tokens: , spflg , and rflag were utilized for flagging bad data. Minimal flagging was necessary for L and X bands, however the S -band data were severely hampered by RFI and five of the eight IFs were almost completely flagged. Los Alamos (LA) was used as the reference antenna, with Pie Town (PT) used when LA was unavailable. Imaging and self-calibration was performed using difmap (Shepherd, Pearson Taylor 1994 ). 3 RESULTS The core of 0313−192 is detected at S band with the LBA, and L, S , and X band with the VLBA. The LBA observations detected an unresolved point source with a flux density of 53.6 ± 8.4 mJy. The longer baselines of the VLBA enabled higher resolution images that were able, at all three observed frequencies, to resolve the radio structure. Table 2 provides a summary of the VLBA data. Table 2. Beam size and flux density measurements for the VLBA observations using different imaging weightings. We assume 10 per cent errors, which is standard for VLBI measurements due to the sparse uv -coverage. 3.1 VLBI detection and chance alignment Keel et al. ( 2006 ) were able to constrain the optical and radio positions to within 0.2 arcsec. The X -band VLBA data provide the best positional information due to the smaller beam size. The error in the radio astrometry is dominated by phase calibration errors, resulting in a positional accuracy of approximately 0.48 mas. As stated in Keel et al. ( 2006 ), the coincidence of the VLBI detections of a compact source with the optical centre of 0313−192 effectively eliminates any possibility of the spiral host and DRAGN being in a chance alignment. A ∼30 mJy compact source detected at L band using the VLBA has a brightness temperature of T b > 10 8 , which can only be attributed to the presence of an AGN. The integrated flux of the naturally weighted S -band source agrees within the errors with the S -band LBA observations from 2009 suggesting little variability on this time-scale. The compact radio detection at the position of the optical host, and the detection of jet components, confirms the presence of an active AGN. 3.2 VLBA-detected core and jet Ledlow et al. ( 2001 ) report an inverted spectral index 1 of the radio core of 0313−192 with , which is common for AGN cores. They also note the steeper inverted spectrum between 1.4 and 4.9 GHz, likely due to either free–free or synchrotron self-absorption. The new VLBA observations confirm the inverted nature of the spectral index of the core. We measure a core spectral index of using the L -, S -, and X -band VLBA measurements of the unresolved radio core. Previously published VLA data of 0313−192 at L and X band suggest the presence of a radio jet to the South of the host galaxy (Ledlow et al. 2001 ). Although the diffuse radio lobes are detected on either side of the host galaxy, the putative jet suggests that the radio jets are oriented with the Southern jet emitting towards the line of sight. We detect components of the Southern jet at L, S , and X
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