The Qitai radio telescope
Na WangQian XuJun MaZhiyong LiuQi LiuHailong ZhangXin PeiMaozheng ChenR. N. ManchesterKejia LeeXingwu ZhengHans KärcherWulin ZhaoHongwei LiDongwei LiMartin SüßMatthias ReichertZhongyi ZhuCongsi WangMingshuai LiRui LiNing LiGuljaina KazezkhanW. M. YanGang WuLang CuiMing ZhangHaitao Li
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Very-long-baseline interferometry
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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).
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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.
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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.
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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.
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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.
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Abstract We present Arecibo 327 MHz confirmation and follow-up studies of seven new pulsars discovered by the Five-hundred-meter Aperture Spherical radio Telescope (FAST). These pulsars are discovered in a pilot program of the Commensal Radio Astronomy FAST Survey (CRAFTS) with the ultra-wide-bandwidth commissioning receiver. Five of them are normal pulsars and two are extreme nulling slow pulsars. PSR J2111+2132’s dispersion measure(DM: 78.5 pc cm −3 ) is above the upper limits of the two Galactic free electron density models, NE2001 and YMW16, and PSR J2057+2133’s position is out of the Scutum-Crux Arm, making them uniquely useful for improving the Galactic free electron density model in their directions. We present a detailed single pulse analysis for the slow nulling pulsars. We show evidence that PSR J2323+1214’s main pulse component follows a non-Poisson distribution and marginal evidence for a sub-pulse-drift or recurrent period of 32.3±0.4 rotations from PSR J0539+0013. We discuss the implication of our finding to the pulsar radiation mechanism.
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The Chinese Very Long Baseline Interferometry (VLBI) network (CVN) is a synthetic aperture radio telescope with the equivalent diameter up to 3000 Km. Through the electronic VLBI (e-VLBI) technology, the four stations and the data processing center are connected by the high speed network. e-CVN is a multi-purpose e-science platform with the merit of quick response ability. e-CVN has been successfully used in the near-real time critical lunar probe tracking missions. Besides, results of the preliminary e-CVN experimental investigations with the aim of rapid radio source mapping and rapid UT1 measurement are presented.
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With the establishment of the AUT University 12m radio telescope at Warkworth, New Zealand has now become a part of the international Very Long Baseline Interferometry (VLBI) community. A major product of VLBI observations are images in the radio domain of astronomical objects such as Active Galactic Nuclei (AGN). Using large geographical separations between radio antennas, very high angular resolution can be achieved. Detailed images can be created using the technique of VLBI Earth Rotation Aperture Synthesis. We review the current process of VLBI radio imaging. In addition we model VLBI configurations using the Warkworth telescope, AuScope (a new array of three 12m antennas in Australia) and the Australian Square Kilometre Array Pathfinder (ASKAP) array currently under construction in Western Australia, and discuss how the configuration of these arrays affects the quality of images. Recent imaging results that demonstrate the modeled improvements from inclusion of the AUT and first ASKAP telescope in the Australian Long Baseline Array (LBA) are presented.
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