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  • ReceivedDec 7, 2018
  • AcceptedFeb 25, 2019
  • PublishedMar 22, 2019
PACS numbers

Abstract

The Five-hundred-meter Aperture Spherical radio Telescope (FAST) was completed with its main structure installed on September 25, 2016, after which it entered the commissioning phase. This paper aims to introduce the commissioning progress of the FAST over the past two years. To improve its operational reliability and ensure effective observation time, FAST has been equipped with a real-time information system for the active reflector system and hierarchical commissioning scheme for the feed support system, which ultimately achieves safe operation of the two systems. For meeting the high-performance indices, a high-precision measurement system was set up based on the effective control methods that were implemented for the active reflector system and feed support system. Since the commissioning of the FAST, a low-frequency ultra-wideband receiver and 19-beam 1.05-1.45 GHz receiver have been mainly used. Telescope efficiency, pointing accuracy, and system noise temperature were completely tested and ultimately achieved the acceptance indices of the telescope. The FAST has been in the process of national acceptance preparations and has begun to search for pulsars. In the future, it will still strive to improve its capabilities and expand its application prospects.


Funded by

the National Natural Science Foundation of China(Grant,Nos.,11673039,11573044,11673002,11803051,11503048,11203048)

the Youth Innovation Promotion Association CAS; the Open Project Program of the Key Laboratory of FAST

NAOC

Chinese Academy of Sciences

the National Key Research and Development Program of China(Grant,No.2017YFA0402600)

CAS “Light of West China” Program

the Young Researcher Grant of National Astronomical Observatories

Chinese Academy of Sciences. The FAST FELLOWSHIP is supported by Special Funding for Advanced Users

budgeted and administrated by Center for Astronomical Mega-Science

Chinese Academy of Sciences(CAMS)


Acknowledgment

This work was supported by the National Natural Science Foundation of China (Grant Nos. 11673039, 11573044, 11673002, 11803051, 11503048, and 11203048), the Youth Innovation Promotion Association CAS, the Open Project Program of the Key Laboratory of FAST, NAOC, Chinese Academy of Sciences, the National Key Research and Development Program of China (Grant No. 2017YFA0402600), the CAS “Light of West China” Program, the Young Researcher Grant of National Astronomical Observatories, Chinese Academy of Sciences. The FAST FELLOWSHIP was supported by the Special Funding for Advanced Users, budgeted and administrated by Center for Astronomical Mega-Science, Chinese Academy of Sciences (CAMS).


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