An International Survey of Front-end Receivers and Observing Performance of Telescopes for Radio Astronomy

Bolli, Pietro; Orfei, A.; Zanichelli, A.; Prestage, Richard; Tingay, S. J.; Beltrán, M. T.; Burgay, M.; Contavalle, C.; Honma, Mareki; Kraus, A.; Lindqvist, Michael; Pérez, José Antonio López; Marongiu, P.; Minamidani, Tetsuhiro; Vilanova, Santiago; Pisanu, T.; Shen, Zhi-Qiang; Sohn, Bong Won; Stanghellini, C.; Tzioumis, A. K.; Zacchiroli, G.

doi:10.1088/1538-3873/ab1f7e

Cited by 9 publications

(8 citation statements)

References 129 publications

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“…III, and described in [22]- [25]. For a more detailed review of radio astronomy receivers in the international context see [26]. The W-band SRT receiver will observe two polarizations at the same time over a broad instantaneous bandwidth, which will allow the SRT to fill an existing observational gap that will benefit the entire international scientific community.…”

Section: W-band Array For the Srt In The International Contextmentioning

confidence: 99%

Feasibility Study of a W-Band Multibeam Heterodyne Receiver for the Gregorian Focus of the Sardinia Radio Telescope

et al. 2022

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We report on the feasibility study of a W-band multibeam heterodyne receiver for the Sardinia Radio Telescope (SRT), a general purpose fully steerable 64-m diameter antenna located on the Sardinia island, Italy, managed by INAF ("Istituto Nazionale di Astrofisica," Italy). The W-band front-end is placed at the telescope Gregorian focal plane and will detect radio astronomy molecular spectral lines and broadband emission in the 3 mm atmospheric window. The goal specification of the receiver is a 4×4 focal plane array operating in dual-linear polarization with a front-end consisting of feed-horns placed in cascade with waveguide Orthomode Transducers (OMTs) and LNAs (Low Noise Amplifiers) cryogenically cooled at ≈20 K. The instantaneous FoV (Field of View) of the telescope is limited by the shaping of the 64-m primary and 7.9-m secondary mirrors. The cryogenic modules are designed to fit in the usable area of the focal plane and provide high-quality beam patterns with high antenna efficiency across the 70-116 GHz Radio Frequency (RF) band. The FoV covered by the 4×4 array is 2.15×2.15 arcmin 2 , unfilled, with separation between contiguous elements of 43 arcsec. Dual-sideband separation (2SB) down-conversion mixers are placed at the cryostat output and arranged in four four-pixel down-conversion modules with 4-12 GHz Intermediate Frequency (IF) bands (both Upper Side Band and Lower Side Band selectable for any pixel and polarization). The receiver utilizes a mechanical derotator to track the parallactic angle.

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Section: W-band Array For the Srt In The International Contextmentioning

confidence: 99%

Feasibility Study of a W-Band Multibeam Heterodyne Receiver for the Gregorian Focus of the Sardinia Radio Telescope

et al. 2022

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“…The following are some examples of Cassegrain-type reflector designs used on radio telescopes across the world [14]. The Nobeyama Radio Observatory (NRO) in Japan (see figure 5) has operated the Nobeyama Radio Telescope, a 45-meter diameter Cassegrain-modified-Coude reflector radio telescope that operates at frequencies between 20 -116 GHz.…”

Section: Implementation Of Cassegrain-type At Radio Telescopementioning

confidence: 99%

“…VERA and KVN initially collaborated to create KaVA, a joint array, and have since expanded their collaboration to the East-Asian VLBI Network (EAVN) with the Chinese VLBI Network (CVN) and the Japanese VLBI Network (JVN) [14], [16]. KaVa has been operating since 2011 observing at 22 and 43 GHz, and has made some progress in investigations of AGN21 jets, 44 GHz methanol maser emission from major star-forming regions22, and other topics [16].…”

Section: Implementation Of Cassegrain-type At Radio Telescopementioning

confidence: 99%

Study of Cassegrain-type antenna for radio telescope

Sobirin

Nugraha

Haz

et al. 2022

J. Phys.: Conf. Ser.

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There are many critical parameters in the design of a radio telescope, such as antenna gain and antenna resolution. In telecommunications, radar, and radio telescopes, an antenna is a very important component. There are many designs of the antenna, such as dipole array and parabolic antenna. Parabolic antennas also have many sub-reflector and antenna methods that control the radio wave, such as the Cassegrain type. A Cassegrain-type antenna is a parabolic antenna in which the feed antenna is mounted at or behind the surface of the main parabolic reflector dish. For the transmitter system, the beam of radio waves from the feed antenna illuminates the secondary reflector (sub-reflector), which reflects it back to the main reflector dish and then forward to space. The Cassegrain design is widely used in parabolic antennas, for large antennas in satellite ground stations, communication satellites, and radio telescopes. In this paper discusses the design of a Cassegrain-type antenna for radio telescope, basic calculation, diameter size of the main reflector of 20 meters, the diameter size of sub-reflector of 2.5 meters, and frequency of 22 GHz and 43 GHz.

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“…These issues make horn antennas the preferred solution in high frequency transmission systems with respect to planar or wire antennas: horn antennas are generally all metallic and are characterized by a simple geometry, easy construction and excitation [5]. Such features make the horn one of the typical feeds at millimeter-wave (mm-wave) frequency range, as a stand-alone antenna, array element [6] or as feed for a reflector system [7]. At mm-wave, the channel is characterized by a high signal attenuation which limits the long distance transmission capability of a stand alone antenna and requires the applications of large reflector dishes to obtain an high directivity [8].…”

Section: Introductionmentioning

confidence: 99%

An In-Line Coaxial-to-Waveguide Transition for Q-Band Single-Feed-Per-Beam Antenna Systems

et al. 2021

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An in-line transition between a coaxial cable and rectangular waveguide operating in Q-band (33–50 GHz) is presented. The aim of the work is to minimize the modifications in the waveguide to the strictly necessary to overcome the manufacturing issues due to the high frequencies involved. In addition, the transition is compact and it does not increase the space occupation on the transverse section, this suggests its application in horn antennas clusters arrangement. The operating principle consists of both a modal conversion and an impedance matching between the devices. The modal conversion is realized in an intermediate region, where the coaxial penetrates in the waveguide: the device geometry is designed so that the electric field in the transition is a trade-off between the TEM mode of the coaxial and the TE10 of the guide. A shaped waveguide backshort and a reactive air gap in the coaxial cable co-participate to achieve the matching. An optimized Chebyshev stepped transformer completes the transition to fulfil the impedance mismatch with the full waveguide. The design issues and technological aspects are considered. The influences of the feeding pin misalignment, the presence of groove is included in the analysis and these practical aspects are discussed and numerically validated via the scattering parameters analysis of the proposed design. The return loss is higher than 25 dB over the whole Q-band.

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An International Survey of Front-end Receivers and Observing Performance of Telescopes for Radio Astronomy

Cited by 9 publications

References 129 publications

Feasibility Study of a W-Band Multibeam Heterodyne Receiver for the Gregorian Focus of the Sardinia Radio Telescope

Feasibility Study of a W-Band Multibeam Heterodyne Receiver for the Gregorian Focus of the Sardinia Radio Telescope

Study of Cassegrain-type antenna for radio telescope

An In-Line Coaxial-to-Waveguide Transition for Q-Band Single-Feed-Per-Beam Antenna Systems

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