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Massive molecular clumps fragment into cores where star formation takesplace, hence star-forming studies should be done at different spatial scales.Using near-IR data obtained with Gemini, data of CH3OCHO and CH3CN from theALMA database, observations of HCN, HNC, HCO+, and C2H carried out with ASTE,and CO data from public surveys, we perform a deep study of the YSOG29.86-0.004 at core and clump spatial scales. The near-IR emission shows twonebulosities separated by a dark lane, suggesting a typical disk-jets system,but highly asymmetric. They are likely produced by scattered light in cavitiescarved out by jets on an infalling envelope of material, which also presentline emission of H2 and [FeII]. The presence of the complex molecular speciesobserved with ALMA confirms that we are mapping a hot molecular core. The CH3CNemission concentrates at the position of the dark lane and it appears slightlyelongated from southwest to northeast in agreement with the inclination of thesystem as observed at near-IR. The morphology of the CH3OCHO emission is morecomplex and extends along some filaments and concentrates in knots and clumps,mainly southwards the dark-lane, suggesting that the southern jet isencountering a dense region. The northern jet flows more freely, generatingmore extended features. This is in agreement with the red-shifted molecularoutflow traced by the 12CO J=3-2 line extending towards the northwest and thelack of a blue-shifted outflow. This configuration can be explained byconsidering that the YSO is located at the furthest edge of the molecular clumpalong the line of sight, which is consistent with the position of the source inthe cloud mapped in the C18O J=3-2 line. The detection of HCN, HNC, HCO+, andC2H allowed us to characterize the dense gas at clump scales, yielding resultsthat are in agreement with the presence of a high-mass protostellar object.

Studying star-forming processes at core and clump scales: the case of the young stellar object G29.862-0.0044