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Title:
VLBI Observations of Southern Gamma-Ray Sources. III
Authors:
Edwards, P. G.; Ojha, R.; Dodson, R.; Lovell, J. E. J.; Reynolds, J. E.; Tzioumis, A. K.; Quick, J.; Nicolson, G.; Tingay, S. J.
Affiliation:
AA(CSIRO Astronomy and Space Science, ATNF, PO Box 76, Epping, NSW 1710, Australia), AB(NASA, Goddard Space Flight Center, Greenbelt, MD, 20771, USA; Catholic University of America, Washington, DC, 20064, USA; University of Maryland, Baltimore County, 1000 Hilltop Cir, Baltimore, MD 21250, USA), AC(ICRAR, University of Western Australia, Crawley, WA 6009, Australia), AD(School of Physical Sciences, University of Tasmania, Private Bag 37, Hobart, TAS 7001, Australia), AE(CSIRO Astronomy and Space Science, ATNF, PO Box 76, Epping, NSW 1710, Australia), AF(CSIRO Astronomy and Space Science, ATNF, PO Box 76, Epping, NSW 1710, Australia), AG(Hartebeesthoek Radio Astronomy Observatory, Krugersdorp 1740, South Africa), AH(Hartebeesthoek Radio Astronomy Observatory, Krugersdorp 1740, South Africa), AI(ICRAR, Curtin University, Bentley, WA 6845, Australia; Istituto Nazionale di Astrofisica (INAF) - Istituto di Radioastronomia, Via Pietro Gobetti, I-40129 Bologna, Italy)
Publication:
Publications of the Astronomical Society of Australia, Volume 35, id.e009 10 pp. (PASA Homepage)
Publication Date:
02/2018
Origin:
CUP
Astronomy Keywords:
galaxies: active, radio continuum: galaxies
Abstract Copyright:
2018: Astronomical Society of Australia
DOI:
10.1017/pasa.2018.4
Bibliographic Code:
2018PASA...35....9E

Abstract

We report the results of Long Baseline Array observations made in 2001 of ten southern sources proposed by Mattox et al. as counterparts to EGRET >100 MeV gamma-ray sources. Source structures are compared with published data where available and possible superluminal motions identified in several cases. The associations are examined in the light of Fermi observations, indicating that the confirmed counterparts tend to have radio properties consistent with other identifications, including flat radio spectral index, high brightness temperature, greater radio variability, and higher core dominance.
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