Design of PHAROS2 Phased Array Feed

Navarrini, A.; Monari, Jader; Scalambra, A.; Melis, A.; Concu, R.; Naldi, G.; Maccaferri, A.; Cattani, A.; Ortu, Pierluigi; Roda, J.; Perini, Federico; Comoretto, G.; Morsiani, M.; Ladu, A.; Rusticelli, Simone; Mattana, A.; Marongiu, P.; Saba, Andrea; Schiaffino, Marco; Carretti, E.; Schillirò, F.; Urru, Enrico; Pupillo, G.; Poloni, M.; Pisanu, T.; Nesti, R.; Muntoni, Giacomo; Adami, K. Zarb; Magro, Alessio; Chiello, Riccardo; Liu, L.; Grainge, Keith; Keith, Michael; Pantaleev, Miroslav; Cappellen, W. van

doi:10.23919/ursi-at-rasc.2018.8471305

Cited by 13 publications

(4 citation statements)

References 6 publications

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“…There are many types of antennas, and the antenna elements used in a PAF array mainly include microstrip antennas (Hay et al 2007), octagonal ring antennas (Zhang & Brown 2011), dipole antennas (Roshi et al 2018), and Vivaldi antennas (Navarrini et al 2018). At present, Australia has developed a fully cooled PAF array for the Parkes 64 m radio telescope, the array element is a rocket type antenna, which is an optimized metal Vivaldi antenna that can achieve a working bandwidth of 0.7-1.98 GHz when applied to the array (Dunning 2022).…”

Section: Selection Of Array Elementsmentioning

confidence: 99%

Development of a Front End Array for Broadband Phased Array Receiver

Wang,

Cao,

et al. 2024

Res. Astron. Astrophys.

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The receiver is a signal receiving device placed at the focus of the telescope. In order to improve the observation efficiency, the concept of phased array receiver has been proposed in recent years, which places a small phased array at the focal plane of the reflector, and flexible pattern and beam scanning functions can be achieved through a beamforming network. If combined with the element multiplexing, all beams within the entire field of view can be observed simultaneously to achieve continuous sky coverage. This article focuses on the front-end array of phased array receiver at 0.7-1.8 GHz for QiTai Telescope, and designs a Vivaldi antenna array of PCB structure with dual line polarization. Each polarization antenna is designed to arrange in a rectangle manner by 11 × 10. Based on the simulation results of the focal field, 32, 18 and 8 elements were selected to form one beam at 0.7, 1.25 and 1.8 GHz. A analog beamforming network was constructed, and the measured gains of axial beam under uniform weighting were 19.32, 13.72 and 15.22 dBi. Combining the beam scanning method of reflector antenna, the pattern test of different position element sets required for PAF beam scanning was carried out under independent array. The pattern optimization at 1.25 GHz was carried out by weighting method of conjugate field matching. Compared with uniform weighting, the gain, sidelobe level, and main beam direction under conjugate field matching have been improved. Although the above test and simulation results are slightly different, which is related to the passive array and laboratory testing condition, the relevant work has accumulated experience in the development of front-end array for phased array receiver, and has good guiding significance for future performance verification after the array is installed on the telescope.

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Section: Selection Of Array Elementsmentioning

confidence: 99%

Development of a Front End Array for Broadband Phased Array Receiver

Wang,

Cao,

et al. 2024

Res. Astron. Astrophys.

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“…Phased arrays can provide quick electronic scanning and flexible beam forming, but large phased arrays are more expensive and sometimes unpractical. The phased array fed reflector (PAFR), which received widespread attention in the radio astronomy community [ 19 , 20 , 21 , 22 ] may become an intermediate option to provide both considerable gain performance and a relatively limited electronic scanning region (usually 20°) and, of course, with lower cost. Generally, PAFR is composed of a reflector and a small phased array antenna on its focal plane, yet various forms of PAFR can be conducted by designing the reflector architectures (center/offset direct-fed, dual reflectors) and feed type (analog/digital phased arrays, switch matrix) [ 23 ].…”

Section: Review On System Designmentioning

confidence: 99%

Towards 100 Gbps over 100 km: System Design and Demonstration of E-Band Millimeter Wave Communication

Zhang

et al. 2022

Sensors

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Long-range E-band communication with fiber-equivalent speed is emerging extensively as a critical technology in the next-generation communication. This paper firstly reviews the relevant progress in recent research. A brief survey is presented on high-speed, long-range E-band communication systems and their relevant techniques that are essential to the link design, including antenna, power amplifier (PA), channel, and digital baseband processing. In the second part, we review our recent field trial of a long-range air-to-ground E-band link, which maintains steady transmission from a slow-moving helium balloon to the ground station with a vertical dimension of 20 km. The improvement directions and future research topics are then discussed.

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“…Only a sub-set of 24 elements of the array with same polarization is populated with cryogenic low noise amplifiers (LNAs), while the non-active elements are terminated into 50 Ω loads. The non-active elements add negligible noise contribution due to their low operating temperature of ≈20 K. The PHAROS upgraded version, PHAROS2 [10], utilizes new components to reduce the system noise temperature, enhance the aperture efficiency and digitize the signals from a sub-array of 24 single-polarization PAF antenna elements that synthesize four independent single polarization beams. PHAROS2 is being developed in the framework of the PAF SKA (Square Kilometer Array) [11] advanced instrumentation program as a technology demonstrator resulting from the international collaboration between the Italian National Institute for Astrophysics (INAF), Jodrell Bank Observatory at the University of Manchester (UK), ASTRON (the Netherlands), the University of Malta (Malta) and the University of Chalmers (Sweden).…”

Section: Introductionmentioning

confidence: 99%

“…Currently, the WS is a necessary piece of hardware for PAFs designed to operate beyond few GHz, as a direct sampling of the RF signal by analog to digital converters (ADCs) is only possible up to several GHz [13]. The existing high-performance ADCs have enough bits of resolution (typically [8][9][10][11][12] to operate in moderate RFI environment, but limited bandwidth and maximum frequency, which makes them suitable solutions for PAFs radio astronomy application up to S-band (or lower frequency), but not yet for 4-8 GHz or beyond. This is likely to change in the near future as the current technology trends of development of ADCs with continuously higher sampling frequency and sufficient bit resolution might soon allow performing direct multichannel RF digitization (through direct sampling or interleaved sampling) of signals from PAF antennas operating at ≈10 GHz and beyond with frequency bandwidths of few GHz.…”

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confidence: 99%

The Room Temperature Multi-Channel Heterodyne Receiver Section of the PHAROS2 Phased Array Feed

et al. 2019

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This paper describes the design, fabrication, and test results of a room temperature multi-channel heterodyne receiver operating across the 2.3–8.2 GHz radio frequency (RF) band. Such a “Warm Section” (WS) receiver is part of phased arrays for reflector observing systems 2 (PHAROS2), a C-band phased array feed (PAF) demonstrator with digital beamformer for radio astronomy application. The WS receiver is cascaded to the PHAROS2 cryostat, which includes an array of Vivaldi antennas with low noise pre-amplification stages. The WS can handle up to 32 RF signals and, for each of them, realizes the operations of filtering, RF amplification and down-conversion from the RF to the 375–650 MHz intermediate frequency (IF). Also, the WS incorporates an IF-to-optical signal conversion through analogue wavelength division multiplexing IF over fiber (IFoF) and fiber-optic transmitters (OTXs). The 32-channel WS receiver consists of four eight-channel WS RF/IF modules, one local oscillator (LO) splitter module and one monitoring and control module, all hosted in a standard 6U × 19-inch rack.

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Design of PHAROS2 Phased Array Feed

Cited by 13 publications

References 6 publications

Development of a Front End Array for Broadband Phased Array Receiver

Development of a Front End Array for Broadband Phased Array Receiver

Towards 100 Gbps over 100 km: System Design and Demonstration of E-Band Millimeter Wave Communication

The Room Temperature Multi-Channel Heterodyne Receiver Section of the PHAROS2 Phased Array Feed

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