2014A&A...567A..99P

The red MSX source G034.5964-01.0292 (MSXG34), catalogued as a massive young stellar object, was observed in molecular lines with the aim of discovering and studying molecular outflows. We mapped a region of 3'x3' centred at MSXG34 using the Atacama Submillimeter Telescope Experiment in the J=3-2 and HCO⁺ J=4-3 lines with an angular and spectral resolution of 22'' and 0.11km/s. Additionally, public J=1-0 and near-IR UKIDSS data obtained from the Galactic Ring Survey and the WFCAM Sciencie Archive were analysed. We found that the spectra towards the YSO present a self-absorption dip, as is common in star-forming regions, and spectral wings that indicate outflow activity. The HCO⁺ was detected only towards the MSXG34 position at v_LSR∼14.2km/s, in coincidence with the absorption dip and approximately with the velocity of previous ammonia observations. HCO⁺ and NH₃ are known to be enhanced in molecular outflows. When we analysed the spectral wings of the line, we discovered misaligned red- and blue-shifted molecular outflows associated with MSXG34. The near-IR emission shows a cone-like nebulosity composed of two arc-like features related to the YSO, which might be due to a cavity cleared in the circumstellar material by a precessing jet. This can explain the misalignment in the molecular outflows. From the analysis of the J=1-0 data we suggest that the YSO is very likely related to a molecular clump ranging between 10 and 14km/s. This suggests that MSXG34, with an associated central velocity of about 14km/s, may be located in the background of this clump. Thus, the blue-shifted outflow is probably deflected by the interaction with dense gas along the line of sight. From a spectral energy distribution analysis of MSXG34 we found that its central object probably is an intermediate-mass protostar.