VLBI astrometry of radio stars to link radio and optical Celestial ...
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Shanghai Astronomical Observatory, Chinese Academy of Sciences
, 80 Nandan Road, Shanghai 200030,
P. R. China
University of Chinese Academy of Sciences
, No.19 (A) Yuquan Rd, Shijingshan, Beijing 100049,
P. R. China
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Shanghai Astronomical Observatory, Chinese Academy of Sciences
, 80 Nandan Road, Shanghai 200030,
P. R. China
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Shanghai Astronomical Observatory, Chinese Academy of Sciences
, 80 Nandan Road, Shanghai 200030,
P. R. China
Korea Astronomy and Space Science Institute
, 776 Daedeok-daero, Yuseong-gu, Daejeon 34055,
Republic of Korea
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School of Astronomy and Space Science, Key Laboratory of Modern Astronomy and Astrophysics (Ministry of Education), Nanjing University
, Nanjing 210023,
P. R. China
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Yunnan Observatories, Chinese Academy of Sciences
, Kunming 650216, Yunnan,
P. R. China
Yunnan Key Laboratory of the Solar Physics and Space Science
, Kunming 650216,
P. R. China
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Shanghai Astronomical Observatory, Chinese Academy of Sciences
, 80 Nandan Road, Shanghai 200030,
P. R. China
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Xinjiang Astronomical Observatory, Chinese Academy of Sciences
, 150 Science 1-Street, Urumqi 830011,
P. R. China
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Shanghai Astronomical Observatory, Chinese Academy of Sciences
, 80 Nandan Road, Shanghai 200030,
P. R. China
Search for other works by this author on:
Shanghai Astronomical Observatory, Chinese Academy of Sciences
, 80 Nandan Road, Shanghai 200030,
P. R. China
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Xinjiang Astronomical Observatory, Chinese Academy of Sciences
, 150 Science 1-Street, Urumqi 830011,
P. R. China
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The Gaia celestial reference frame (Gaia-CRF) will benefit from a close assessment with independent methods, such as Very Long Baseline Interferometry (VLBI) measurements of radio stars at bright magnitudes. However, obtaining full astrometric parameters for each radio star through VLBI measurements demands a significant amount of observation time. This study proposes an efficient observing strategy that acquires double-epoch VLBI positions to measure the positions and proper motions of radio stars at a reduced cost. The solution for CRF link compatible with individual VLBI position measurements is introduced, and the optimized observing epoch scheduling is discussed. Applying this solution to observational data yields results sensitive to sample increase or decrease, yet they remain consistently in line with the literature at the 1-σ level. This suggests the potential for improvement with a larger sample size. Simulations for adding observations demonstrate the double-epoch strategy reduces CRF link parameter uncertainties by over 30 % compared to the five-parameter strategy.
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© The Author(s) 2024. Published by Oxford University Press on behalf of Royal Astronomical Society.
This is an Open Access article distributed under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited.
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