GCN Circular 21574
D. Kaplan (UWM), T. Murphy (University of Sydney), K. Bannister (CSIRO), C. Lynch (University of Sydney), D. Dobie (University of Sydney) on behalf of the VAST collaboration. Following Bannister et al. (LVC GCN 21559), who reported ATCA detections of a radio source consistent with the position of NGC 4993 that is also seen with the VLA (Alexander et al. LVC GCN 21548), we present upper limits to the radio emission of any source at the position of the potential optical counterpart, SSS17a (Coulter et al., LVC GCN 21529). We fit and subtracted a point-source at the optical position of NGC 4993 (13:09:47.706, -23:23:01.79; Skrutskie et al. 2003, 2MASS Extended Source Catalog). The flux densities were consistent with the values reported by Bannister et al. (LVC GCN 21559). We then measured the rms noise at the position of SSS17a as well as 3 other source-free positions nearby. In all cases there was no detectable emission at the position of SSS17a (9.9 arcsec away), and the noise was essentially identical across all positions. Assuming that all of the emission originates with the center of NGC 4993, our flux density for the galaxy and 3-sigma upper limits to emission at the position of SSS17a are: Frequency NGC 4993 Flux Density 3-sigma Limit for SSS17a 8.5 GHz: 0.66 mJy 120 uJy 10.5 GHz: 0.54 mJy 150 uJy 16.7 GHz: 0.42 mJy 130 uJy 21.2 GHz: 0.34 mJy 140 uJy Thank you to CSIRO staff for supporting these observations.