A digital radio interferometric data acquisition system

Grenkov, S. A.; Nosov, E. V.; Fedotov, L. V.; Kol’tsov, N. E.

doi:10.1134/s002044121005009x

Cited by 16 publications

(5 citation statements)

References 1 publication

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“…The example of a synthesized correlation response is presented on figure 10. VGOS mode was also successfully tested in domestic observations with RT-32 antennas, equipped with R1002M DAS [6] as a backend and Mark5B as a recorder.…”

Section: Experimental Results With Mdbementioning

confidence: 99%

“…Until 2015, the network consisted of three 32-meter radio telescopes (RT-32) located in Svetloe, Zelenchukskaya and Badary observatories [2]. The backends of RT-32 include various devices for single-dish observations, mostly radiometric and spectral ones [3][4][5], and VLBI backend R1002M DAS [6], that supports 16 frequency channels with up to 32 MHz bandwidth each and the total output data rate of 2 Gbps. The R1002M DAS allows Quasar VLBI network stations to participate in international VLBI observations within the International VLBI Service (IVS) [7] and the European VLBI Network (EVN) [8], but neither the antenna nor the backend of RT-32 meet the requirements of the actively growing VLBI Global Observing System (VGOS), which is the new global VLBI infrastructure [9].…”

Section: Introductionmentioning

confidence: 99%

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Multifunctional Digital Backend for Quasar VLBI network

Nosov¹,

Marshalov²,

Fedotov³

et al. 2021

J. Inst.

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The new 13-meters radio telescope recently built at Svetloe observatory (Russia) required a backend device that could digitize wideband signals from the receiving system, process the signal appropriately, prepare and transmit the resulting signal to the recorder. The previously existing backends, also used at other radio telescopes of Quasar VLBI network, could not provide compatibility with VGOS (VLBI Global Observing System) requirements. We developed Multifunctional Digital Backend (MDBE) with superior performance, flexibility and functions to equip the new antenna and other radio telescopes of the network with the same backend compatible with both domestic and international systems. The MDBE contains up to 12 input channels with 2 GHz bandwidth, powerful and remotely configurable Field programmable gate arrays (FPGA) for digital signal processing, and optical transceivers with total throughput of 50 Gbps per channel. The digital downconverters implemented in FPGA can form sub channels with 0.5, 2, 4, 8, 16, and 32 MHz bandwidth freely tuned with 10 kHz step. In wideband mode a single channel with 512, 1024 or full 2048 MHz bandwidth can be recorded. The MDBE also supports single-dish applications, such as radiometric and spectrometric observations. The paper presents the results of hardware and firmware development of the system, and the experimental results received with the MDBE in Svetloe observatory.

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Section: Experimental Results With Mdbementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Multifunctional Digital Backend for Quasar VLBI network

Nosov¹,

Marshalov²,

Fedotov³

et al. 2021

J. Inst.

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“…The radio telescope receiving system converted the signal from SHF to an intermediate frequency of 390 MHz. Then, the data acquisition system P1002M [8] converted the signal to video frequencies in the 2 MHz bandwidth from intermediate frequencies. The data were recorded by the Mark5B registration system with two-bit sampling.…”

Section: Observations and Data Processingmentioning

confidence: 99%

3-Way Lunar Radio Ranging Experiment on RT-32 Radio Telescopes

Marshalov

Ping

et al. 2020

Latvian Journal of Physics and Technical Sciences

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Since 2017, the Institute of Applied Astronomy of the Russian Academy of Sciences in cooperation with the National Astronomical Observatories of the Chinese Academy of Sciences has been conducting observations of the Chang’E-3 lander carrier wave signal. The paper presents the features of observation scheduling and results of data processing. High-precision phase radar measurements have been obtained with an instrumental error of 1–2 mm. The deviation of residuals in model calculations does not exceed ± 1 cm. The estimates of CE-3 lander position have been obtained with an accuracy of 0.5’’, 7.4 m and 3.2 m in celenocentric cylindrical longitude, Px and Py coordinates, respectively.

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“…Circular polarization of the signal is reversed after reflection from the plane surface and the maximum power of the reflected signal is expected in the OC polarization, though some of the signal, due to secondary reflections, is received with the same polarization. The received echo is sampled by R1002M Data Acquisition System [2] and recorded by Mark5B. Taking into account the Doppler frequency as a function of time we apply the Fourier transform to the echo time series.…”

Section: Observations and Data Processingmentioning

confidence: 99%