“Giant Ukrainian Radio Telescope”的意思、由来-开放百科全书

Giant Ukrainian Radio Telescope (GURT, Ukrainian: Гігантський Український Радіотелескоп, ГУРТ) is a low frequency (8-80 MНz) radio telescope which is being developed, built and operated by Institute of Radio Astronomy of National Academy of Sciences of Ukraine (IRA NASU). It is located at S. Y. Braude radio astronomical observatory in Kharkiv oblast of Ukraine. The GURT system is designed to be an extension of Ukrainian T-shaped Radio telescope, second modification (UTR-2) in terms of spatial dimensions and frequency range. The goals of creating this new instrument include enhancement of UTR-2 functional properties and contribution to the progress of low frequency radio astronomy in synergy with other distant instruments.

System overview

GURT is a large phased array composed of many identical subarrays. The basic part of this radio telescope is a square regular subarray made of 25 active dipoles (5×5).^[1]^[2]^[3] The distance between the crossed dipole antenna elements in the subarray is 3.75 m, the suspension height is 1.6 m. The subarray design provides a wide frequency coverage from 8 to 80 MHz, high sensitivity (the galactic background level exceeds their self-noise by more than 7 dB), and high RFI immunity (achieved due to high dynamic range of the dipole amplifier: input IP3 is 30 dBm). The effective area at the central frequency is about 350 m².^[4] The HPBW of a single subarray beam at 40 MHz is about 20.4°. The estimate is consistent with the direct measurements that give 22±2°.^[5] The GURT subarray geometry provides a high filling factor that is important for a number of research tasks.

Phasing inside a subarray is accomplished by analogue devices whereas the phasing between subarrays is planned to be digital. A powerful dedicated digital recorder for the GURT system has been developed at the IRA NASU. It is designed for spectral analysis of a band up to 80 MHz (at a sampling frequency of 160 MHz), with high spectral and temporal resolutions, high dynamic range and several operation modes including real time FFT, waveform recording, auto- and cross-correlation spectral measurements, addition and subtraction regime between the two input channels, normalization, and programmable signal delay.

Current status

Four GURT subarrays have already been installed, equipped, and are operational now.^[6] For now most of the time subarrays are used for radio astronomical observations separately because of limited resources for digital phasing system. It has been found that in spite of comparatively small effective area and sensitivity of the subarray it is possible to observe a number of important astrophysical phenomena in a wide frequency range (8–80 MHz). They have proven their ability to address many radio astronomical problems, e.g. for observations of solar bursts, Jovian Io-related decametric radiation, ionospheric scintillation, emission of pulsars, etc. The presence of large and well-studied UTR-2 at the same observatory opens vast opportunities in antenna testing in the shared frequency range^[7]

Future prospects

GURT, currently under construction, will consist of many (up to 100) identical subarrays. The available area of the S. Y. Braude observatory exceeds one square kilometer. Construction of new subarrays is successive, spanning over a period of time, as resources become available. With increase of number of subarrays and effective area the number of astrophysical problems to be solved by GURT will increase significantly.

Joint simultaneous observations of radio astronomical sources with many instruments all over the world are very important at low frequencies due to many hindering factors. Various RFI conditions, different impact of ionosphere at the site of radio telescope, various configurations and parameters of distant radio telescopes increase significantly the informativity of received signals.

References

1. ^Falkovich, I.S., Konovalenko, A.A., Gridin, A.A., et al.: Wide-band high linearity active dipole for low frequency radio astronomy. Exp. Astron. 32, 127–145 (2011)
2. ^Konovalenko, A.A., Falkovich, I.S., Kalinichenko, N.N., et al.: Thirty-elements active antenna array as a prototype of a huge low-frequency radio telescope. Exp. Astron. 16(3), 149–164 (2005)
3. ^Konovalenko, A.A., Falkovich, I.S., Gridin, A.A., et al.: UWB Active Antenna Array for Low Frequency Radio Astronomy. Proc. of the VI-th Intern. Conf. on Ultrawideband and Ultrashort Impulse Signals (UWBUSIS’12), Sevastopol, Ukraine, 17–21 Sept. 39–43 (2012)
4. ^Konovalenko, A., L. Sodin, V. Zakharenko, P. Zarka, O. Ulyanov, M. Sidorchuk, S. Stepkin et al. "The modern radio astronomy network in Ukraine: UTR-2, URAN and GURT." Experimental Astronomy (2016): 1-38.
5. ^Konovalenko, O.O., Tokarsky, P.L., Yerin, S.N.: Effective Area of Phased Antenna Array of GURT Radio Telescope. Proc. of the VII-th Intern. Conf. on Ultrawideband and Ultrashort Impulse Signals (UWBUSIS’14), Kharkiv, Ukraine, 15–19 Sept. 25–29 (2014)
6. ^Stanislavsky, A.A., Bubnov, I.N., Konovalenko, A.A. et al.: First radio astronomy examination of the lowfrequency broadband active antenna subarray. Advances in Astronomy. ID 517058. 5 p. (2014)
7. ^Zakharenko, V., Yerin, S., Bubnov, I., Vasilieva, I. and Kravtsov, I., 2016, October. Using of pulsar spectra catalogue at frequencies below 80 MHz for astronomical calibration of phased antenna arrays. In Applied Physics and Engineering (YSF), 2016 II International Young Scientists Forum on (pp. 210-213). IEEE.