Characterization of a Low-Frequency Radio Astronomy Prototype Array in Western Australia

Sutinjo, Adrian; Colegate, T.; Wayth, R. B.; Hall, Peter; Acedo, Eloy de Lera; Booler, T.; Faulkner, A. J.; Lü, Feng; Hurley‐Walker, N.; Juswardy, Budi; Padhi, S.K.; Razavi-Ghods, Nima; Sokołowski, M.; Tingay, S. J.; Vaate, Jan Geralt bij de

doi:10.1109/tap.2015.2487504

Cited by 72 publications

(76 citation statements)

References 37 publications

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“…In FEKO we used a Greens function to implement a finite ground plane modeled over the soil. We used values for the dielectric constant of 3.5 and conductivity of 0.02 S/m because they are based upon the soil measurements made at the MRO for dry conditions reported by Sutinjo et al (2015). In CST we modeled the finite ground plane as a finite sheet in free space.…”

Section: Systematic Error Estimationmentioning

confidence: 99%

Improved measurement of the spectral index of the diffuse radio background between 90 and 190 MHz

Mozdzen¹,

Bowman²,

Monsalve³

et al. 2016

Mon. Not. R. Astron. Soc.

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We report absolutely calibrated measurements of diffuse radio emission between 90 and 190 MHz from the Experiment to Detect the Global EoR Signature (EDGES). EDGES employs a wide beam zenith-pointing dipole antenna centred on a declination of −26.7 • . We measure the sky brightness temperature as a function of frequency averaged over the EDGES beam from 211 nights of data acquired from July 2015 to March 2016. We derive the spectral index, β, as a function of local sidereal time (LST) and find −2.60 > β > − 2.62 ±0.02 between 0 and 12 h LST. When the Galactic Centre is in the sky, the spectral index flattens, reaching β = −2.50 ±0.02 at 17.7 h. The EDGES instrument is shown to be very stable throughout the observations with night-to-night reproducibility of σ β < 0.003. Including systematic uncertainty, the overall uncertainty of β is 0.02 across all LST bins. These results improve on the earlier findings of by reducing the spectral index uncertainty from 0.10 to 0.02 while considering more extensive sources of errors. We compare our measurements with spectral index simulations derived from the Global Sky Model (GSM) of de Oliveira-Costa et al. (2008) and with fits between the Guzmán et al. (2011) 45 MHz andHaslam et al. (1982) 408 MHz maps. We find good agreement at the transit of the Galactic Centre. Away from transit, the GSM tends to over-predict (GSM less negative) by 0.05 < ∆ β = β GSM − β EDGES < 0.12, while the 45-408 MHz fits tend to over-predict by ∆ β < 0.05.

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Section: Systematic Error Estimationmentioning

confidence: 99%

Improved measurement of the spectral index of the diffuse radio background between 90 and 190 MHz

Mozdzen¹,

Bowman²,

Monsalve³

et al. 2016

Mon. Not. R. Astron. Soc.

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“…The authors are with the International Centre for Radio Astronomy Research/Curtin Institute of Radio Astronomy, Curtin University, Bentley, WA 6102, Australia (e-mail: daniel.ung@icrar.org). astronomical observations using similar methods seen in [10]- [12]. The measured T rcv using astronomical observations also includes the effects of mutual coupling.…”

Section: Introductionmentioning

confidence: 99%

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

Ung

Sokołowski

Sutinjo

et al. 2020

IEEE Trans. Antennas Propagat.

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This paper presents a framework to compute the receiver noise temperature (Trcv) of two low-frequency radio telescopes, the Murchison Widefield Array (MWA) and the Engineering Development Array (EDA). The MWA was selected because it is the only operational low-frequency Square Kilometre Array (SKA) precursor at the Murchison Radio-astronomy Observatory, while the EDA was selected because it mimics the proposed SKA-Low station size and configuration. It will demonstrated that the use of an existing power wave based framework for noise characterization of multiport amplifiers is sufficiently general to evaluate Trcv of phased arrays. The calculation of Trcv was done using a combination of measured noise parameters of the low-noise amplifier (LNA) and simulated S-parameters of the arrays. The calculated values were compared to measured results obtained via astronomical observation and both results are found to be in agreement. Such verification is lacking in current literature. It was shown that the receiver noise temperatures of both arrays are lower when compared to a single isolated element. This is caused by the increase in mutual coupling within the array which is discussed in depth in this paper.

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“…More recent work, discussed further below, suggests that the actual level of point source polarization is lower than M13 assumed (Asad et al 2015). It may also be possible to address polarization leakage due to wide-field beams with modest calibration requirements, as demonstrated with the Murchison Widefield Array (MWA, a precursor of SKA, the Square Kilometer Array) (Sutinjo et al 2015a) and ongoing characterization of the SKA prototype antennas (Sutinjo et al 2015b).…”

Section: Introductionmentioning

confidence: 99%

Limits on Polarized Leakage for the PAPER Epoch of Reionization Measurements at 126 and 164 MHz

Moore

Aguirre

Kohn

et al. 2017

ApJ

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Polarized foreground emission is a potential contaminant of attempts to measure the fluctuation power spectrum of highly redshifted 21 cm H I emission from the epoch of reionization. Using the Donald C. Backer Precision Array for Probing the Epoch of Reionization, we present limits on the observed power spectra of all four Stokes parameters in two frequency bands, centered at 126 MHz (z=10.3) and 164 MHz (z=7.66), for a three-month observing campaign of a deployment involving 32 antennas, for which results on the unpolarized power spectrum have been reported at z=7.7 (by Parsons et al.) and at < < z 7.5 10.5 (by Jacobs et al.). The power spectra in this paper are processed in the same way as by those authors, and show no definitive detection of polarized power. This nondetection is consistent with what is known about polarized sources, combined with the suppression of polarized power by fluctuations in the ionospheric rotation measure, which can strongly affect Stokes Q and U. We are able to show that the net effect of polarized leakage is a negligible contribution at the levels of the limits reported by Parsons et al. and Jacobs et al.

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Characterization of a Low-Frequency Radio Astronomy Prototype Array in Western Australia

Cited by 72 publications

References 37 publications

Improved measurement of the spectral index of the diffuse radio background between 90 and 190 MHz

Improved measurement of the spectral index of the diffuse radio background between 90 and 190 MHz

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

Limits on Polarized Leakage for the PAPER Epoch of Reionization Measurements at 126 and 164 MHz

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