由中国科学院紫金山天文台牵头,联合国内外多家研究机构组成的研究团队,利用500 m口径球面射电望远镜中国天眼(FAST)取得重要突破——在国际上首次捕捉到重复快速射电暴(fost rodio bursts,FRB)的法拉第旋转量(rotation measure,RM)发...由中国科学院紫金山天文台牵头,联合国内外多家研究机构组成的研究团队,利用500 m口径球面射电望远镜中国天眼(FAST)取得重要突破——在国际上首次捕捉到重复快速射电暴(fost rodio bursts,FRB)的法拉第旋转量(rotation measure,RM)发生剧烈跃变并随后回落的详细演化过程。这一发现结果为“快速射电暴起源于双星系统”的假说提供了迄今为止最有力的观测证据。2026年1月16日,相关研究成果发表于《Science》。展开更多
The Haoping 40 m radio telescope at the National Time Service Center,Chinese Academy of Sciences was built in 2014 and is primarily used to observe navigation satellites and pulsars.Since the first successful very lon...The Haoping 40 m radio telescope at the National Time Service Center,Chinese Academy of Sciences was built in 2014 and is primarily used to observe navigation satellites and pulsars.Since the first successful very long baseline interferometry(VLBI)observation of L-band radio source fringes in 2022,ten observations have been made so far.The stations involved in the observations include the Haoping 40 m radio telescope(Haoping),the Tianma 65 m radio telescope(Tianma),the Nanshan 26 m radio telescope(Urumqi),the Guizhou 500 m radio telescope(FAST),the Jilin 13 m radio telescope(Jilin),the Effelsberg 100 m radio telescope(Effelsberg),the Onsala 25 m radio telescope(Onsala),and the Chiang Mai 40 m radio telescope(Chiang Mai).This paper presents details on the specifications of the Haoping 40 m radio telescope,as well as the design of the VLBI experiment,the observation process,and the data processing.We also discuss the analysis of the fringe results involving the Haoping 40 m radio telescope,using Distributed FX Correlator to obtain excellent results.We confirm that the telescope is capable of participating in VLBI observations and performing specific data processing tasks.It can therefore play a greater role in future VLBI observations.展开更多
Owing to its large aperture and advanced receivers,research plans for the Qitai 110 m radio telescope(QTT)include a variety of spectral line scientific studies.Sequential construction of receiver systems and multidisc...Owing to its large aperture and advanced receivers,research plans for the Qitai 110 m radio telescope(QTT)include a variety of spectral line scientific studies.Sequential construction of receiver systems and multidisciplinary planning require overcoming serious challenges to spectral line digital backend development,notably to digitize,process,and transmit considerable quantities of observational data,to minimize time-to-science with an easily scalable architecture,and to provide robust,high-quality data.As a proof-of-concept for the QTT backend,here we implement a baseband spectral line digital backend with a SNAP+GPU architecture.The SNAP-based digital frontend comprises two digitization links(1000 MHz,8-bit),two parallel quad-channel preprocessing modules,a quantization module,and a finite-state packaging module,generating a 100-MHz bandwidth digital link from the original analog signal through high-speed Ethernet transmission.The GPU node receives preprocessed baseband packets,constructs a ring buffer for lossless unpacking and distributing,with real-time data reception and caching,and conducts real-time spectral analysis(frequency resolution:3.051 kHz)of the 100 MHz baseband data.We evaluated system performance experimentally using spectral line observations with the Nanshan 26-m radio telescope(NSRT).For the QTT,the SNAP digital frontend will be seamlessly migrated to a radio frequency system-on-chip(RFSoC)architecture,resulting in five-and tenfold increases in instantaneous bandwidth and data throughput,respectively.The low-coupling digital frontend and GPU node can be easily extended to multiple nodes.展开更多
射电天文的发展需要更宽的观测频率,但是随着通讯的不断发展,射频无线电干扰(Radio Frequency Interference,RFI)对射电观测的影响日益加重,射电望远镜需要选择电磁环境优良的站址并进行保护.文中描述了目前国内在建和预研阶段的望远镜...射电天文的发展需要更宽的观测频率,但是随着通讯的不断发展,射频无线电干扰(Radio Frequency Interference,RFI)对射电观测的影响日益加重,射电望远镜需要选择电磁环境优良的站址并进行保护.文中描述了目前国内在建和预研阶段的望远镜的电磁环境的测试过程,阐述了数据分析和处理方法.通过对我国射电望远镜台址选择和保护进行的电磁环境测试,优选出适合建立大型射电望远镜的台址.展开更多
云南天文台射电天文研究团组采用40 m射电望远镜以及数字基带转换器(Digital Base Band Conveter,DBBC)数据采集终端、Mark5B记录系统和DSPSR(The Digital Signal Processing for Pulsars)软件包实现对脉冲星观测数据的相干消色散处理...云南天文台射电天文研究团组采用40 m射电望远镜以及数字基带转换器(Digital Base Band Conveter,DBBC)数据采集终端、Mark5B记录系统和DSPSR(The Digital Signal Processing for Pulsars)软件包实现对脉冲星观测数据的相干消色散处理的脉冲星观测系统。该系统对PSR J0835-4510和PSR J0332+5434进行观测,采用DSPSR软件包对脉冲星观测处理,还可以生成PSRFITS格式的数据。观测频段选用S波段右旋圆极化信号,分别实现了2通道总带宽为4 MHz、4通道总带宽为16 MHz、8通道总带宽为128 MHz的观测和数据处理。构建以DSPSR为数据处理核心的脉冲星观测系统,比DBBC+Mark5B的观测系统在数据处理方法、运算效率和观测数据的通用性方面具有更好的优越性。展开更多
文摘由中国科学院紫金山天文台牵头,联合国内外多家研究机构组成的研究团队,利用500 m口径球面射电望远镜中国天眼(FAST)取得重要突破——在国际上首次捕捉到重复快速射电暴(fost rodio bursts,FRB)的法拉第旋转量(rotation measure,RM)发生剧烈跃变并随后回落的详细演化过程。这一发现结果为“快速射电暴起源于双星系统”的假说提供了迄今为止最有力的观测证据。2026年1月16日,相关研究成果发表于《Science》。
基金supported by the National Science and Technology Major Project(E152KJ1201)the Natural Science Basic Research Program of Shaanxi(2024JC-YBQN-0036)+1 种基金the National Natural Science Foundation of China(42030105 and 11973046)the National SKA Program of China(2020SKA0120200).
文摘The Haoping 40 m radio telescope at the National Time Service Center,Chinese Academy of Sciences was built in 2014 and is primarily used to observe navigation satellites and pulsars.Since the first successful very long baseline interferometry(VLBI)observation of L-band radio source fringes in 2022,ten observations have been made so far.The stations involved in the observations include the Haoping 40 m radio telescope(Haoping),the Tianma 65 m radio telescope(Tianma),the Nanshan 26 m radio telescope(Urumqi),the Guizhou 500 m radio telescope(FAST),the Jilin 13 m radio telescope(Jilin),the Effelsberg 100 m radio telescope(Effelsberg),the Onsala 25 m radio telescope(Onsala),and the Chiang Mai 40 m radio telescope(Chiang Mai).This paper presents details on the specifications of the Haoping 40 m radio telescope,as well as the design of the VLBI experiment,the observation process,and the data processing.We also discuss the analysis of the fringe results involving the Haoping 40 m radio telescope,using Distributed FX Correlator to obtain excellent results.We confirm that the telescope is capable of participating in VLBI observations and performing specific data processing tasks.It can therefore play a greater role in future VLBI observations.
基金supported by the “Light in China’s Western Region” program (2022-XBQNXZ012)by the National Natural Science Foundation of China(12073067)
文摘Owing to its large aperture and advanced receivers,research plans for the Qitai 110 m radio telescope(QTT)include a variety of spectral line scientific studies.Sequential construction of receiver systems and multidisciplinary planning require overcoming serious challenges to spectral line digital backend development,notably to digitize,process,and transmit considerable quantities of observational data,to minimize time-to-science with an easily scalable architecture,and to provide robust,high-quality data.As a proof-of-concept for the QTT backend,here we implement a baseband spectral line digital backend with a SNAP+GPU architecture.The SNAP-based digital frontend comprises two digitization links(1000 MHz,8-bit),two parallel quad-channel preprocessing modules,a quantization module,and a finite-state packaging module,generating a 100-MHz bandwidth digital link from the original analog signal through high-speed Ethernet transmission.The GPU node receives preprocessed baseband packets,constructs a ring buffer for lossless unpacking and distributing,with real-time data reception and caching,and conducts real-time spectral analysis(frequency resolution:3.051 kHz)of the 100 MHz baseband data.We evaluated system performance experimentally using spectral line observations with the Nanshan 26-m radio telescope(NSRT).For the QTT,the SNAP digital frontend will be seamlessly migrated to a radio frequency system-on-chip(RFSoC)architecture,resulting in five-and tenfold increases in instantaneous bandwidth and data throughput,respectively.The low-coupling digital frontend and GPU node can be easily extended to multiple nodes.
文摘射电天文的发展需要更宽的观测频率,但是随着通讯的不断发展,射频无线电干扰(Radio Frequency Interference,RFI)对射电观测的影响日益加重,射电望远镜需要选择电磁环境优良的站址并进行保护.文中描述了目前国内在建和预研阶段的望远镜的电磁环境的测试过程,阐述了数据分析和处理方法.通过对我国射电望远镜台址选择和保护进行的电磁环境测试,优选出适合建立大型射电望远镜的台址.
文摘云南天文台射电天文研究团组采用40 m射电望远镜以及数字基带转换器(Digital Base Band Conveter,DBBC)数据采集终端、Mark5B记录系统和DSPSR(The Digital Signal Processing for Pulsars)软件包实现对脉冲星观测数据的相干消色散处理的脉冲星观测系统。该系统对PSR J0835-4510和PSR J0332+5434进行观测,采用DSPSR软件包对脉冲星观测处理,还可以生成PSRFITS格式的数据。观测频段选用S波段右旋圆极化信号,分别实现了2通道总带宽为4 MHz、4通道总带宽为16 MHz、8通道总带宽为128 MHz的观测和数据处理。构建以DSPSR为数据处理核心的脉冲星观测系统,比DBBC+Mark5B的观测系统在数据处理方法、运算效率和观测数据的通用性方面具有更好的优越性。
