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.
Measurement campaigns of radio frequency interferences (RFIs) represent a fundamental aspect to optimize data collected by radio astronomical observations. In order to monitor the state of unwanted man-made signals, every radio telescope needs to have a radio frequency map in the frequencies range of its receivers. The Sardinia Aperture Array Demonstrator (SAD) is an Italian aperture array demonstrator composed of prototypical Vivaldi antennas designed to work at frequencies below 500 MHz. The antennas are located at the Sardinia Radio Telescope (SRT) site and they are arranged with a versatile approach that is able to provide different array configurations. In this paper, we present the results of measurement campaigns conducted with the SAD antennas at the SRT observing site with the aim to monitor the evolution of RFI scenario from 2016 to date. The signal acquisition chain and the software tool used for RFI detection are, also, presented.
KEYWORDS: Receivers, Radio telescopes, Cryogenics, Polarization, Oscillators, Waveguides, Interference (communication), Electronic filtering, Linear filtering, L band
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.
G. Valente, P. Marongiu, A. Navarrini, A. Saba, G. Montisci, A. Ladu, T. Pisanu, M. Pili, S. Dessi, A. Uccheddu, N. Iacolina, D. Perrodin, M. Buttu, E. Egron, A. Melis, C. Tiburzi, V. Vacca
Existing radio receivers have a very low noise temperature. To further increase the observation speed, the new generation
of radio receivers use a multi-beam focal plane array (FPA) together with wide bandwidth. In this article, we present the
front-end and cryogenic design of the 7-beam FPA double linear polarization receiver for the 64-m primary focus of the
Sardinia Radio Telescope. At the end of this article, we show the simulated performances of the front-end receiver and
the measurements of the down-conversion section.
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.
G. Valente, G. Serra, F. Gaudiomonte, A. Ladu, T. Pisanu, P. Marongiu, A. Corongiu, A. Melis, M. Buttu, D. Perrodin, G. Montisci, Gi. Mazzarella, E. Egron, N. Iacolina, C. Tiburzi, V. Vacca
The noise temperature of existing radio telescope receivers has actually achieved very low values. In any case, there are other practical ways to increase the observational speed of a single dish antennas without using longer integration time: observe with multi-beam and large bandwidth receiver. In this paper we present the front end and the cryogenic dewar design of the 5 beams FPA double linear polarization receiver for the primary focus of the 64 m Sardinia Radio Telescope.
We present the optical and mechanical design of a 3mm band SIS receiver for the Gregorian focus of the Sardinia Radio Telescope (SRT). The receiver, was designed and built at IRAM and deployed on the IRAM for the Plateau de Bure Interferometer antennas until 2006. Following its decommissioning the receiver was purchased by the INAFAstronomical Observatory of Cagliari with the aim to adapt its optics for test of the performance of the new 64-m diameter Sardinia Radio Telescope (SRT) in the 3 mm band (84 – 116 GHz). The instrument will be installed in the rotating turret inside of the Gregorian focal room of SRT. The dimensions of the focal room, the horn position in the lower side of the cryostat and the vessel for the liquid helium impose very hard constraints to the optical and mechanical mounting structure of the receiver inside the cabin. We present the receiver configuration and how we plan to install it on SRT.
Access to the requested content is limited to institutions that have purchased or subscribe to SPIE eBooks.
You are receiving this notice because your organization may not have SPIE eBooks access.*
*Shibboleth/Open Athens users─please
sign in
to access your institution's subscriptions.
To obtain this item, you may purchase the complete book in print or electronic format on
SPIE.org.
INSTITUTIONAL Select your institution to access the SPIE Digital Library.
PERSONAL Sign in with your SPIE account to access your personal subscriptions or to use specific features such as save to my library, sign up for alerts, save searches, etc.