Abstract

Aims. 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. Methods. We mapped a region of 3' x 3' centred at MSXG34 using the Atacama Submillimeter Telescope Experiment in the (CO)-C-12 J = 3-2 and HCO+ J = 4-3 lines with an angular and spectral resolution of 22 and 0.11 km s(-1). Additionally, public (CO)-C-13 J = 1-0 and near-IR UKIDSS data obtained from the Galactic Ring Survey and the WFCAM Sciencie Archive were analysed. Results. We found that the (CO)-C-12 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) similar to 14.2 km s(-1), in coincidence with the (CO)-C-12 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 (CO)-C-12 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 (CO)-C-13 J = 1-0 data we suggest that the YSO is very likely related to a molecular clump ranging between 10 and 14 km s(-1). This suggests that MSXG34, with an associated central velocity of about 14 km s(-1), 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.