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An observation control system for radio telescopes based on Python and C++languages

Astronomical Techniques and Instruments 2024年第6期1卷 307-315页

作者： Yuxiang Huang Longfei Hao Kejia Lee Wei Dai Min Wang Zhixuan Li Yonghua Xu Bojun Wang Faxin Shen Yunnan Observatories Chinese Academy of SciencesKunming 650216China University of Chinese Academy of Sciences Beijing 100049China Kavli Institute for Astronomy and Astrophysics Peking UniversityBeijing 100871China Computer Technology Application Key Lab of Yunnan Province Kunming University of Science and Technology Kunming 650050China National Astronomical Observatories Chinese Academy of SciencesBeijing 100101China

An observation control system is the foundation to support automatic observations by any radio *** observation control systems are usually coded using a compiled language,which is of higher efficiency compared with interpreted ***,observation control systems are usually programmed using the C or C++***,the high execution efficiency of C/C++is at the cost of a long development cycle,which is not only time consuming but also requires considerable skills for the *** development of computer hardware performance,as well as the optimization of the just-in-time compiler for new interpreted languages such as Python,provides a good balance between execution and development *** this paper,we introduce the observation control system developed for the Kunming 40-meter radio telescope run by Yunnan Observatories,Chinese Academy of *** system is developed mainly with the Python language,and we have optimized computationally intensive components with C++.We demonstrate that it is possible to achieve the required functionality and control precision with such a Python-C++programming *** performance of the control system is also assessed in this paper,demonstrating that satisfactory pointing accuracy and user experience can be attained.

关键词： Observation control system radio telescopes Ease of development

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The Giant radio Array for Neutrino Detection(GRAND):Science and design

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Science China(Physics,Mechanics & Astronomy) 2020年第1期63卷 1-43页

作者： Jaime Alvarez-Muniz Rafael Alves Batista Aswathi Balagopal V. Julien Bolmont Mauricio Bustamante Washington Carvalho Jr. Didier Charrier Ismael Cognard Valentin Decoene Peter B.Denton Sijbrand De Jong Krijn D.De Vries Ralph Engel Ke Fang Chad Finley Stefano Gabici Quan Bu Gou Jun Hua Gu Claire Guépin Hong Bo Hu Yan Huang Kumiko Kotera Sandra Le Coz Jean-Philippe Lenain Guo Liang Léü Olivier Martineau-Huynh Miguel Mostafá Fabrice Mottez Kohta Murase Valentin Niess Foteini Oikonomou Tanguy Pierog Xiang Li Qian Bo Qin Duan Ran Nicolas Renault-Tinacci Markus Roth Frank G.Schroder Fabian Schüssler Cyril Tasse Charles Timmerman Matías Tueros Xiang Ping Wu Philippe Zarka Andreas Zech B.Theodore Zhang Jian Li Zhang Yi Zhang Qian Zheng Anne Zilles Departamento de Fisica de Particulas&lnstituto Galego de Fisica de Altas Enerxias Universidad de Santiago de CompostelaSantiago de Compostela 15782Spain Instituto de Astronomia Geofisica e Ciencias AtmosfericasUniversidade de Sao PauloSao Paulo-SP 05508-090Brazil Department of Physics-Astrophysics University of OxfordDWBOxford 0X13RHUK Institute of Experimental Particle Physics(ETP) Karlsruhe Institute of Technology(KIT)Karlsru he D-76021Germany Laboratoire de Physique Nucleeaire et de Hautes Energies(LPNHE) Sorbonne UniversiteUniversite Paris DiderotSorbonne Paris CiteCNRS place Jussieu F-75252Paris Cedex 5France Niels Bohr International Academy and DARK Niels Bohr InstituteCopenhagen 2100Denmark Discovery Center Niels Bohr InstituteCopenhagen 2100Denmark Center for Cosmology and AstroParticle Physics(CCA.PP)&Department of Physics Ohio State UniversityColumbus OH 43210USA Universidade de Santiago de Compostela Santiago de Compostela 15782Spain 0SUBATECH Institut Mines-Telecom Atlantique-CNRS/IN2P3-Universite de NantesNantes 44300France Laboratoire de Physique et Chimie de KEnvironnement et de VEspace LPC2E CNRS-Universite d'Orleans Orleans F-45071France Station de radioastronomie de Nancay Observatoire de ParisCNRS/INSU F-18330 NangayFrance Sorbonne Universite UMR 7095Institut d'Astrophysique de Paris98 bis bd AragoParis 75014France Institute for Mathematics Astrophysics and Particle Physics(IMAPP)Radboud UniversiteitNijmegen 6500Netherlands Nationaal Instituut voor Kemfysica en Hoge Energie Fysica(NIKHEF) Amsterdam NL-1009Netherlands IIHE/ELEM Vrije Universiteit BrusselPleinlaan 2Brussels 1050Belgium Institute for Nuclear Physics(IKP) Karlsruhe Institute of Technology(KIT)Karlsruhe D-76021Germany Einstein Fellow Stanford UniversityStanford CA 94305USA Department of Astronomy University of MarylandCollege Park MD 20742-2421USA Joint Space-Science Institute College Park MD 20742-2421USA Oskar Klein Centre Stockholm UniversityStockholm SE-10691Sweden Department of Phy

The Giant radio Array for Neutrino Detection(GRAND)is a planned large-scale observatory of ultra-high-energy(UHE)cosmic particles,with energies exceeding 10~8 Ge *** goal is to solve the long-standing mystery of the origin of UHE cosmic *** do this,GRAND will detect an unprecedented number of UHE cosmic rays and search for the undiscovered UHE neutrinos and gamma rays associated to them with unmatched *** will use large arrays of antennas to detect the radio emission coming from extensive air showers initiated by UHE particles in the *** design is modular:20 separate,independent sub-arrays,each of 10000 radio antennas deployed over 10000 km^2.A staged construction plan will validate key detection techniques while achieving important science goals *** we present the science goals,detection strategy,preliminary design,performance goals,and construction plans for GRAND.

关键词： radio telescopes neutrinos in astronomical observations cosmic rays in astronomical observations radiowave radiation:sources galactic and extragalactic cosmic rays:galactic and extragalactic

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Pulsar timing observations with Haoping radio Telescope

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Research in Astronomy and Astrophysics 2020年第7期20卷 187-192页

作者： Jin-Tao Luo Yu-Ping Gao Ting-Gao Yang Cheng-Shi Zhao Ming-Lei Tong Yong-Nan Rao Yi-Feng Li Bian Li Xing-Zhi Zhu Hai-Hua Qiao Xiao-Chun Lu National Time Service Center Chinese Academy of SciencesXi’an 710600China Key Lab of Precision Navigation&Timing Technology Chinese Academy of SciencesXi’an 710600China University of Chinese Academy of Sciences Beijing 100049China

We report pulsar timing observations carried out in L-band with NTSC’s 40-meter Haoping radio Telescope(HRT),which was constructed in *** observations were carried out using the pulsar machine we *** observations toward millisecond pulsar J0437–4715 obtain a timing residual(r.m.s.)of 397 ns in the time span of 284 *** observations successfully detected Crab pulsar’s glitch that happened on 2019 July 23.

关键词： radio telescopes instrumentation:miscellaneous methods:data analysis pulsars:general

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An Event Horizon Imager(EHI) Mission Concept Utilizing Medium Earth Orbit Sub-mm Interferometry

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空间科学学报 2021年第2期41卷 211-233页

作者： KUDRIASHOV V MARTIN-NEIRA M ROELOFS F FALCKE H BRINKERINK C BARYSHEV A HOGERHEIJDE M YOUNG A POURSHAGHAGHI H KLEIN-WOLT M MOSCIBRODZKA M DAVELAAR J BARAT I DUESMANN B VALENTA V PERDIGUES ARMENGOL J M DE WILDE D MARTIN IGLESIAS P ALAGHA N VAN DER VORST M Department of Astrophysics/IMAPP Radboud University NijmegenP.O.Box 90106500 GL Nijmegenthe Netherlands ESTEC/ESA Keplerlaan 12201 A2 Noordurigkthe Netherlands Mar Planck Institute for radio Astrorny Auf dem Higel 69D-53121 Bon(Endenich)Germany University of Groningen Landleven 129747 AD Groningenthe Netherlands Leiden Observatory Leiden UniversityPO Box 95132300 RALeidenthe Netherlands Anton Pannekoek Institute for Astronomy University of AmsterdamScience Park 9041098 XHAmsterdamthe Netherlands Center for Computational Astrophysics Flatiron Institute162 Fifth AvenueNew YorkNY 10010USA

Submillimeter interferometry has the potential to image supermassive black holes on event horizon scales,providing tests of the theory of general relativity and increasing our understanding of black hole accretion *** Event Horizon Telescope(EHT) performs these observations from the ground,and its main imaging targets are Sagittarius A~* in the Galactic Center and the black hole at the center of the M87 ***,the EHT is fundamentally limited in its performance by atmospheric effects and sparse terrestrial(u,v)-coverage(Fourier sampling of the image).The scientific interest in quantitative studies of the horizon size and shape of these black holes has motivated studies into using space interferometry which is free of these *** resolution considerations and interstellar scattering effects push the desired observing frequency to bands above 500 *** paper presents the requirements for meeting these science goals,describes the concept of interferometry from Polar or Equatorial Medium Earth Orbits(PECMEO) which we dub the Event Horizon Imager(EHI),and utilizes suitable space technology *** this concept,two or three satellites orbit at slightly different orbital radii,resulting in a dense and uniform spiral-shaped(u,v)-coverage over *** local oscillator signals are shared via an inter-satellite link,and the data streams are correlated on-board before final processing on the ***-satellite metrology and satellite positioning are extensively employed to facilitate the knowledge of the instrument position vector,and its time *** European space heritage usable for both the front ends and the antenna technology of such an instrument is *** and future sensors for the required inter-satellite metrology are *** performance estimates and simulation results are given.

关键词： Instrumentation Space VLBI radio telescopes

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Kinematic calibration of precise 6-DOF Stewart platform-type positioning systems for radio telescope applications

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Frontiers of Mechanical Engineering 2013年第3期8卷 252-260页

作者： Juan Carlos JUREGUI Eusebio E.HERNNDEZ Marco CECCARELLI Carlos LOPEZ-CAJUN Alejandro GARCIA División de Estudios de Posgrado Facultad de IngenieríaUniversidad Autónoma de Quéretaro QuéretaroQro.Mexico National Polytechnic Institute IPNSection of Graduate Studies and ResearchESIME-UPTMéxico D.F.Mexico Laboratory of Robotics and Mechatronics University of Cassino Italy Universidad Autónoma de Quéretaro Querétaro Qro.México CIATEQ A.C.AguascalientesAgs.México

The pose accuracy of a parallel robot is a function of the mobile platform ***,there is no a single value of the robot’s *** this paper,two novel methods for estimating the accuracy of parallel robots are *** the frst method,the pose accuracy estimation is calculated by considering the propagation of each error,i.e.,error variations are considered as a function of the actuator’s *** the second method,it is considered that each actuator has a constant error at any *** methods can predict pose accuracy of precise robots at design stages,and/or can reduce calibration time of existing *** example of a six degree-of-freedom parallel manipulator is included to show the application of the proposed methods.

关键词： pose errors error estimation parallel robot radio telescopes

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The Giant radio Array for Neutrino Detection(GRAND):Science and design

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Science China(Physics,Mechanics & Astronomy) 2020年第1期Mechanics & Astronomy) .卷 5-47页

作者： Jaime álvarez-Mu?iz Rafael Alves Batista Aswathi Balagopal V. Julien Bolmont Mauricio Bustamante Washington Carvalho Jr. Didier Charrier Isma?l Cognard Valentin Decoene Peter B.Denton Sijbrand De Jong Krijn D.De Vries Ralph Engel Ke Fang Chad Finley Stefano Gabici Quan Bu Gou Jun Hua Gu Claire Guépin Hong Bo Hu Yan Huang Kumiko Kotera Sandra Le Coz Jean-Philippe Lenain Guo Liang Léü Olivier Martineau-Huynh Miguel Mostafá Fabrice Mottez Kohta Murase Valentin Niess Foteini Oikonomou Tanguy Pierog Xiang Li Qian Bo Qin Duan Ran Nicolas Renault-Tinacci Markus Roth Frank G.Schr ?der Fabian Schüssler Cyril Tasse Charles Timmerman Matías Tueros Xiang Ping Wu Philippe Zarka Andreas Zech B.Theodore Zhang Jian Li Zhang Yi Zhang Qian Zheng Anne Zilles Departamento de Física de Partículas & Instituto Galego de Física de Altas Enerxías Universidad de Santiago de Compostela Instituto de Astronomia Geofísica e Ciências Atmosféricas Universidade de S?o Paulo Department of Physics—Astrophysics University of Oxford DWB Institute of Experimental Particle Physics (ETP) Karlsruhe Institute of Technology (KIT) Laboratoire de Physique Nucléeaire et de Hautes Energies (LPNHE) Sorbonne Université Université Paris Diderot Sorbonne Paris Cité Niels Bohr International Academy and DARK Niels Bohr Institute Discovery Center Niels Bohr Institute Center for Cosmology and Astro Particle Physics (CCAPP) & Department of Physics Ohio State University Universidade de Santiago de Compostela SUBATECH Institut Mines-Telecom Atlantique – CNRS/IN2P3 – Université de Nantes Laboratoire de Physique et Chimie de l’Environnement et de l’Espace LPC2E CNRS-Université d’Orléans Station de radioastronomie de Nan?cay Observatoire de Paris Sorbonne Université UMR 7095 Institut d’Astrophysique de Paris Institute for Mathematics Astrophysics and Particle Physics (IMAPP) Radboud Universiteit Nationaal Instituut voor Kernfysica en Hoge Energie Fysica (NIKHEF) IIHE/ELEM Vrije Universiteit Brussel Institute for Nuclear Physics (IKP) Karlsruhe Institute of Technology (KIT) Einstein Fellow Stanford University Department of Astronomy University of Maryland Joint Space-Science Institute Oskar Klein Centre Stockholm University Department of Physics Stockholm University Astro Particule et Cosmologie (APC) Université Paris Diderot CNRS/IN2P3 CEA/Irfu Observatoire de Paris Institute of High Energy Physics Chinese Academy of Sciences National Astronomical Observatories Chinese Academy of Sciences School of Physical Science and Technology Xinjiang University Center for Particle and Gravitational Astrophysics Pennsylvania State University Department of Physics Pennsylvania State University Department of Astronomy & Astrophysics Pennsylvania State University LUTH Observatoire de Paris

The Giant radio Array for Neutrino Detection（GRAND） is a planned large-scale observatory of ultra-high-energy（UHE） cosmic particles, with energies exceeding 10～8 Ge V. Its goal is to solve the long-standing mystery of the origin of UHE cosmic rays. To do this, GRAND will detect an unprecedented number of UHE cosmic rays and search for the undiscovered UHE neutrinos and gamma rays associated to them with unmatched sensitivity. GRAND will use large arrays of antennas to detect the radio emission coming from extensive air showers initiated by UHE particles in the atmosphere. Its design is modular: 20 separate, independent sub-arrays, each of 10000 radio antennas deployed over 10000 km2. A staged construction plan will validate key detection techniques while achieving important science goals early. Here we present the science goals, detection strategy, preliminary design, performance goals, and construction plans for GRAND.

关键词： radio telescopes neutrinos in astronomical observations cosmic rays in astronomical observations radiowave radiation: sources galactic and extragalactic cosmic rays

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