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The FAST all sky HI survey(FASHI):The first release of catalog

Science China(Physics,Mechanics & Astronomy) 2024年第1期67卷 112-133页

作者： Chuan-Peng Zhang Ming Zhu Peng Jiang Cheng Cheng Jing Wang Jie Wang Jin-Long Xu Xiao-Lan Liu Nai-Ping Yu Lei Qian Haiyang Yu Mei Ai Yingjie Jing Chen Xu Ziming Liu Xin Guan Chun Sun Qingliang Yang Menglin Huang Qiaoli Hao FAST Collaboration Guizhou Radio Astronomical Observatory Guizhou UniversityGuiyang 550000China National Astronomical Observatories Chinese Academy of Sciences(CAS)Beijing 100101China Chinese Academy of Sciences South America Center for Astronomy National Astronomical ObservatoriesCASBeijing 100101China Kavli Institute for Astronomy and Astrophysics Peking UniversityBeijing 100871China

The FAST All Sky HI survey(FASHI)was designed to cover the entire sky observable by the Five-hundred-meter Aperture Spherical radio telescope(FAST),spanning approximately 22000 square degrees of declination between-14°and+66°,and in the frequency range of 1050-1450 MHz,with the expectation of eventually detecting more than 100000 HI sources.Between August 2020 and June 2023,FASHI had covered more than 7600 square degrees,which is approximately 35%of the total sky observable by FAST.It has a median detection sensitivity of around 0.76 m Jy beam-1and a spectral line velocity resolution of~6.4 km s-1at a frequency of~1.4 GHz.As of now,a total of 41741 extragalactic HI sources have been detected in the frequency range 1305.5-1419.5 MHz,corresponding to a redshift limit of z■0.09.By cross-matching FASHI sources with the Siena Galaxy Atlas(SGA)and the Sloan Digital Sky Survey(SDSS)catalogs,we found that 16972(40.7%)sources have spectroscopic redshifts and 10975(26.3%)sources have only photometric redshifts.Most of the remaining 13794(33.0%)HI sources are located in the direction of the Galactic plane,making their optical counterparts difficult to identify due to high extinction or high contamination of Galactic stellar sources.Based on current survey results,the FASHI survey is an unprecedented blind extragalactic H I survey.It has higher spectral and spatial resolution and broader coverage than the Arecibo Legacy Fast ALFA Survey(ALFALFA).When completed,FASHI will provide the largest extragalactic HI catalog and an objective view of HI content and large-scale structure in the local universe.

关键词： surveys redshifts galaxies telescope radio lines HI line

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FAST:The Five-Hundred-Meter Aperture Spherical Radio telescope

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Engineering 2023年第9期28卷 21-25页

作者： Peng Jiang Hengqian Gan Rui Yao Jinghai Sun Jiguang Lu Dongjun Yu Hui Li Jinglong Yu Bin Dong Xiaoming Chai Jianing Yin Guizhou Radio Astronomical Observatory Guizhou UniversityGuiyang 550025China FAST Operation and Development Center National Astronomical ObservatoriesChinese Academy of SciencesBeijing 100101China

In the 90 years since its inception,radio astronomy has become the setting of almost all major astronomical discoveries and a hothouse for Nobel Prizes in Physics.As a result,countries all over the world have actively explored new engineering concepts to build large-aperture radio telescopes.Limited by their self-weight and wind load,100 m radio telescopes are regarded as the maximum limit of traditional radio telescopes.This perspective allowed the Arecibo 305 m telescope—built by Cornell University in the United States in 1963—to dominate the field for more than half a century.During this period,scholars have been exploring how to further expand their horizons in order to make a breakthrough in the problem of the universe.

关键词： breakthrough telescope horizon

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Understanding the circular polarization of fast radio bursts observed by the Five-hundred-meter Aperture Spherical Radio telescope

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Science China(Physics,Mechanics & Astronomy) 2022年第10期65卷 155-156页

作者： Hao Tong School of Physics and Materials Science Guangzhou UniversityGuangzhou 510006China

China's Five-hundred-meter Aperture Spherical Radio telescope(FAST)is the world's largest single-disk radio telescope.Because of its high sensitivity,it can reveal the most intriguing properties of pulsars and fast ra... 详细信息

关键词： bursts telescope observed

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The High Energy X-ray telescope (HE) onboard the Insight-HXMT astronomy satellite

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Science China(Physics,Mechanics & Astronomy) 2020年第4期63卷 20-34页

作者： CongZhan Liu YiFei Zhang XuFang Li XueFeng Lu Zhi Chang ZhengWei Li AiMei Zhang YongJie Jin HuiMing Yu Zhao Zhang MinXue Fu YiBao Chen JianFeng Ji YuPeng Xu JingKang Deng RenCheng Shang GuoQing Liu FangJun Lu ShuangNan Zhang YongWei Dong TiPei Li Mei Wu YanGuo Li HuanYu Wang BoBing Wu YongJie Zhang Zhi Zhang ShaoLin Xiong Yuan Liu Shu Zhang HongWei Liu YiJung Yang Fan Zhang Key Laboratory of Particle Astrophysics Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China Department of Engineering Physics Tsinghua UniversityBeijing 100084China Department of Physics Tsinghua UniversityBeijing 100084China University of Chinese Academy of Sciences Beijing 100049China

The Insight-Hard X-ray Modulation telescope(Insight-HXMT) is a broadband X-ray and γ-ray(1-3000 ke V) astronomy satellite. One of its three main telescopes is the High Energy X-ray telescope(HE). The main detector plane of HE comprises 18 Na I(Tl)/Cs I(Na) phoswich detectors, where Na I(Tl) is used as the primary detector to measure ~ 20-250 ke V photons incident from the field of view(FOV) defined by collimators, and Cs I(Na) is used as the active shielding detector to Na I(Tl) by pulse shape discrimination. Additionally, Cs I(Na) is used as an omnidirectional γ-ray monitor. The HE collimators have a diverse FOV,i.e. 1.1°×5.7°(15 units), 5.7°×5.7°(2 units), and blocked(1 unit). Therefore, the combined FOV of HE is approximately5.7°×5.7°. Each HE detector has a diameter of 190 mm resulting in a total geometrical area of approximately 5100 cm2, and the energy resolution is ~15% at 60 ke V. For each recorded X-ray event by HE, the timing accuracy is less than 10 μs and the deadtime is less than 10 μs. HE is used for observing spectra and temporal variability of X-ray sources in the 20-250 ke V band either by pointing observations for known sources or scanning observations to unveil new sources. Additionally, HE is used for monitoring the γ-ray burst in 0.2-3 Me V band. This paper not only presents the design and performance of HE instruments but also reports results of the on-ground calibration experiments.

关键词： X-ray telescope HXMT calibration scintillation detector

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Research on telescope TTL Coupling Noise in Intersatellite Laser Interferometry

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Photonic Sensors 2020年第3期10卷 265-274页

作者： Zhi WANG Tao YU Ya ZHAO Ziren LUO Wei SHA Chao FANG Yukun WANG Shaoxin WANG Keqi QI Yongxian WANG Xuanwen XU Changchun Institute of Optics Fine Mechanics and PhysicsChinese Academy of SciencesChangchun 130033China University of Chinese Academy of Sciences Beijing 100049China Institute of Mechanics Chinese Academy of SciencesBeijing 100190China Jilin University Changchun 130022China

The detection mission of gravitational waves in space is that the accuracy of the long-baseline intersatellite laser interferometry on the million-kilometer order needs to reach the order of 8 pm/Hz.Among all noise sources that affect the interferometry accuracy,tilt-to-length(TTL)coupling noise is the second largest source of noise after shot noise.This paper focuses on studying the contribution of TTL coupling noise of the telescope system in the intersatellite scientific interferometer.By referring to the laser interferometer space antenna(LISA)’s noise budget,TTL coupling noise is required to be within±25μm/rad(±300μrad).Therefore,this paper focuses on studying both the mechanism of TTL coupling noise due to the noise sources of the telescope and the method of suppressing the TTL noise,which can lay a foundation for noise distribution and the development of engineering prototypes in subsequent tasks.

关键词： Intersatellite laser interferometry telescope TTL coupling noise

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The Low Energy X-ray telescope (LE) onboard the Insight-HXMT astronomy satellite

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Science China(Physics,Mechanics & Astronomy) 2020年第4期63卷 49-61页

作者： Yong Chen WeiWei Cui Wei Li Juan Wang YuPeng Xu FangJun Lul YuSa Wang TianXiang Chen DaWei Han Wei Hu Yi Zhang Jia Huo YanJi Yang MaoShun Li Bo Lu ZiLiang Zhang TiPei Li ShuangNan Zhang ShaoLin Xiong Shu Zhang RongFeng Xue XiaoFan Zhao Yue Zhu YuXuan Zhu HongWei Liu YiJung Yang Fan Zhang Key Laboratory of Particle Astrophysics Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China University of Chinese Academy of Sciences Beijing 100049China Department of Physics Tsinghua UniversityBeijing 100084China Department of Education Lu Liang UniversityLuliang 033000China Qian Xuesen Laboratory of Space Technology China Academy of Space TechnologyBeijing 100094China College of Physics Jilin UniversityChangchun 130023China

The Low Energy X-ray telescope(LE) is one of the three main instruments of the Insight-Hard X-ray Modulation telescope(Insight-HXMT). It is equipped with Swept Charge Device(SCD) sensor arrays with a total geometrical area of 384 cm^2 and an energy band from 0.7 to 13 ke V. In order to evaluate the particle induced X-ray background and the cosmic X-ray background simultaneously, LE adopts collimators to define four types of Field Of Views(FOVs), i.e., 1.6°×6°, 4°×6°, 50°-60°×2°-6 oand the blocked ones which block the X-ray by an aluminum cover. LE is constituted of three detector boxes(LEDs) and an electric control box(LEB) and achieves a good energy resolution of 140 e V@5.9 ke V, an excellent time resolution of 0.98 ms, as well as an extremely low pileup(<1%@18000 cts/s). Detailed performance tests and calibration on the ground have been performed,including energy-channel relation, energy response, detection efficiency and time response.

关键词： LE X-ray telescope SCD collimators

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Stray light analysis of the Xinglong 2.16-m telescope

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Research in Astronomy and Astrophysics 2020年第3期20卷 50-61页

作者： Tao-Ran Li Jian-Feng Wang Xiao-Ming Zhang Yong Zhao Jian-Feng Tian Key Laboratory of Optical Astronomy National Astronomical ObservatoriesChinese Academy of SciencesBeijing 100101China University of Chinese Academy of Sciences Beijing 100049China

An effort towards understanding the problems associated with stray light related to the Xinglong2.16-m telescope is presented to estimate the stray light performance of the telescope itself and provide a method for improving stray light suppression.Stray light analysis for the 2.16-m telescope model,which consists of an onion shaped dome,telescope structure,equatorial mount and telescope optics,has been developed in two cases(1)pointing to 60?and(2)pointing to zenith,in both azimuth and elevation directions.The Point Source Normalized Irradiance Transmittance(PSNIT),which is generally used for assessing stray light and is uncorrelated to entrance aperture,is calculated with a series of off-axis angles.It shows that the PSNIT values are less than 10-7 when off-axis angles are larger than±20?.The dominant contributors to stray light(primary and secondary mirror,telescope structure and dome)are identified to guide performance improvement.The analyses indicate that significant benefit can be realized by adding only five vanes inside the bottom portion of the secondary baffle.In the case of pointing to zenith,the PSNIT values will decrease about 40%on average.

关键词： telescope scattering methods:data analysis

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Upgraded photometric system on the 85-cm telescope at Xinglong station

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Research in Astronomy and Astrophysics 2018年第9期18卷 21-30页

作者： Chun-Hai Bai Jian-Ning Fu Tao-Ran Li Zhou Fan Jiang-Hua Wu Yong Zhao Xian-Qun Zeng Wen-Zhao Zhang Peng Qiu Guo-Jie Feng Xiao-Jun Jiang National Astronomical Observatories Chinese Academy of SciencesBeijing 100101China University of Chinese Academy of Sciences Beijing 100049China Xinjiang Astronomical Observatory Chinese Academy of SciencesUrumqi 830011China Department of Astronomy Beijing Normal UniversityBeijing 100875China

The 85-cm telescope at Xinglong station is a prime focus system that operates well with high science outputs. The telescope has been upgraded since 2014 with a new corrector, and new filters and camera, which are provided by Beijing Normal University. The filter set is the Johnson-Cousins UBV RI system. We report the test results of the new system including bias, dark current, linearity, gain and readout noise of the CCD camera. Then we derive accurate instrumental calibration coefficients in UBV RI bands with Landolt standard stars during photometric nights. Finally, we give the limiting magnitudes with various exposure times and signal-to-noise ratios for observers as references.

关键词： telescope instrumentation CCD photometry

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Five hundred meter aperture spherical radio telescope (FAST)

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Science China(Physics,Mechanics & Astronomy) 2006年第2期49卷 129-148页

作者： NAN Rendong National Astronomical Observatories Beijing 100012 China

Five hundred meter aperture spherical radio telescope (FAST) will be the largest radio telescope in the world. The innovative engineering concept and design pave a new road to realizing a huge single dish in the most effective way. Three outstanding features of the telescope are the unique karst depressions as the sites, the active main reflector which corrects spherical aberration on the ground to achieve full polarization and a wide band without involving a complex feed system, and the light focus cabin driven by cables and servomechanism plus a parallel robot as secondary adjustable system to carry the most precise parts of the receivers. Being the most sensitive radio telescope, FAST will enable astronomers to jumpstart many of the science goals, for example, the neutral hydrogen line surveying in distant galaxies out to very large redshifts, looking for the first shining star, detecting thousands of new pulsars, etc. Extremely interesting and exotic objects may yet await discovery by FAST. As a multi-science platform, the telescope will provide treasures to astronomers, as well as bring prosperity to other research, e.g. space weather study, deep space exploration and national security. The construction of FAST itself is expected to promote the development in high technology of relevant fields.

关键词： radio astronomy radio telescope active reflector.

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The wide-field photometric system of the Nanshan One-meter telescope

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Research in Astronomy and Astrophysics 2020年第12期20卷 373-382页

作者： Chun-Hai Bai Guo-Jie Feng Xuan Zhang Hu-Biao Niu Abdusamatjan Eskandar Guang-Xin Pu Shu-Guo Ma Jin-Zhong Liu Xiao-Jun Jiang Lu Ma Ali Esamdin Na Wang Xinjiang Astronomical Observatories Chinese Academy of SciencesUrumqi 830011China Key Laboratory of Optical Astronomy National Astronomical ObservatoriesChinese Academy of SciencesBeijing 100101China

The Nanshan One-meter Wide-field telescope is a prime focus system that is located at Nanshan Station of Xinjiang Astronomical Observatories.The field of view was designed to 1.5°× 1.5°,and the Johnson-Cousins UBVRI system was chosen as the main filter set.The telescope has been providing observation services for astronomers since September 2013.Variable source searching and time-domain surveys are the main scientific goals.The system’s test results are reported including linearity,dark current,bias,readout noise and gain of the CCD camera.The accurate instrumental calibration coefficients in UBVRI bands were driven with Landolt standard stars during photometric nights.Finally,the limiting magnitudes are given with signal-to-noise ratios and various exposure times for observers.

关键词： telescope filter CCD photometry

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