| CONDENSED MATTER: ELECTRONIC STRUCTURE, ELECTRICAL, MAGNETIC, AND OPTICAL PROPERTIES |
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Pathfinding Pulsar Observations with the CVN Incorporating the FAST |
| Zhen Yan1,5*, Zhiqiang Shen1,5, Peng Jiang2,5, Bo Zhang1,5, Haiyan Zhang2,5, Lang Cui3,5, Jintao Luo4,5, Rurong Chen2, Wu Jiang1,5, Hua Zhang3, De Wu4, Rongbing Zhao1,5, Jianping Yuan3,5, Yue Hu4, Yajun Wu1,5, Bo Xia1, Guanghui Li3, Yongnan Rao4,5, Chenyu Chen3, Xiaowei Wang1,5, Hao Ding1, Yongpeng Liu4, Fuchen Zhang4, and Yongbin Jiang1 |
1Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai 200030, China
2National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China
3Xinjiang Astronomical Observatory, Chinese Academy of Sciences, Urumqi 830011, China
4National Time Service Center, Chinese Academy of Sciences, Xi'an 710600, China
5School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing 100049, China
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| Cite this article: |
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Zhen Yan, Zhiqiang Shen, Peng Jiang et al 2024 Chin. Phys. Lett. 41 117501 |
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Abstract The importance of Very Long Baseline Interferometry (VLBI) for pulsar research is becoming increasingly prominent and receiving more and more attention. We present the pathfinding pulsar observation results with the Chinese VLBI Network (CVN) incorporating the Five-hundred-meter Aperture Spherical radio Telescope (FAST). On MJD 60045 (11th April 2023), PSRs B0919+06 and B1133+16 were observed with the phase-referencing mode in the L-band using four radio telescopes (FAST, TianMa, Haoping, and Nanshan) and correlated with the pulsar binning mode of the distributed FX-style software correlator in Shanghai. After further data processing with the NRAO Astronomical Image Processing System (AIPS), we detected these two pulsars and fitted their current positions with accuracy at the milliarcsecond level. By comparison, our results show significantly better agreement with predicted values based on historical VLBI observations than those with previous timing observations, as pulsar astrometry with the VLBI provides a more direct and model-independent method for accurately obtaining related parameters.
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Received: 01 July 2024
Published: 04 November 2024
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| PACS: |
97.60.Gb
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(Pulsars)
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95.85.-e
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(Astronomical observations (additional primary heading(s) must be chosen with these entries to represent the astronomical objects and/or properties studied))
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95.85.Bh
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(Radio, microwave (>1 mm))
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97.82.Cp
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(Photometric and spectroscopic detection; coronographic detection; interferometric detection)
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