scholarly journals Noise Temperature of Phased Array Radio Telescope: The Murchison Widefield Array and the Engineering Development Array

2020 ◽  
pp. 1-1
Author(s):  
Daniel C. X. Ung ◽  
Marcin Sokolowski ◽  
Adrian T. Sutinjo ◽  
David B. Davidson
Keyword(s):  
Radio Telescope ◽  
Phased Array ◽  
Noise Temperature ◽  
Engineering Development ◽  
Murchison Widefield Array

scholarly journals NOISE TEMPERATURE OF THE ACTIVE PHASED ARRAY OF THE GURT RADIO TELESCOPE

2018 ◽  
Vol 23 (1) ◽  
pp. 43-59 ◽  
Author(s):  
P. L. Tokarsky ◽  
◽  
A. A. Konovalenko ◽  
S. N. Yerin ◽  
I. N. Bubnov ◽  
...  
Keyword(s):  
Radio Telescope ◽  
Phased Array ◽  
Noise Temperature

scholarly journals The Engineering Development Array: A Low Frequency Radio Telescope Utilising SKA Precursor Technology

2017 ◽  
Vol 34 ◽  
Author(s):  
Randall Wayth ◽  
Marcin Sokolowski ◽  
Tom Booler ◽  
Brian Crosse ◽  
David Emrich ◽  
...  
Keyword(s):  
Radio Telescope ◽  
Low Frequency ◽  
Dipole Antennas ◽  
Modular Architecture ◽  
Low Frequencies ◽  
Square Kilometre Array ◽  
Engineering Development ◽  
Staged Approach ◽  
Murchison Widefield Array ◽  
And Performance

AbstractWe describe the design and performance of the Engineering Development Array, which is a low-frequency radio telescope comprising 256 dual-polarisation dipole antennas working as a phased array. The Engineering Development Array was conceived of, developed, and deployed in just 18 months via re-use of Square Kilometre Array precursor technology and expertise, specifically from the Murchison Widefield Array radio telescope. Using drift scans and a model for the sky brightness temperature at low frequencies, we have derived the Engineering Development Array’s receiver temperature as a function of frequency. The Engineering Development Array is shown to be sky-noise limited over most of the frequency range measured between 60 and 240 MHz. By using the Engineering Development Array in interferometric mode with the Murchison Widefield Array, we used calibrated visibilities to measure the absolute sensitivity of the array. The measured array sensitivity matches very well with a model based on the array layout and measured receiver temperature. The results demonstrate the practicality and feasibility of using Murchison Widefield Array-style precursor technology for Square Kilometre Array-scale stations. The modular architecture of the Engineering Development Array allows upgrades to the array to be rolled out in a staged approach. Future improvements to the Engineering Development Array include replacing the second stage beamformer with a fully digital system, and to transition to using RF-over-fibre for the signal output from first stage beamformers.

scholarly journals Status of the Thai 40-m Radio Telescope

2017 ◽  
Vol 13 (S337) ◽  
pp. 346-347
Author(s):  
Phrudth Jaroenjittichai
Keyword(s):  
Radio Telescope ◽  
Radio Astronomy ◽  
Time Domain ◽  
Phased Array ◽  
Low Frequency ◽  
Great Leap ◽  
Great Leap Forward ◽  
Astronomical Research ◽  
L Band ◽  
K Band

AbstractSince the first light of the 2.4-m Thai National Telescope in 2013, Thailand foresees another great leap forward in astronomy. A project known as “Radio Astronomy Network and Geodesy for Development” (RANGD) by National Astronomical Research Institute of Thailand (NARIT) has been approved for year 2017-2021. A 40-m radio telescope has been planned to operate up to 115-GHz observation with prime-focus capability for low frequency and phased array feed receivers. The telescope’s first light is expected in late 2019 with a cryogenics K-band and L-band receivers. RFI environment at the site has been investigated and shown to be at reasonable level. A 13-m VGOS telescope is also included for geodetic applications. Early single-dish science will focus on time domain observations, such as pulsars and transients, outbursts and variability of maser and AGN sources.

scholarly journals PAFINDER – Searching for FRBs and pulsars using Phased Array Feeds

2017 ◽  
Vol 13 (S337) ◽  
pp. 370-371
Author(s):  
Mateusz Malenta ◽  
Ewan Barr ◽  
Aaron Chippendale ◽  
Xinping Deng ◽  
Daniel George ◽  
...  
Keyword(s):  
Real Time ◽  
Radio Telescope ◽  
Phased Array ◽  
Single Pulse ◽  
Radio Bursts ◽  
Pulse Detection ◽  
Phased Array Feeds

AbstractThe challenges of detecting and localising Fast Radio Bursts in real time can be met with the use of Phased Array Feeds. One such system, capable of creating up to 36 simultaneous beams, is currently being commissioned at the Effelsberg radio telescope in Germany following testing at the 64 m Parkes radio telescope. The PAFINDER (Phased Array Feed FRB Finder) pipeline will be used with this receiver to enable real–time single–pulse detection and localisation.

scholarly journals BEAM-FORMING ERRORS IN MURCHISON WIDEFIELD ARRAY PHASED ARRAY ANTENNAS AND THEIR EFFECTS ON EPOCH OF REIONIZATION SCIENCE

2016 ◽  
Vol 820 (1) ◽  
pp. 44 ◽  
Author(s):  
Abraham R. Neben ◽  
Jacqueline N. Hewitt ◽  
Richard F. Bradley ◽  
Joshua S. Dillon ◽  
G. Bernardi ◽  
...  
Keyword(s):  
Phased Array ◽  
Beam Forming ◽  
Phased Array Antennas ◽  
Array Antennas ◽  
Murchison Widefield Array

scholarly journals Measuring Noise Temperatures of Phased-Array Antennas for Astronomy at CSIRO

2014 ◽  
Vol 31 ◽  
Author(s):  
A. P. Chippendale ◽  
D. B. Hayman ◽  
S. G. Hay
Keyword(s):  
Phased Array ◽  
Signal To Noise Ratio ◽  
Noise Temperature ◽  
Broadband Noise ◽  
Systematic Effect ◽  
Antenna Measurement ◽  
Detailed Model ◽  
Phased Array Antennas ◽  
Array Antennas ◽  
Equivalent Noise Temperature

AbstractWe describe the development of a noise-temperature testing capability for phased-array antennas operating in receive mode from 0.7 GHz to 1.8 GHz. Sampled voltages from each array port were recorded digitally as the zenith-pointing array under test was presented with three scenes: (1) a large microwave absorber at ambient temperature, (2) the unobstructed radio sky, and (3) broadband noise transmitted from a reference antenna centred over and pointed at the array under test. The recorded voltages were processed in software to calculate the beam equivalent noise temperature for a maximum signal-to-noise ratio beam steered at the zenith. We introduced the reference-antenna measurement to make noise measurements with reproducible, well-defined beams directed at the zenith and thereby at the centre of the absorber target. We applied a detailed model of cosmic and atmospheric contributions to the radio sky emission that we used as a noise-temperature reference. We also present a comprehensive analysis of measurement uncertainty including random and systematic effects. The key systematic effect was due to uncertainty in the beamformed antenna pattern and how efficiently it illuminates the absorber load. We achieved a combined uncertainty as low as 4 K for a 40 K measurement of beam equivalent noise temperature. The measurement and analysis techniques described in this paper were pursued to support noise-performance verification of prototype phased-array feeds for the Australian Square Kilometre Array Pathfinder telescope.

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