Description of source "G10.29-0.13" from Towner et al. (2017)

Like Cyganowski et al. (2011a), we detect 1.3 cm continuum emission associated with the MIR-bright (MIPSGAL-saturated) source directly to the east of the EGO.

Both the MIR-bright source and the EGO lie on the edge of the W31 H II region G10.32−00.15 (Westerhout 1958; see also the discussion in Cyganowski et al. 2011a). In our image, the 1.3 cm continuum emission partially overlaps the extended 4.5 μm emission of the EGO and so is included in Tables 4 and 6 as an EGO-associated 1.3 cm source (Section 3.1). We note, however, that the morphology of the 1.3 cm continuum differs markedly from that of the extended 4.5 μm emission, and it is unclear if the two are really associated. Indeed, Cyganowski et al. (2011a) deem their 1.3 and 3.6 cm detections to be unrelated (at the higher resolution and poorer sensitivity of those data, there is no overlap in the centimeter continuum and extended 4.5 μm emission). Higher angular resolution and sensitivity continuum observations are needed to verify that there is cm-λ emission directly associated with the EGO.

Unlike most EGOs, G10.29−0.13 lacks a discrete 24 μm counterpart, though it is associated with a 6.7 GHz Class II CH3OH maser (Cyganowski et al. 2009). We do not detect any 25 GHz CH3OH emission coincident with this EGO (Figure 1).

We do detect two 25 GHz CH3OH masers in the field, located ~25² NW and SE of the EGO, respectively, that appear to be distributed along the same line as the 44 GHz Class I CH3OH masers reported in Cyganowski et al. (2009). Neither 25 GHz maser is associated with the 1.3 cm continuum or extended 4.5 μm emission.