Gain calibration of phased array feeds

Hayman, Douglas B.; Chippendale, A. P.; Qiao, Rong-Yu; Bunton, John D.; Beresford, Ron; Roberts, P.; Axtens, P.

doi:10.1109/iceaa.2010.5653177

Cited by 4 publications

(3 citation statements)

References 13 publications

(12 reference statements)

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“…The main contribution of the ODC at present is to stop beams from being completely destroyed by phase slopes corresponding to unpredictable delay changes that occur with each full reset of the analogue-to-digital converters (ADCs). With further research it is hoped to use the ODC to temporally stabilise PAF beam (voltage) patterns to better than 1% at the half power points (Hayman et al 2010).…”

Section: On-dish Calibrationmentioning

confidence: 99%

Australian square kilometre array pathfinder: I. system description

Hotan

Bunton

Chippendale

et al. 2021

Publ. Astron. Soc. Aust.

215

159

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In this paper, we describe the system design and capabilities of the Australian Square Kilometre Array Pathfinder (ASKAP) radio telescope at the conclusion of its construction project and commencement of science operations. ASKAP is one of the first radio telescopes to deploy phased array feed (PAF) technology on a large scale, giving it an instantaneous field of view that covers $31\,\textrm{deg}^{2}$ at $800\,\textrm{MHz}$ . As a two-dimensional array of 36 $\times$ 12 m antennas, with baselines ranging from 22 m to 6 km, ASKAP also has excellent snapshot imaging capability and 10 arcsec resolution. This, combined with 288 MHz of instantaneous bandwidth and a unique third axis of rotation on each antenna, gives ASKAP the capability to create high dynamic range images of large sky areas very quickly. It is an excellent telescope for surveys between 700 and $1800\,\textrm{MHz}$ and is expected to facilitate great advances in our understanding of galaxy formation, cosmology, and radio transients while opening new parameter space for discovery of the unknown.

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Section: On-dish Calibrationmentioning

confidence: 99%

Australian square kilometre array pathfinder: I. system description

Hotan

Bunton

Chippendale

et al. 2021

Publ. Astron. Soc. Aust.

215

159

View full text Add to dashboard Cite

show abstract

“…We chose the reference port to be 141 in our numbering system [12]. We use the system described in [13] to measure the relative port responses d j . A source at the vertex of the reflector radiates stable broadband noise at a low level into all the PAF elements.…”

Section: A Techniquementioning

confidence: 99%

Recent developments in measuring signal and noise in phased array feeds at CSIRO

Chippendale

McConnell

Bannister

et al. 2016

2016 10th European Conference on Antennas and Propagation (EuCAP)

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Abstract-We describe recent developments in measuring both signal and noise in phased array feeds for radio astronomy at CSIRO. We introduce new techniques including aperture array noise measurements with beamforming weights matched to a reflector's focal field. Weights are calculated via antenna-range and in-reflector measurements. We also describe the separation of system temperature and aperture efficiency via drift scans.

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“…A copy of the calibration signal is sent directly to the receiver and correlated with the PAF outputs, allowing real-time monitoring of the relative gain and phase for each element. This information can in turn be used to adjust beam weights for maximum pattern stability (Hayman et al 2010). The power of this noise source is kept to an absolute minimum to reduce the possibility of it correlating between adjacent antennas.…”

Section: Pedestal Electronicsmentioning

confidence: 99%

The Australian Square Kilometre Array Pathfinder: System Architecture and Specifications of the Boolardy Engineering Test Array

Hotan¹,

Bunton²,

Harvey-Smith³

et al. 2014

Publ. Astron. Soc. Aust.

130

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This paper describes the system architecture of a newly constructed radio telescope -the Boolardy engineering test array, which is a prototype of the Australian square kilometre array pathfinder telescope. Phased array feed technology is used to form multiple simultaneous beams per antenna, providing astronomers with unprecedented survey speed. The test array described here is a six-antenna interferometer, fitted with prototype signal processing hardware capable of forming at least nine dual-polarisation beams simultaneously, allowing several square degrees to be imaged in a single pointed observation. The main purpose of the test array is to develop beamforming and wide-field calibration methods for use with the full telescope, but it will also be capable of limited early science demonstrations.

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Gain calibration of phased array feeds

Cited by 4 publications

References 13 publications

Australian square kilometre array pathfinder: I. system description

Australian square kilometre array pathfinder: I. system description

Recent developments in measuring signal and noise in phased array feeds at CSIRO

The Australian Square Kilometre Array Pathfinder: System Architecture and Specifications of the Boolardy Engineering Test Array

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