Link between the Optical and Radio Frames from Gaia DR3 Data and VLBI Measurements

V. V. Bobylev

doi:10.1134/s1063773722110032

Bobylev, V. V.

2022-12-01 00:00:00

Based on published data, we have assembled a sample of 126 radio stars with the trigonometric parallaxes and proper motions measured by VLBI and available in the Gaia DR3 catalogue (in fact, Gaia EDR3). Our analysis of the Gaia–VLBI proper motion differences for 84 radio stars based on the model of solid-body mutual rotation has revealed no rotation components differing significantly from zero, \documentclass[12pt]{minimal}\usepackage{amsmath}\usepackage{wasysym}\usepackage{amsfonts}\usepackage{amssymb}\usepackage{amsbsy}\usepackage{mathrsfs}\usepackage{upgreek}\setlength{\oddsidemargin}{-69pt}\begin{document}$$(\omega_{x},\omega_{y},\omega_{z})=(0.06,0.08,{-}0.10)\pm(0.06,0.07,0.08)$$\end{document} mas yr\documentclass[12pt]{minimal}\usepackage{amsmath}\usepackage{wasysym}\usepackage{amsfonts}\usepackage{amssymb}\usepackage{amsbsy}\usepackage{mathrsfs}\usepackage{upgreek}\setlength{\oddsidemargin}{-69pt}\begin{document}$${}^{-1}$$\end{document}. Based on the trigonometric parallax differences for 90 stars, we have obtained a new estimate of the systematic offset between the optical and radio frames, \documentclass[12pt]{minimal}\usepackage{amsmath}\usepackage{wasysym}\usepackage{amsfonts}\usepackage{amssymb}\usepackage{amsbsy}\usepackage{mathrsfs}\usepackage{upgreek}\setlength{\oddsidemargin}{-69pt}\begin{document}$$\Delta\pi={-}0.022\pm 0.017$$\end{document} mas, and showed that the parallax scale factor is close to unity, \documentclass[12pt]{minimal}\usepackage{amsmath}\usepackage{wasysym}\usepackage{amsfonts}\usepackage{amssymb}\usepackage{amsbsy}\usepackage{mathrsfs}\usepackage{upgreek}\setlength{\oddsidemargin}{-69pt}\begin{document}$$b=1.001\pm 0.002$$\end{document}.

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Astronomy Letters Springer Journals

http://www.deepdyve.com/lp/springer-journals/link-between-the-optical-and-radio-frames-from-gaia-dr3-data-and-vlbi-KEX6i4wKOj

$Based on published data, we have assembled a sample of 126 radio stars with the trigonometric parallaxes and proper motions measured by VLBI and available in the Gaia DR3 catalogue (in fact, Gaia EDR3). Our analysis of the Gaia–VLBI proper motion differences for 84 radio stars based on the model of solid-body mutual rotation has revealed no rotation components differing significantly from zero, \documentclass[12pt]{minimal}\usepackage{amsmath}\usepackage{wasysym}\usepackage{amsfonts}\usepackage{amssymb}\usepackage{amsbsy}\usepackage{mathrsfs}\usepackage{upgreek}\setlength{\oddsidemargin}{-69pt}\begin{document}$$(\omega_{x},\omega_{y},\omega_{z})=(0.06,0.08,{-}0.10)\pm(0.06,0.07,0.08)$$\end{document} mas yr\documentclass[12pt]{minimal}\usepackage{amsmath}\usepackage{wasysym}\usepackage{amsfonts}\usepackage{amssymb}\usepackage{amsbsy}\usepackage{mathrsfs}\usepackage{upgreek}\setlength{\oddsidemargin}{-69pt}\begin{document}$${}^{-1}$$\end{document}. Based on the trigonometric parallax differences for 90 stars, we have obtained a new estimate of the systematic offset between the optical and radio frames, \documentclass[12pt]{minimal}\usepackage{amsmath}\usepackage{wasysym}\usepackage{amsfonts}\usepackage{amssymb}\usepackage{amsbsy}\usepackage{mathrsfs}\usepackage{upgreek}\setlength{\oddsidemargin}{-69pt}\begin{document}$$\Delta\pi={-}0.022\pm 0.017$$\end{document} mas, and showed that the parallax scale factor is close to unity, \documentclass[12pt]{minimal}\usepackage{amsmath}\usepackage{wasysym}\usepackage{amsfonts}\usepackage{amssymb}\usepackage{amsbsy}\usepackage{mathrsfs}\usepackage{upgreek}\setlength{\oddsidemargin}{-69pt}\begin{document}$$b=1.001\pm 0.002$$\end{document}.$

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Link between the Optical and Radio Frames from Gaia DR3 Data and VLBI Measurements

Link between the Optical and Radio Frames from Gaia DR3 Data and VLBI Measurements

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Link between the Optical and Radio Frames from Gaia DR3 Data and VLBI Measurements

Link between the Optical and Radio Frames from Gaia DR3 Data and VLBI Measurements

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