VLBA Observations of Radio Reference Frame Sources. III. Astrometric Suitability of an Additional 225 Sources

By A. Fey, P. Charlot. 2000

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Superluminal Radio Features in the M87 Jet and the Site of Flaring TeV Gamma-Ray Emission (2007, methodology): “A short 2.3 GHzVLBA observation obtained in Jul. 2004 by the USNO6 (Fey & Charlot 2000) detected only the two brightest features in HST-1 seen in our earlyVLBA images allowing us to trace these structures back by∼1/2 year before our program commenced.”
The VLBA Calibrator Survey—VCS1 (2002, methodology): “The complex effects of undetermined and variable source structure on astrometric positions have been studied recently (Charlot 1990; Fey & Charlot 2000) and may be assessed for the VCS1 in the future using the results of automated imaging and follow–up observations.”
The Measurement of the Light Deflection from Jupiter: Experimental Results (2003, result): “These properties are in agreement with previous observations of J0842 (source names will be abbreviated) and J0839, which show little long-term structure changes (Fey & Charlot 2000; Beasley et al. 2002), whereas J0854 is a known variable source.”
THE SECOND REALIZATION OF THE INTERNATIONAL CELESTIAL REFERENCE FRAME BY VERY LONG BASELINE INTERFEROMETRY (2015, background): “The vast majority of the images for the sources north of about −40◦ declination were obtained from RDV sessions or from earlier VLBA sessions [Fey et al., 1996; Fey & Charlot, 1997, 2000].”