Solaris is a scientific and technological project aimed at the development of a smart Solar monitoring system at high radio frequencies, based on single-dish imaging techniques. It combines the implementation of dedicated and interchangeable high-frequency receivers on existing small single-dish radio telescope systems (1.5/2.6m class) available in our laboratories and in Antarctica, to be adapted for Solar observations. Solaris can perform Solar imaging observations nearly 20h/day during Antarctic summer with optimal sky opacity, and it will be the only Solar facility offering continuous monitoring at 100GHz. In perspective, our system could be implemented also in the Northern hemisphere to offer unprecedented Solar radio monitoring and imaging for the whole year.
This study focuses on the radiation performance of a system composed of a room-temperature C-band Phased Array Feed (PAF) illuminating the 64-m diameter Sardinia Radio Telescope (SRT) main reflector from its primary focus (f/D=0.328). The PAF, a square array with 8x8 dual-polarized antennas, is the first version of a prototype designed for radio astronomy applications in the framework of an R&D (Research and Development) project of the Italian National Institute for Astrophysics (INAF). To guarantee high sensitivity and low noise temperature, the PAF elements have been designed for an optimum coupling with the SRT main reflector by trading off between maximizing the illumination efficiency and minimizing the spillover. In this paper, first, we present the results of the electromagnetic simulation of the PAF element radiation patterns in the Far Field (FF) region, both by assuming no interaction with the reflector and by taking into account the reflection from the SRT main reflector primary focus; second, we present the performance of the beamformed patterns obtained by applying two different beamforming methods; finally, we assess the aperture blockage effect due to the SRT sub-reflector. Results are shown at three frequencies within the operative band of the C-band PAF, i.e. at 4.5, 5.5 and 6.0 GHz.
We present the control system of the 84-116 GHz (3 mm band) Superconductor-Insulator-Superconductor (SIS)
heterodyne receiver to be installed at the Gregorian focus of the Sardinia Radio Telescope (SRT). The control system is
based on a single-board computer from Raspberry, on microcontrollers from Arduino, and on a Python program for
communication between the receiver and the SRT antenna control software, which remotely controls the backshorttuned
SIS mixer, the receiver calibration system and the Local Oscillator (LO) system.
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