Antarctic telescopes,as well as the challenges of reliability improvement.Combined with the development of Antarctic telescopes and the experience of Antarctic scientific expeditions,we introduce,in detail,the optimization strategy for reliability enhancement,including the hardware layer,software layer,modular design to facilitate maintenance,and reliability management.The current status of the Antarctic Survey Telescope(AST3)is also briefly introduced,along with future development plans.We aim to provide ideas for the reliability design of Antarctic telescopes and provide technical support for the development of future Antarctic telescopes.展开更多
Adaptive optics(AO)has significantly advanced high-resolution solar observations by mitigating atmospheric turbulence.However,traditional post-focal AO systems suffer from external configurations that introduce excess...Adaptive optics(AO)has significantly advanced high-resolution solar observations by mitigating atmospheric turbulence.However,traditional post-focal AO systems suffer from external configurations that introduce excessive optical surfaces,reduced light throughput,and instrumental polarization.To address these limitations,we propose an embedded solar adaptive optics telescope(ESAOT)that intrinsically incorporates the solar AO(SAO)subsystem within the telescope's optical train,featuring a co-designed correction chain with a single Hartmann-Shack full-wavefront sensor(HS f-WFS)and a deformable secondary mirror(DSM).The HS f-WFS uses temporal-spatial hybrid sampling technique to simultane-ously resolve tip-tilt and high-order aberrations,while the DSM performs real-time compensation through adaptive modal optimization.This unified architecture achieves symmetrical polarization suppression and high system throughput by min-imizing optical surfaces.A 600 mm ESAOT prototype incorporating a 12×12 micro-lens array HS f-WFS and 61-actuator piezoelectric DSM has been developed and successfully conducted on-sky photospheric observations.Validations in-cluding turbulence simulations,optical bench testing,and practical observations at the Lijiang observatory collectively confirm the system's capability to maintain aboutλ/10 wavefront error during active region tracking.This architectural breakthrough of the ESAOT addresses long-standing SAO integration challenges in solar astronomy and provides scala-bility analyses confirming direct applicability to the existing and future large solar observation facilities.展开更多
In order to improve the deep learning training efficiency of the large reflector antenna active adjustment technique,this paper synthesizes the characteristic that each actuator can only adjust the panel connected to ...In order to improve the deep learning training efficiency of the large reflector antenna active adjustment technique,this paper synthesizes the characteristic that each actuator can only adjust the panel connected to it,and proposes a divided-ring antenna active adjustment deep learning training modeling method.The method organizes panel node data according to actuator ring positions,using panel displacements as input features and actuator adjustments as output labels.Through systematic sorting,reorganization,and normalization,the ring-divided data are transformed into grid-structured tensors suitable for convolutional processing.Multi-layer convolutional neural networks are then constructed for surface adjustment prediction,optimized through a hybrid strategy combining simulated annealing and the Adam algorithm.Through the dataset divided-ring preprocessing,active adjustment neural network construction and model training for the case of an 8 m reflector antenna,the analytical results show that the proposed method can effectively shorten the training time,and the final model's prediction accuracy is greatly improved,which demonstrates the feasibility and effectiveness of the proposed method.展开更多
Scientists have been searching for possible new particles beyond the standard model(SM),the theory that has predicted the building bricks that have constituted the known matter world today,including the Higgs-“the l...Scientists have been searching for possible new particles beyond the standard model(SM),the theory that has predicted the building bricks that have constituted the known matter world today,including the Higgs-“the last”SM particle.展开更多
Sulfur-bearing species are widely utilized to investigate the physical structure of star-forming regions in interstellar media;however,the underlying sulfur chemistry in these environments remains poorly understood.Th...Sulfur-bearing species are widely utilized to investigate the physical structure of star-forming regions in interstellar media;however,the underlying sulfur chemistry in these environments remains poorly understood.Therefore,further studies of S-bearing species are fundamentally important,as they can enhance our understanding of the physical evolution of star-forming regions.This study presents observations of C_(2)S and C_(3)S in L1544,acquired using the Nanshan 26-m radio telescope,along with simulations of their chemical behavior using a one-dimensional physical model.The simulation results reveal significant radial variations in the column densities of C_(2)S and C_(3)S.Additionally,the column densities of both molecules are found to be sensitive to the cosmic ray ionization rate at several radial positions,while variations in the C/O ratio have comparatively minimal impact on L1544.展开更多
To further improve the pointing accuracy of altazimuth telescopes,this study takes the NAOC 2.5 m telescope as the research object and develops a comprehensive pointing model.The paper rst analyzes the causes of error...To further improve the pointing accuracy of altazimuth telescopes,this study takes the NAOC 2.5 m telescope as the research object and develops a comprehensive pointing model.The paper rst analyzes the causes of errors and accordingly constructs three core models:the basic parametric model,the spherical harmonic model,and the polynomial regression model.Among them,the basic parametric model aims to t error terms with clear physical meanings,but its correction capability is limited and cannot fully cover all in uencing factors.To address this limitation,a spherical harmonic model is introduced.This model demonstrates excellent performance in handling higher-order error terms and can accurately t errors across the celestial sphere.Additionally,a polynomial regression model is designed to improve the tting capability and prediction accuracy for nonlinear errors by exibly adjusting the polynomial order.The resulting comprehensive pointing model combines the advantages of these three models,enabling more precise and complete correction of pointing errors while balancing computational complexity and accuracy by adjusting the tting weight of each model.Experimental veri cation shows that the telescope’s pointing accuracy is improved from 17".805 to 3".1029,meeting the requirements for high-precision astronomical observations.展开更多
The Ground-based Wide-Angle Cameras array necessitates the integration of more than 100 hardware devices,100 servers,and 2500 software modules that must be synchronized within a 3-second imaging cycle.However,the comp...The Ground-based Wide-Angle Cameras array necessitates the integration of more than 100 hardware devices,100 servers,and 2500 software modules that must be synchronized within a 3-second imaging cycle.However,the complexity of real-time,high-concurrency processing of large datasets has historically resulted in substantial failure rates,with an observation efficiency estimated at less than 50%in 2023.To mitigate these challenges,we developed a monitoring system designed to improve fault diagnosis efficiency.It includes two innovative monitoring views for“state evolution”and“transient lifecycle”.Combining these with“instantaneous state”and“key parameter”monitoring views,the system represents a comprehensive monitoring strategy.Here we detail the system architecture,data collection methods,and design philosophy of the monitoring views.During one year of fault diagnosis experimental practice,the proposed system demonstrated its ability to identify and localize faults within minutes,achieving fault localization nearly ten times faster than traditional methods.Additionally,the system design exhibited high generalizability,with possible applicability to other telescope array systems.展开更多
The Mini-SiTian project,which is a pathfinder for the SiTian project,utilizes three 30 cm telescopes equipped with commercial CMOS cameras(ZWO ASI6200MM Pro)to simulate a large-area time-domain survey.Due to the avoid...The Mini-SiTian project,which is a pathfinder for the SiTian project,utilizes three 30 cm telescopes equipped with commercial CMOS cameras(ZWO ASI6200MM Pro)to simulate a large-area time-domain survey.Due to the avoidance of the traditional mechanical shutter,the CMOS camera is favorable in time-domain survey projects.In the future,the SiTian telescope array will employ a two-by-two scientific-grade mosaic CMOS camera to survey a10,000 degree square area every 30 minutes.Therefore,the performance of CMOS directly determines the detection capability of SiTian telescopes for transient sources,and a comprehensive understanding of the performance of CMOS cameras is crucial.In this research,laboratory testing was conducted to thoroughly evaluate three cameras by assessing several critical parameters,including bias stability,dark current,pixel anomalies,linearity,gain,and read noise.We find exceptional short-term bias stability with standard deviations below 0.02 ADU,negligible dark current of approximately 0.002 e-pixel^(-1)s^(-1)at 0℃,and excellent linearity with nonlinearity consistently below±0.5%,and a small proportion(0.06%-0.08%)of pixels with anomalous responses.Furthermore,our analysis demonstrates uniform gain values across all cameras,ranging from 0.252 to 0.255 e-ADU^(-1),with low readout noise,measured to be below 1.6 e-using conventional methods.We also propose a novel method for pixel-level gain and read noise calculation for CMOS sensors,which revealed a narrow gain distribution and a low median read noise of 1.028 e-for one of the cameras.The laboratory testing of the ZWO ASI6200MM Pro cameras indicates their potential to meet the requirements of time-domain surveys for the Mini-SiTian project.展开更多
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
We developed a dedicated data analysis framework for silicon strip detector telescopes(SSDTs)of the Compact Spectrometer for Heavy-IoN Experiments(CSHINE)that addresses the challenges of processing complex signals.The...We developed a dedicated data analysis framework for silicon strip detector telescopes(SSDTs)of the Compact Spectrometer for Heavy-IoN Experiments(CSHINE)that addresses the challenges of processing complex signals.The framework integrates advanced algorithms for precise calibration,accurate particle identification,and efficient event reconstruction,aiming to account for critical experimental factors such as charge-sharing effects,multi-hit event resolution,and detector response nonuniformity.Its robust performance was demonstrated through the successful analysis of light-charged particles in the 25 MeV/u^(86)Kr+^(124)Sn experiment conducted at the first Radioactive Ion Beam Line in Lanzhou,allowing for precise extraction of physical observables,including energy,momentum,and particle type.Furthermore,utilizing the reconstructed physical information,such as the number of effective physical events and energy spectra to optimize the track recognition algorithm,the final track recognition efficiencies of approximately 90%were achieved.This framework establishes a valuable reference methodology for SSDT-based detector systems in heavy-ion reaction experiments,thereby significantly enhancing the accuracy and efficiency of data analysis in nuclear physics research.展开更多
A bicuspid aortic valve,from autologous tissue,with growth potential can be constructed using the simple,and reproducible telescoping arterial trunk technique.
Effective motors are crucial for driving astronomical telescopes,especially for those operating in Antarctica,where the harsh environment and operating conditions,including extreme low temperature,ice/snow accumulatio...Effective motors are crucial for driving astronomical telescopes,especially for those operating in Antarctica,where the harsh environment and operating conditions,including extreme low temperature,ice/snow accumulation,low power consumption,and unattended operation,introduce challenges to the design and development of motor drives.We present the design of a permanent magnet synchronous motor suitable for this environment,conducting a quantitative analysis on the impacts of cryogenic conditions on lubricant performance,differential thermal contraction of metallic components,and remanent flux density of neodymium iron boron(N52)permanent magnets.We also implement a labyrinth seal structure,combined with silicone sealing rings,to mitigate ice crystal intrusion risks.Finite element analysis and laboratory tests demonstrate a maximum torque output of 25 Nm.This kind of motor is used in the Antarctic 15 cm Near Infrared Telescope at Dome A,Antarctica.Operation data shows a total encoder feedback error of 0.0678"for the telescope control system with 15"s^(−1)tracking speed at−56.79°C.These results comprehensively validate the high reliability and precision of the motor under the extreme conditions of the polar environment.展开更多
文摘In order to achieve the optimized design of a cased telescoped ammunition(CTA) interior ballistic design,a genetic algorithm was introduced into the optimal design of CTA interior ballistics with coupling the CTA interior ballistic model. Aiming at the interior ballistic characteristics of a CTA gun, the goal of CTA interior ballistic design is to obtain a projectile velocity as large as possible. The optimal design of CTA interior ballistic is carried out using a genetic algorithm by setting peak pressure, changing the chamber volume and gun powder charge density. A numerical simulation of interior ballistics based on a 35 mm CTA firing experimental scheme was conducted and then the genetic algorithm was used for numerical optimization. The projectile muzzle velocity of the optimized scheme is increased from 1168 m/s for the initial experimental scheme to 1182 m/s. Then four optimization schemes were obtained with several independent optimization processes. The schemes were compared with each other and the difference between these schemes is small. The peak pressure and muzzle velocity of these schemes are almost the same. The result shows that the genetic algorithm is effective in the optimal design of the CTA interior ballistics. This work will be lay the foundation for further CTA interior ballistic design.
基金supported by the National Key R&D Program of China(grant No.2023YFA1608304 and No.2023YFA1608300)the Strategic Priority Research Program of the Chinese Academy of Sciences(XDB0550100 and XDB0550000)the National Natural Science Foundation of China(NSFC,grant Nos.12090041,12090040,11903054,12422303,and 12261141690)。
文摘The Si Tian project,designed to utilize 60 telescopes distributed across multiple sites in China,is a next-generation timedomain survey initiative.As a pathfinder for the Si Tian project,the Mini-Si Tian(MST)has been proposed and implemented to test the Si Tian’s brain and data pipeline,and to evaluate the feasibility of its technology and science cases.Mounted at the Xinglong Observatory,the MST project comprises three 30 cm telescopes and has been operated since 2022 November.Each telescope of the MST possesses a large field of view,covering 2°.29×1°.53 FOV,and is equipped withg',r'andi'filters,respectively.Acting as the pioneer of the forthcoming Si Tian project,the MST is dedicated to the discovery of variable stars,transients,and outburst events,and has already obtained some interesting scientific results.In this paper,we will summarize the first-two-year operation of the MST project.
基金supported by the National Key Basic R&D Program of China via 2023YFA1608303the Strategic Priority Research Program of the Chinese Academy of Sciences(XDB0550103)+3 种基金the Strategic Priority Research Program of Chinese Academy of Sciences(grant Nos.XDB0550000,XDB0550100 and XDB0550102)supported from the Strategic Pioneer Program of the Astronomy Large-Scale Scientific Facility,Chinese Academy of Sciences and the Science and Education Integration Funding of University of Chinese Academy of Sciencessupported by the National Natural Science Foundation of China(NSFCgrant Nos.12090040,12090041,12090041,12422303,12261141690,and 12403022)。
文摘This paper outlines the scientific goals and observational strategies of the Mini-SiTian Array.Mounted at Xinglong Observatory,the Mini-SiTian Array consists of three 30 cm telescopes and has been in operation since 2022.The large field of view,combined with the capability for multi-band photometric observations,enables the Mini-SiTian Array to perform rapid follow-up observations to identify optical counterparts of gravitational waves,capture the early light curves of tidal disruption events and supernovae,and monitor stellar flares,Be star outbursts,and cataclysmic variable stars,although its limiting magnitude is not very deep.By collaborating with the Xinglong2.16 m telescope and leveraging a real-time image processing pipeline,simultaneous photometric and spectroscopic observations could be performed to reveal their underlying physical mechanisms.The observational and research experience provides critical guidance for the implementation of the full-scale SiTian project in the future.
文摘To realize effective co-phasing adjustment in large-aperture sparse-aperture telescopes,a multichannel stripe tracking approach is employed,allowing simultaneous interferometric measurements of multiple optical paths and circumventing the need for pairwise measurements along the mirror boundaries in traditional interferometric methods.This approach enhances detection efficiency and reduces system complexity.Here,the principles of the multibeam interference process and construction of a co-phasing detection module based on direct optical fiber connections were analyzed using wavefront optics theory.Error analysis was conducted on the system surface obtained through multipath interference.Potential applications of the interferometric method were explored.Finally,the principle was verified by experiment,an interferometric fringe contrast better than 0.4 is achieved through flat field calibration and incoherent digital synthesis.The dynamic range of the measurement exceeds 10 times of the center wavelength of the working band(1550 nm).Moreover,a resolution better than one-tenth of the working center wavelength(1550 nm)was achieved.Simultaneous three-beam interference can be achieved,leading to a 50%improvement in detection efficiency.This method can effectively enhance the efficiency of sparse aperture telescope co-phasing,meeting the requirements for observations of 8-10 m telescopes.This study provides a technological foundation for observing distant and faint celestial objects.
文摘For segmented detectors,surface flatness is critical as it directly influences both energy resolution and image clarity.Additionally,the limited adjustment range of the segmented detectors necessitates precise benchmark construction.This paper proposes an architecture for detecting detector flatness based on channel spectral dispersion.By measuring the dispersion fringes for coplanar adjustment,the final adjustment residual is improved to better than 300 nm.This result validates the feasibility of the proposed technology and provides significant technical support for the development of next-generation large-aperture sky survey equipment.
文摘The FAST radio telescope has significantly better sensitivity than any other current radio telescope.Consequently,FAST has discovered over a thousand new pulsars in sky regions already searched for 50 yr.The Galactic Plane Pulsar Snapshot(GPPS)survey found three-quarters of these new pulsars.The article by Han et al.(2025)details the latest batch of 473 discoveries,bringing the total to 751.
基金supported by the China Postdoctoral Science Foundation(2024M754113)the Chongqing Postdoctoral Innovative Fund(CQBX202419)the Natural Science Foundation of Chongqing(CSTB2023NSCOMSX0629).
文摘Earth-based deep space radar studies celestial bodies by both transmitting and receiving radio waves,whereas radio telescopes only work passively.On the operational level,radar missions use only short observation times,which leaves a large portion of the time available for astronomical observations.However,the design principles used for radar and radio telescopes differ.Technical challenges are involved in making the instruments required to meet the requirements of these two applications simultaneously.In this study,we have attempted to tune a deep space radar system for use in radio astronomical applications and conducted a successful pulsar observation,thus demonstrating the feasibility of using radar systems,particularly distributed deep space radar,to perform astronomical research.Additionally,given the limited astronomical capacity available within the observed frequency range,this system has the potential to contribute to the long-term monitoring of specific radio sources.This work represents the first successful attempt to use an Earth-based deep space radar system to perform radio astronomy in China.We also discuss the challenges of tuning a built radar system for astronomical observation applications and propose recommendations for the design of future large-scale distributed deep space radar systems with innate astronomical capabilities.
基金supported by National Key R&D Program of China(2023YFA1609700)Research and Education Integration Funding。
文摘This paper presents a comprehensive analysis of the photometric system of the University of Chinese Academy of Sciences 70 cm Telescope located at the Yan-qi Lake campus of the University of Chinese Academy of Sciences.We evaluated the linearity,bias stability,and dark current of the camera.Utilizing the Johnson-Cousins Blue-Visible-Red-Infrared filter system and an Andor DZ936 charge-coupled device camera,we conducted extensive observations of Landolt standard stars to determine the color terms,atmospheric extinction coefficients,photometric zero-points,and the sky background brightness.The results indicate that this telescope demonstrates excellent performance in photometric calibration and good system performance overall,meeting the requirements for limited scientific research and teaching purposes.
基金supported by the National Natural Science Foundation of China (12303089, 11973065)the Jiangsu Funding Program for Excellent Postdoctoral Talent (2022ZB449)the Polar Research Institute of China (PRIC) for their support and help with the Antarctic telescope project
文摘Antarctic telescopes,especially those located at Dome A,face significant reliability challenges owing to the extremely harsh working environment,among which the reliability of the control system is critical in ensuring stable operation.This paper describes various factors affecting the reliability of Antarctic telescopes,as well as the challenges of reliability improvement.Combined with the development of Antarctic telescopes and the experience of Antarctic scientific expeditions,we introduce,in detail,the optimization strategy for reliability enhancement,including the hardware layer,software layer,modular design to facilitate maintenance,and reliability management.The current status of the Antarctic Survey Telescope(AST3)is also briefly introduced,along with future development plans.We aim to provide ideas for the reliability design of Antarctic telescopes and provide technical support for the development of future Antarctic telescopes.
基金support from the National Science Foundation of China(NSFC)(Grants No.12293031 and No.61905252)the National Science Foundation for Distinguished Young Scholars(Grant No.12022308)the National Key R&D Program of China(Grants No.2021YFC2202200 and No.2021YFC2202204).
文摘Adaptive optics(AO)has significantly advanced high-resolution solar observations by mitigating atmospheric turbulence.However,traditional post-focal AO systems suffer from external configurations that introduce excessive optical surfaces,reduced light throughput,and instrumental polarization.To address these limitations,we propose an embedded solar adaptive optics telescope(ESAOT)that intrinsically incorporates the solar AO(SAO)subsystem within the telescope's optical train,featuring a co-designed correction chain with a single Hartmann-Shack full-wavefront sensor(HS f-WFS)and a deformable secondary mirror(DSM).The HS f-WFS uses temporal-spatial hybrid sampling technique to simultane-ously resolve tip-tilt and high-order aberrations,while the DSM performs real-time compensation through adaptive modal optimization.This unified architecture achieves symmetrical polarization suppression and high system throughput by min-imizing optical surfaces.A 600 mm ESAOT prototype incorporating a 12×12 micro-lens array HS f-WFS and 61-actuator piezoelectric DSM has been developed and successfully conducted on-sky photospheric observations.Validations in-cluding turbulence simulations,optical bench testing,and practical observations at the Lijiang observatory collectively confirm the system's capability to maintain aboutλ/10 wavefront error during active region tracking.This architectural breakthrough of the ESAOT addresses long-standing SAO integration challenges in solar astronomy and provides scala-bility analyses confirming direct applicability to the existing and future large solar observation facilities.
基金sponsored by the Tianshan Talent Foundation of Xinjiang Uygur Autonomous Region under No.2024TSYCCX0010the National Natural Science Foundation of China(12303094 and 52165053)+2 种基金the National Key R&D Program of China(No.2021YFC220350)the Natural Science Foundation of Xinjiang Uygur Autonomous Region(2022D01C683)the China Postdoctoral Science Foundation(2021M702751&2023T160549)。
文摘In order to improve the deep learning training efficiency of the large reflector antenna active adjustment technique,this paper synthesizes the characteristic that each actuator can only adjust the panel connected to it,and proposes a divided-ring antenna active adjustment deep learning training modeling method.The method organizes panel node data according to actuator ring positions,using panel displacements as input features and actuator adjustments as output labels.Through systematic sorting,reorganization,and normalization,the ring-divided data are transformed into grid-structured tensors suitable for convolutional processing.Multi-layer convolutional neural networks are then constructed for surface adjustment prediction,optimized through a hybrid strategy combining simulated annealing and the Adam algorithm.Through the dataset divided-ring preprocessing,active adjustment neural network construction and model training for the case of an 8 m reflector antenna,the analytical results show that the proposed method can effectively shorten the training time,and the final model's prediction accuracy is greatly improved,which demonstrates the feasibility and effectiveness of the proposed method.
文摘Scientists have been searching for possible new particles beyond the standard model(SM),the theory that has predicted the building bricks that have constituted the known matter world today,including the Higgs-“the last”SM particle.
基金the support from the Natural Science Foundation of Xinjiang Uygur Autonomous Region(Grant No.2024D01E37)the National Science Foundation of China(Grant No.12473025)+5 种基金funded by the National Natural Science Foundation of China(Grant Nos.12373026,12203091,12173075,and 11973076)the Xinjiang Tianchi Talent Program(2024)the support from the Xinjiang Tianchi Talent Program(2023)the Shanghai Natural Science Foundation(Grant No.22ZR1421400)the Natural Science Foundation of Xinjiang Uygur Autonomous Region(Grant No.2022D01A156)partially funded by the Regional Collaborative Innovation Project of Xin jiang Uyghur Autonomous Region(Grant No.2022E01050)。
文摘Sulfur-bearing species are widely utilized to investigate the physical structure of star-forming regions in interstellar media;however,the underlying sulfur chemistry in these environments remains poorly understood.Therefore,further studies of S-bearing species are fundamentally important,as they can enhance our understanding of the physical evolution of star-forming regions.This study presents observations of C_(2)S and C_(3)S in L1544,acquired using the Nanshan 26-m radio telescope,along with simulations of their chemical behavior using a one-dimensional physical model.The simulation results reveal significant radial variations in the column densities of C_(2)S and C_(3)S.Additionally,the column densities of both molecules are found to be sensitive to the cosmic ray ionization rate at several radial positions,while variations in the C/O ratio have comparatively minimal impact on L1544.
文摘To further improve the pointing accuracy of altazimuth telescopes,this study takes the NAOC 2.5 m telescope as the research object and develops a comprehensive pointing model.The paper rst analyzes the causes of errors and accordingly constructs three core models:the basic parametric model,the spherical harmonic model,and the polynomial regression model.Among them,the basic parametric model aims to t error terms with clear physical meanings,but its correction capability is limited and cannot fully cover all in uencing factors.To address this limitation,a spherical harmonic model is introduced.This model demonstrates excellent performance in handling higher-order error terms and can accurately t errors across the celestial sphere.Additionally,a polynomial regression model is designed to improve the tting capability and prediction accuracy for nonlinear errors by exibly adjusting the polynomial order.The resulting comprehensive pointing model combines the advantages of these three models,enabling more precise and complete correction of pointing errors while balancing computational complexity and accuracy by adjusting the tting weight of each model.Experimental veri cation shows that the telescope’s pointing accuracy is improved from 17".805 to 3".1029,meeting the requirements for high-precision astronomical observations.
基金supported by the Young Data Scientist Program of the China National Astronomical Data Center,the Strategic Priority Research Program of the Chinese Academy of Sciences(XDB0550401)the National Natural Science Foundation of China(12494573).
文摘The Ground-based Wide-Angle Cameras array necessitates the integration of more than 100 hardware devices,100 servers,and 2500 software modules that must be synchronized within a 3-second imaging cycle.However,the complexity of real-time,high-concurrency processing of large datasets has historically resulted in substantial failure rates,with an observation efficiency estimated at less than 50%in 2023.To mitigate these challenges,we developed a monitoring system designed to improve fault diagnosis efficiency.It includes two innovative monitoring views for“state evolution”and“transient lifecycle”.Combining these with“instantaneous state”and“key parameter”monitoring views,the system represents a comprehensive monitoring strategy.Here we detail the system architecture,data collection methods,and design philosophy of the monitoring views.During one year of fault diagnosis experimental practice,the proposed system demonstrated its ability to identify and localize faults within minutes,achieving fault localization nearly ten times faster than traditional methods.Additionally,the system design exhibited high generalizability,with possible applicability to other telescope array systems.
基金supported by the National Key R&D Program of China(grant Nos.2023YFA1609700,2023YFA1608304,and2023YFA1608303)the Strategic Priority Research Program of the Chinese Academy of Sciences(XDB0550103)+1 种基金the National Natural Science Foundation of China(NSFC,Nos.12090040 and 12090041)supported from the Strategic Pioneer Program of the Astronomy Large-Scale Scientific Facility,Chinese Academy of Sciences,and the Science and Education Integration Funding of the University of Chinese Academy of Sciences。
文摘The Mini-SiTian project,which is a pathfinder for the SiTian project,utilizes three 30 cm telescopes equipped with commercial CMOS cameras(ZWO ASI6200MM Pro)to simulate a large-area time-domain survey.Due to the avoidance of the traditional mechanical shutter,the CMOS camera is favorable in time-domain survey projects.In the future,the SiTian telescope array will employ a two-by-two scientific-grade mosaic CMOS camera to survey a10,000 degree square area every 30 minutes.Therefore,the performance of CMOS directly determines the detection capability of SiTian telescopes for transient sources,and a comprehensive understanding of the performance of CMOS cameras is crucial.In this research,laboratory testing was conducted to thoroughly evaluate three cameras by assessing several critical parameters,including bias stability,dark current,pixel anomalies,linearity,gain,and read noise.We find exceptional short-term bias stability with standard deviations below 0.02 ADU,negligible dark current of approximately 0.002 e-pixel^(-1)s^(-1)at 0℃,and excellent linearity with nonlinearity consistently below±0.5%,and a small proportion(0.06%-0.08%)of pixels with anomalous responses.Furthermore,our analysis demonstrates uniform gain values across all cameras,ranging from 0.252 to 0.255 e-ADU^(-1),with low readout noise,measured to be below 1.6 e-using conventional methods.We also propose a novel method for pixel-level gain and read noise calculation for CMOS sensors,which revealed a narrow gain distribution and a low median read noise of 1.028 e-for one of the cameras.The laboratory testing of the ZWO ASI6200MM Pro cameras indicates their potential to meet the requirements of time-domain surveys for the Mini-SiTian project.
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supported by the National Natural Science Foundation of China(NNSFC)(Nos.12375123,12205160,and 12335008)the Natural Science Foundation of Henan Province,China(No.242300421048)the postgraduate research and practice innovation project of Henan Normal University(No.YB202402).
文摘We developed a dedicated data analysis framework for silicon strip detector telescopes(SSDTs)of the Compact Spectrometer for Heavy-IoN Experiments(CSHINE)that addresses the challenges of processing complex signals.The framework integrates advanced algorithms for precise calibration,accurate particle identification,and efficient event reconstruction,aiming to account for critical experimental factors such as charge-sharing effects,multi-hit event resolution,and detector response nonuniformity.Its robust performance was demonstrated through the successful analysis of light-charged particles in the 25 MeV/u^(86)Kr+^(124)Sn experiment conducted at the first Radioactive Ion Beam Line in Lanzhou,allowing for precise extraction of physical observables,including energy,momentum,and particle type.Furthermore,utilizing the reconstructed physical information,such as the number of effective physical events and energy spectra to optimize the track recognition algorithm,the final track recognition efficiencies of approximately 90%were achieved.This framework establishes a valuable reference methodology for SSDT-based detector systems in heavy-ion reaction experiments,thereby significantly enhancing the accuracy and efficiency of data analysis in nuclear physics research.
基金funded by internal grants from the Ward Family Heart Center.
文摘A bicuspid aortic valve,from autologous tissue,with growth potential can be constructed using the simple,and reproducible telescoping arterial trunk technique.
基金supported by the Space Debris Resear-ch Project,China(KJSP2020010102)the NationalKey R&D Program of China(2022YFC2807300).
文摘Effective motors are crucial for driving astronomical telescopes,especially for those operating in Antarctica,where the harsh environment and operating conditions,including extreme low temperature,ice/snow accumulation,low power consumption,and unattended operation,introduce challenges to the design and development of motor drives.We present the design of a permanent magnet synchronous motor suitable for this environment,conducting a quantitative analysis on the impacts of cryogenic conditions on lubricant performance,differential thermal contraction of metallic components,and remanent flux density of neodymium iron boron(N52)permanent magnets.We also implement a labyrinth seal structure,combined with silicone sealing rings,to mitigate ice crystal intrusion risks.Finite element analysis and laboratory tests demonstrate a maximum torque output of 25 Nm.This kind of motor is used in the Antarctic 15 cm Near Infrared Telescope at Dome A,Antarctica.Operation data shows a total encoder feedback error of 0.0678"for the telescope control system with 15"s^(−1)tracking speed at−56.79°C.These results comprehensively validate the high reliability and precision of the motor under the extreme conditions of the polar environment.
