The AuScope geodetic VLBI array

Lovell, J. E. J.; McCallum, Jamie; Reid, P. B.; McCulloch, P. M.; Baynes, B. E.; Dickey, John M.; Shabala, Stanislav S.; Watson, CS; Titov, Oleg; Ruddick, Ryan; Twilley, R.; Reynolds, C.; Tingay, S. J.; Shield, P.; Adada, R.; Ellingsen, S. P.; Morgan, John S.; Bignall, H. E.

doi:10.1007/s00190-013-0626-3

Cited by 43 publications

(35 citation statements)

References 19 publications

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“…Three 12 m dishes were erected on Australian territory, in Hobart (Hb), Katherine (Ke), and Yarragadee (Yg). They make up the AuScope VLBI network (Lovell et al 2013) that is managed and operated by the University of Tasmania (UTAS). The other new antennas are the Warkworth 12 m antenna in New Zealand (Ww), which is practically identical to the AuScope dishes, and a 15 m telescope (Ht) at the Hartebeesthoek Radio Astronomy Observatory in South Africa (Fig.…”

Section: Introductionmentioning

confidence: 99%

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The AUSTRAL VLBI observing program

Plank

Lovell

McCallum

et al. 2016

J Geod

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The AUSTRAL observing program was started in 2011, performing geodetic and astrometric very long baseline interferometry (VLBI) sessions using the new Australian AuScope VLBI antennas at Hobart, Katherine, and Yarragadee, with contribution from the Warkworth (New Zealand) 12 m and Hartebeesthoek (South Africa) 15 m antennas to make a southern hemisphere array of telescopes with similar design and capability. Designed in the style of the nextgeneration VLBI system, these small and fast antennas allow for a new way of observing, comprising higher data rates and more observations than the standard observing sessions coordinated by the International VLBI Service for Geodesy and Astrometry (IVS). In this contribution, the continuous development of the AUSTRAL sessions is described, leading to an improvement of the results in terms of baseline length repeatabilities by a factor of two since the start of this program. The focus is on the scheduling strategy and increased number of observations, aspects of automated operation, and data logistics, as well as results of the 151 AUSTRAL sessions performed so far. The high number of the AUSTRAL

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Section: Introductionmentioning

confidence: 99%

“…At present, it is equipped with legacy S/X receivers and state-of-the-art back-end and recording systems (Lovell et al 2013). However, the fact that the 12 m dishes are less sensitive than most of the other legacy antennas (usually ≥20 m in diameter) makes them somewhat inferior in today's IVS observing program.…”

Section: Introductionmentioning

confidence: 99%

The AUSTRAL VLBI observing program

Plank

Lovell

McCallum

et al. 2016

J Geod

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“…Observations are made at two radio frequencies (8 and 22 GHz) approximately every two months with the telescopes of the Australian Long Baseline Array (LBA; e.g., Ojha et al 2004) in combination with telescopes in Australia (NASA's Tidbinbilla facility), South Africa, Antarctica, Chile, and New Zealand. The array has been further expanded by the inclusion of one of the antennas of the Australian Square Kilometre Array Pathfinder (ASKAP) array, the Warkworth antenna in New Zealand (see, e.g., Tzioumis et al 2010), and the new AuScope antennas at Yarragadee (Western Australia) and Katherine (Northern Territory; see, e.g., Lovell et al 2013). The dual frequency nature of the VLBI observations yields spectral index maps of parsec-scale jet features.…”

Section: Introductionmentioning

confidence: 99%

Radio and gamma-ray properties of extragalactic jets from the TANAMI sample

Böck

Kadler

Müller

et al. 2016

A&A

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The TANAMI program has been observing parsec-scale radio jets of southern (declination south of −30 • ) γ-ray bright AGN, simultaneously with Fermi/LAT monitoring of their γ-ray emission, via high-resolution radio imaging with Very Long Baseline Interferometry techniques. We present the radio and γ-ray properties of the TANAMI sources based on one year of contemporaneous TANAMI and Fermi/LAT data. A large fraction (72%) of the TANAMI sample can be associated with bright γ-ray sources for this time range. Association rates differ for different optical classes with all BL Lacs, 76% of quasars, and just 17% of galaxies detected by the LAT. Upper limits were established on the γ-ray flux from TANAMI sources not detected by LAT. This analysis led to the identification of three new Fermi sources whose detection was later confirmed. The γ-ray and radio luminosities are related by L γ ∝ L 0.89 ± 0.04 r . The brightness temperatures of the radio cores increase with the average γ-ray luminosity and the presence of brightness temperatures above the inverse Compton limit implies strong Doppler boosting in those sources. The undetected sources have lower γ/radio luminosity ratios and lower contemporaneous brightness temperatures. Unless the Fermi/LAT-undetected blazars are much γ-ray-fainter than the Fermi/LAT-detected sources, their γ-ray luminosity should not be significantly lower than the upper limits calculated here.

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“…The University of Tasmania also operates the AuScope geodetic array of three 12 m telescopes (Lovell et al, 2013). On occasions, elements of the AuScope array have participated in LBA observations at 8.4 GHz.…”

Section: The Telescopesmentioning

confidence: 99%

The Long Baseline Array

Edwards¹,

Phillips²

2015

Publications of The Korean Astronomical Society

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The Long Baseline Array is an array of radio telescopes using the technique of Very Long Baseline Interferometry to achieve milli-arcsecond-scale angular resolution. The core telescopes are located in Australia, with telescopes in New Zealand and South Africa also participating regularly. In this paper the capabilities of the Long Baseline Array are described, and examples of the science undertaken with the array are given.

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The AuScope geodetic VLBI array

Abstract: tematic effects must be further improved to reach the ambitious goals of VLBI2010.

Cited by 43 publications

References 19 publications

The AUSTRAL VLBI observing program

The AUSTRAL VLBI observing program

Radio and gamma-ray properties of extragalactic jets from the TANAMI sample

The Long Baseline Array

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