A 3mm band SIS receiver for the Sardinia Radio Telescope

Ladu, A.; Pisanu, T.; Navarrini, A.; Marongiu, P.; Valente, G.

doi:10.1117/12.2056339

Cited by 2 publications

(3 citation statements)

References 3 publications

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“…Some feasibility studies were conducted and the receiver with its original cooling system (based on the helium vessel) and with the upgraded version (explained in the following Section 3.3) were both considered. In [30,31], the results of these studies are reported in detail.…”

Section: Feasibility Study For the Installation On The Gregorian Focu...mentioning

confidence: 99%

“…Since the SRT was designed to cover all frequencies up to 116 GHz, only the 3 mm channel of the ex-PdBI receiver was upgraded and is presented in this work. The original version of the instrument was unsuitable for the SRT and it required significant modifica-tions and refurbishment from the point of view of its structural and logistical characteristics and its electronic control system [30,31].…”

Section: Introductionmentioning

confidence: 99%

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Adaptation of an IRAM W-Band SIS Receiver to the INAF Sardinia Radio Telescope: A Feasibility Study and Preliminary Tests

Ladu,

Schirru,

Ortu

et al. 2023

Sensors

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Radio telescopes are used by astronomers to observe the naturally occurring radio waves generated by planets, interstellar molecular clouds, galaxies, and other cosmic objects. These telescopes are equipped with radio receivers that cover a portion of the radio frequency (RF) and millimetre-wave spectra. The Sardinia Radio Telescope (SRT) is an Italian instrument designed to operate between 300 MHz and 116 GHz. Currently, the SRT maximum observational frequency is 26.5 GHz. A feasibility study and preliminary tests were performed with the goal of equipping the SRT with a W-band (84–116 GHz) mono-feed radio receiver, whose results are presented in this paper. In particular, we describe the adaptation to the SRT of an 84–116 GHz cryogenic receiver developed by the Institute de Radio Astronomie Millimétrique (IRAM) for the Plateau de Bure Interferometer (PdBI) antennas. The receiver was upgraded by INAF with a new electronic control system for the remote control from the SRT control room, with a new local oscillator (LO), and with a new refrigeration system. Our feasibility study includes the design of new receiver optics. The single side band (SSB) receiver noise temperature measured in the laboratory, Trec ≈ 66 K at 86 GHz, is considered sufficiently low to carry out the characterisation of the SRT active surface and metrology system in the 3 mm band.

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Section: Feasibility Study For the Installation On The Gregorian Focu...mentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Adaptation of an IRAM W-Band SIS Receiver to the INAF Sardinia Radio Telescope: A Feasibility Study and Preliminary Tests

Ladu,

Schirru,

Ortu

et al. 2023

Sensors

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show abstract

“…So far, no scientific observations have been conducted with the SRT across the 3 mm atmospheric window. One of the initial INAF goals for the upgrade of the current set of SRT front-ends aimed at constructing a prototype W-band single-pixel receiver [15]- [17] to test the telescope active surface [18] and the metrology system to demonstrate observation capabilities up to the antenna highest design frequency (≈100 GHz). Thus, a W-band single-pixel receiver prototype was adapted and characterized in the laboratory.…”

Section: B Srt Upgrade Program and Pon Grantmentioning

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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A 3mm band SIS receiver for the Sardinia Radio Telescope

Cited by 2 publications

References 3 publications

Adaptation of an IRAM W-Band SIS Receiver to the INAF Sardinia Radio Telescope: A Feasibility Study and Preliminary Tests

Adaptation of an IRAM W-Band SIS Receiver to the INAF Sardinia Radio Telescope: A Feasibility Study and Preliminary Tests

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

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