NAVARRINI, AlessandroAlessandroNAVARRINIOLMI, LucaLucaOLMINESTI, RenzoRenzoNESTIORTU, PierluigiPierluigiORTUMARONGIU, PasqualinoPasqualinoMARONGIUORLATI, ANDREAANDREAORLATISCALAMBRA, ALESSANDROALESSANDROSCALAMBRAORFEI, ALESSANDROALESSANDROORFEIRODA, JURIJURIRODACATTANI, ALESSANDROALESSANDROCATTANILeurini, SilviaSilviaLeuriniGOVONI, FEDERICAFEDERICAGOVONIMURGIA, MATTEOMATTEOMURGIACARRETTI, ETTOREETTORECARRETTIFIERRO, DavideDavideFIERROPELLIZZONI, ALBERTO PAOLOALBERTO PAOLOPELLIZZONI2023-05-222023-05-2220222169-3536http://hdl.handle.net/20.500.12386/34174We 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 designed for the telescope Gregorian focal plane and will detect both continuum and molecular spectral lines from astronomical sources and radio emission from the Sun in the 3 mm atmospheric window. The goal specification of the receiver is a $4\times 4$ 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 $\approx $ 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 $4\times 4$ array is $2.15\times 2.15$ arcmin2, unfilled, with separation between contiguous elements of 43 arcsec. Dual-sideband separation (2SB) down-conversion mixers are designed to be 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.ELETTRONICOenArticle10.1109/ACCESS.2022.31534922-s2.0-85125291709https://api.elsevier.com/content/abstract/scopus_id/85125291709https://ieeexplore.ieee.org/document/9718287FIS/05 - ASTRONOMIA E ASTROFISICA