A radiointerferometric terminal of the Badary observatory

Ипатов, А. В.; Kol’tsov, N. E.; Fedotov, L. V.

doi:10.1134/s0020441209010060

Cited by 6 publications

(3 citation statements)

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“…An important feature of the focusing system is a slight deflection of the focal axis of the secondary mirror from the rotation axis of the quasi paraboloid of the principal mirror. Such an orientation scheme of the axes allows placement of the primary feeds of the RT [9,10] receivers on a circle with a diameter of ~3 m and provides prompt switch ing of the ranges of received signals via adjustment of the convergent mirror position [3].…”

Section: Purpose and Main Characteristics Of The Radio Telescope Antementioning

confidence: 99%

The RT-32 radio telescope pointing system

et al. 2012

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The new generation multiwave high precision radio telescope (RT) with a 32 m diameter mirror was developed and manufactured within the framework of the project of creating the national Quasar KVO radiointerferometric network [1][2][3][4]. To date, three RTs have been built and actively operate at the Svetloe (Leningrad oblast), Zelenchuk (North Caucasus), and Badary (near lake Baikal) observatories. The RT of the Badary observatory is shown in Fig. 1.The RT is intended for fundamental investigations of celestial objects of different natures within wave length ranges from 1.35 to 21.00 cm [5][6][7][8]. The main element of the RT is the reflector antenna system (AS). The AS was built according to the modified Cas segrain scheme with a quasi parabolic principal mir ror and quasi hyperbolic secondary mirror (conver gent mirror) 4 m in diameter. An important feature of the focusing system is a slight deflection of the focal axis of the secondary mirror from the rotation axis of the quasi paraboloid of the principal mirror. Such an orientation scheme of the axes allows placement of the primary feeds of the RT [9, 10] receivers on a circle with a diameter of ~3 m and provides prompt switch ing of the ranges of received signals via adjustment of the convergent mirror position [3].The rotary support of the AS provides azimuthal and elevation angle rotations. The electrical drive of the principal mirror provides azimuthal and elevation angle displacements of the AS within angles of ±270°a nd 0°-90°, respectively.The AS azimuthal movement is performed along a 40 m diameter circular rail track. The azimuthal drive consists of four paired carriages, each of which is equipped with two pairs of dc motors with different powers.The large weight of the RT 32 structure (>600 t) and the requirements imposed on the dynamic char acteristics of the RT movement determine the param eters of the AS electrical drive and control system.The electrical drive provides high speed displace ments along the azimuthal (up to 1.5 deg/s) and eleva tion angle (up to 1 deg/s) coordinates with accelera tions of up to 0.8 deg/s 2 at the speed up stage [3]. In this case, the AS control system must control the RT movement dynamics so as to ensure the required accu racy, absence of vibrations, and a dynamic but smooth acceleration and deceleration. Impact loads on the RT structure must be excluded. When nonstandard situa tions arise, the safe RT stoppage must be provided.The electrical drive of the AS operates in two modes. The AS is displaced to a specified region using more powerful high speed motors for a maximally rapid change in the orientation of the antenna princi pal mirror upon a change to the next object under observation. The source tracking mode is provided by low speed motors that are enabled after the AS reaches the rated vicinity of the radio source coordi APPLICATION OF COMPUTERS IN EXPERIMENTSAbstract-Quasar-KVO RT 32 radio telescopes of the radio interferometric complex of the Russian Acad emy of Sciences are equipped with unique 32 m diam...

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Section: Purpose and Main Characteristics Of The Radio Telescope Antementioning

confidence: 99%

The RT-32 radio telescope pointing system

et al. 2012

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“…The RT-32 telescope in the "Svetloe" observatory, for example, uses a standard radiometric receiver (RR) comprising a noise generator (NG) for calibration of the reception-amplification channel [11], a video down-converter [12], and an NI-5620 digital spectrum analyzer (Fig. 1).…”

Section: Signal Recording Techniquementioning

confidence: 99%

Method of cosmic radiation recording in spectral lines

Grenkov

Ипатов

Kol’tsov³

2008

Radiophys Quantum El

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We propose a method for recording of energy parameters of cosmic radio emission in spectral lines, differing in the principle of amplitude calibration of the reception-measurement channel. This method does not require the use of additional channels of signal-power measurement and reduces the source observation time required for extraction of a signal from noise and its recording. Radio emission is recorded using a standard high-sensitivity receiver of the RT-32 radio telescope and a digital spectrum analyzer based on the fast Fourier transform. We consider two variants of the recording system: a variant with off-shelf general-purpose spectrum analyzers (e.g., NI-5620), which use PC processors, and a variant with high-speed specialized analyzers based on programmable logical devices. The system with an XC4VLX25 integrated-circuit analyzer is operated in a frequency band of up to 32 MHz and has a minimum response time, which makes it possible to minimize the source observation time. The spectrum recording system developed at the Institute of Applied Astronomy of the Russian Academy of Sciences and "Radioelectronic Technological Equipment Ltd" and supported by a project of the Russian Science Agency was put into service in the "Svetloe" radioastronomical observatory in 2006.

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“…In very long baseline interferometry (VLBI) com plexes, the received radio frequency signals are at first transferred to the video frequency band and further converted into digital data streams for recording and subsequent correlation processing [1,2]. In this case, the spectrum width of the recorded signal is limited by the bandwidth of the video converter (Δf ≤ 16 MHz).…”

Section: Introductionmentioning

confidence: 99%

A data acquisition system of the S/X-wave range of the radio interferometer for the universal time on-line monitoring

et al. 2013

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A system is intended for equipping radio telescopes with antennas of small (12-13 m) diameters, used in the very long baseline interferometers (VLBIs), including universal time on line monitoring interfer ometers. The system operates in S and X wavelength ranges and process up to 8 signals with spectrum widths of up to 512 MHz, converts them into digital sequences with a 1024 MHz clock frequency, and forms data streams in the VLBI Data Interchange Format (VDIF) with a 2048 Mbit/s rate per channel. Data from each channel of the system via the 10G Ethernet interface are transmitted to the data buffering unit for their send ing to the correlation processing center.

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A radiointerferometric terminal of the Badary observatory

Cited by 6 publications

References 0 publications

The RT-32 radio telescope pointing system

The RT-32 radio telescope pointing system

Method of cosmic radiation recording in spectral lines

A data acquisition system of the S/X-wave range of the radio interferometer for the universal time on-line monitoring

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