Description of source "05274+3345" from Gomez-Ruiz et al. (2016)

Mol 10 does not present a high level of star formation activity; its IRAS luminosity is 3 × 103Le, but its molecular emission is very weak (Estalella et al. 1993). About 30″ to the east of the IRAS source, centimeter-continuum emission and millimeter-continuum emission reveal a cluster of five proto-stars (the AFGL 5142 region: Hunter et al. 1995, 1999; Zhang et al. 2007). Associated with the continuum cores are at least three bipolar outflows. The main outflow (named outflow A by Zhang et al. 2007) was reported by Hunter et al. (1999) in a north–south direction in SiO emission, but recent millimeter/ submillimeter observations show that at least two additional outflows are present in different directions (Zhang et al. 2007; see Figure 3). Water masers and IR emission are coincident with shocked regions within the outflow lobes (Hunter et al. 1995, 1999; Zhang et al. 2007).

Our VLA observations do not show maser emission near the IRAS source, but masers are found to the east, near the molecular outflows (see Figure 3; also Section 5.6). The positions of the maser components in AFGL 5142 confirm their relation with the outflow lobes, as shown in Figure 3. All maser components seem to be associated with the western lobe of outflow C and possibly the southern, inner part of outflow B.

Despite the positional coincidence with the outflows, the maser velocities are within a few km s −1 of the systemic velocity (−3.8 km s−1), while Zhang et al. (2007) report terminal velocities of 25 km s−1 for outflows B and C. Thus, if the masers participate in the dynamics of the outflows, they should be related to its low-velocity component or the swept-up material.