Abstract:
Very Long Baseline Interferometry (VLBI) technique occupies a special place among tools for studying the Universe due to its record high angular resolution. The latter is in the inverse proportion to the length of interferometer baseline at any given wavelength. Until recently, the available angular resolution in radio domain of about 1 milliarcsecond at centimeter wavelengths was limited by the diameter of the Earth. However, many astrophysical problems require a higher angular resolution. The only way to achieve this at a given wavelength is to create an interferometer with the baseline larger than the Earth’s diameter by placing at least one telescope in space. In February 1997, the first dedicated Space VLBI mission, VLBI Space Observatory Program (VSOP), led by the Institute of Space and Astronautical Sciences (Japan) has been launched (Hirabayashi 1997). The VSOP mission opens a new dimension in the development of radio astronomy of extremely high angular resolution and will be followed by other Space VLBI missions. A review of scientific drives and technological challenges of the next generation Space VLBI mission have been discussed, for example, by Gurvits et al. (1996) and Ulvestad et al. (1997).Keywords:
Very-long-baseline interferometry
Radio Astronomy
Angular diameter
Very Long Baseline Interferometry (VLBI) technique occupies a special place among tools for studying the Universe due to its record high angular resolution. The latter is in the inverse proportion to the length of interferometer baseline at any given wavelength. Until recently, the available angular resolution in radio domain of about 1 milliarcsecond at centimeter wavelengths was limited by the diameter of the Earth. However, many astrophysical problems require a higher angular resolution. The only way to achieve this at a given wavelength is to create an interferometer with the baseline larger than the Earth's diameter by placing at least one telescope in space. In February 1997, the first dedicated Space VLBI mission, VLBI Space Observatory Program (VSOP), led by the Institute of Space and Astronautical Sciences (Japan) has been launched (Hirabayashi 1997). The VSOP mission opens a new dimension in the development of radio astronomy of extremely high angular resolution and will be followed by other Space VLBI missions. A review of scientific drives and technological challenges of the next generation Space VLBI mission have been discussed, for example, by (1996) and (1997).
Very-long-baseline interferometry
Angular diameter
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The 26m radio telescope of the Hartebeesthoek Radio Astronomy Observatory (HartRAO) suffered a failure of the main bearing in the polar shaft in 2008 October. This was replaced in 2010 and the telescope returned to service. Very Long Baseline Interferometry (VLBI) restarted in 2010 August. The internet link to other continents operates at 1 GB/s, permitting e-VLBI at this data rate with the European VLBI Network (EVN).
Very-long-baseline interferometry
Radio Astronomy
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Very-long-baseline interferometry
space science
Spitzer Space Telescope
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Very-long-baseline interferometry
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Abstract The Five-hundred-meter Aperture Spherical radio Telescope (FAST) is the largest single-dish radio telescope in the world, and is now being commissioned after the first light in September 2016. Very long baseline interferometry (VLBI) is among the key science topics according to the original design. The FAST VLBI system has been established, and the first VLBI fringe has been successfully obtained. FAST will significantly improve the sensitivity of the existing VLBI networks in the future, and some science projects in need of high sensitivity will benefit from its participation.
Very-long-baseline interferometry
Baseline (sea)
Aperture (computer memory)
Radio Astronomy
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A new mathematical model to estimate the International VLBI Service (IVS) reference point and additional parameters of a Very Long Baseline Interferometry (VLBI) radio telescope was developed by Lösler and Hennes (2008). To verify this analysis procedure a reference point determination was carried out on the 20 m radio telescope at the "Fundamentalstation Wettzell" (Germany) from April to May 2008. This paper describes the terrestrial local survey, the analysis methodology and the results obtained, in particular the accuracy of the determination of the IVS reference point.
Very-long-baseline interferometry
Radio Astronomy
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This article presents the features of creation of the VLBI time scale system of the Zolochiv RT-32 radio telescope in Ukraine. Based on the research results, directions for its further improvement have been determined for transformation into the Precision Time Scale System based on an ensemble (group) of atomic standards. Ways to achieve the characteristics necessary to include the RT-32 radio telescope in the EVN network are considered. In addition, further modernization and transformation into a group time scale will allow the integration of the VLBI Zolochiv RT-32 time scale system into the National Time and Frequency Service.
Very-long-baseline interferometry
Radio Astronomy
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Abstract The radio astronomy satellite HALCA was launched by the Institute of Space and Astronautical Science in 1997 February to participate in Very Long Baseline Interferometry (VLBI) observations with arrays of ground radio telescopes. HALCA is the main element of the VLBI Space Observatory Programme (VSOP), a complex international endeavor involving over 25 ground radio telescopes, five tracking stations and three correlators. Simultaneous observations with HALCA's 8 meter diameter radio telescope and ground radio telescopes synthesize a radio telescope over twice the size of the Earth, enabling the highest resolution 1.6 GHz and 5 GHz images to be made.
Very-long-baseline interferometry
Radio Astronomy
Astronautics
Satellite Tracking
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Very-long-baseline interferometry
Angular diameter
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Very Long Baseline Interferometry (VLBI) technique occupies a special place among tools for studying the Universe due to its record high angular resolution. The latter is in the inverse proportion to the length of interferometer baseline at any given wavelength. Until recently, the available angular resolution in radio domain of about 1 milliarcsecond at centimeter wavelengths was limited by the diameter of the Earth. However, many astrophysical problems require a higher angular resolution. The only way to achieve this at a given wavelength is to create an interferometer with the baseline larger than the Earth’s diameter by placing at least one telescope in space. In February 1997, the first dedicated Space VLBI mission, VLBI Space Observatory Program (VSOP), led by the Institute of Space and Astronautical Sciences (Japan) has been launched (Hirabayashi 1997). The VSOP mission opens a new dimension in the development of radio astronomy of extremely high angular resolution and will be followed by other Space VLBI missions. A review of scientific drives and technological challenges of the next generation Space VLBI mission have been discussed, for example, by Gurvits et al. (1996) and Ulvestad et al. (1997).
Very-long-baseline interferometry
Radio Astronomy
Angular diameter
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