Notes. ⁽⁰⁾ The source name starts with J when detected with the VLA, either in this study or in Dzib et al. (2013). The rest of the name correspond to the J2000 RA-Dec coordinates hhmmss.ss-ddmmss.s. When undetected with VLA, we used the coordinates given in the references listed in Col. 8. ⁽¹⁾The fluxes measured at 10.0 GHz were derived with Gaussian fit. The uncertainties correspond to the fit uncertainties only. The fluxes measured at 4.5 and 7.5 GHz come from Dzib et al. (2013), while the ones at 107 GHz come from Kirk et al. (2017). It should be noted that the flux measured at 107 GHz for J162626.31-242 430.7 and J162626.39-242 430.8 includes the two sources. The upper limits correspond to the 3σ levels (1σ = 17 μJy beam⁻¹ for both frequencies) measured in the three-epoch combined images from Dzib et al. (2013). ⁽²⁾ The source is either YSO (Young Stellar Object) or EG (Extragalactic candidate). The YSOs are classified into: PC (prestellar core), 0 (Class 0 protostar), I (Class I protostar), FS (Flat Spectrum), II (Class II protostar), III (Class III protostar), U (Unknown classification for the YSO candidates). ⁽⁴⁾ Variability taken from Dzib et al. (2013). A source is considered variable when its variability fraction is ≥25%. Legend: Y – variable; N – not variable; U – unknown. ⁽⁵⁾X-ray luminosity in the 0.5–9.0 keV (Imanishi et al. 2003). ⁽⁶⁾This source could be a binary. The flux given here corresponds to the total flux. ⁽⁷⁾ Contrary to the othersources, the fluxes of these objects were integrated over a circular area selected with CASA due to their particular structure, which may be caused by residual phase errors, or due to a very uncertain Gaussian fit. ⁽⁸⁾ This source may be a young star or an outflow knot feature. ⁽⁹⁾This source was proposed to contain an extremely young, deeply embedded protostellar object (Friesen et al. 2014). ⁽¹⁰⁾ Source variable only at the indicated frequency. ⁽¹¹⁾Source only detected in epoch 3 with a flux of 0.4 Jy.

References. ⁽³⁾ References for the YSOclassification : (a) Dzib et al. (2013), (b) Friesen et al. (2014), (c) Wilking et al. (2008), (d) Hsieh & Lai (2013), (e) Kruger et al. (2012), (f) Jørgensen et al. (2008), (g) Evans et al. (2009).