Catena di distribuzione di LO1 per multifeed banda Q

Realizzazione di PCB splitter a 8 vie per la distribuzione del segnale LO (15.5-16GHz) per 38 mixer di prima conversione del multifeed banda

CONSIDERAZIONI DI PROGETTO PER L’ALLARGAMENTO DI BANDA DEL RICEVITORE MULTIFEED BANDA K DI SRT

Descrizione dell'aggiornamento a tutta banda del ricevitore multifeed in banda K montato all'antenna SRT

Ricevitore multifeed banda 33-50GHz: stima delle prestazioni stand alone e con il collegamento fibra ottica

Nel presente rapporto vengono descritte le prestazioni simulate del ricevitore multifeed 19 beam operante nella banda 33-50 GHz (Q-band) da installare su SRT

DBESM P1 (primo prototipo) Matrice di commutazione

Validazione del prototipo di scheda DBESM: na matrice di commutazione funzionale all'instradamento dei ricevitori ai back-end del sistema osservativo SR

Caratterizzazione della nuova versione del modulo di conversione di frequenza in banda Q 33-50 GHz (Q-CONV)

Misure sui prototipi di convertitore di frequenza per il ricevitore multifeed 33-50GHz per l'antenna SRT

Progetto di sistema per ricevitori e back-end a srt

Si descrive l'architettura di gestione dei ricevitori, attuali e in costruzione, del radio telescopio della Sardegna (SRT) e il loro interfacciamento con tutti i back-end attuali e futuri. Vengono discusse le problematiche insite in questa nuova architettura e le possibili configurazioni, indicando anche quella scelta e i motivi della decisione

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

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 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

Preliminary Characterization of the Digitally Formed Beams of PHAROS2 Phased Array Feed

We describe the beamforming strategy and the preliminary laboratory characterization results of the beam pattern synthesized by the PHAROS2 Phased Array Feed (PAF), a 4-8 GHz PAF with digital beamformer for radio astronomy application. The PAF is based on an array of 10×11 dual-polarization Vivaldi antennas cryogenically cooled at 20 K along with low noise amplification modules (LNAs) cascaded with a multi-channel Warm Section (WS) receiver. We present the beamforming and test procedures used to, respectively digitally synthesize and characterize the PHAROS2 antenna array beam pattern at 6 GHz. The tests of the array were carried out at room temperature by directly connecting 24 antenna elements to the WS and iTPM digital beamformer in a laboratory measurement setup

The Sardinia Radio Telescope Front-Ends

The 64 m diameter Sardinia Radio Telescope (SRT) has recently started an early science program using three cryogenic front-ends covering four bands: P-band (305-410 MHz), L-band (1.3-1.8 GHz), high C-band (5.7-7.7 GHz), K-band (18-26.5 GHz). The L- and the P-bands can be observed simultaneously with a single coaxial receiver installed at the primary focus, while a seven beam K-band receiver and a mono-feed high C-band receiver are installed, respectively at the secondary and beam waveguide focus. Additional front-ends are under construction to further expand the telescope observing capabilities. We report on the design and performance of the front-ends already installed on SRT and give an overview of the new ones to be completed in the near future

Status of the radio receiver system of the Sardina Radio Telescope

In this article, we present the design and performances of the radio receiver system installed at the Sardinia Radio Telescope (SRT). The three radio receivers planned for the first light of the Sardinian Telescope have been installed in three of the four possible focus positions. A dual linear polarization coaxial receiver that covers two frequency bands, the P-band (305-410 MHz) and the L-band (1.3-1.8 GHz) is installed at the primary focus. A mono-feed that covers the High C-band (5.7-7.7 GHz) is installed at the beam waveguide foci. A multi-beam (seven beams) K-band receiver (18- 26.5 GHz) is installed at the Gregorian focus. Finally, we give an overview about the radio receivers, which under test and under construction and which are needed for expanding the telescope observing capabilities