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The fine-structure line of [OI] at 63micron is an important diagnostic toolin different fields of astrophysics. However, our knowledge of this line relieson observations with low spectral resolution, and the real contribution of eachcomponent (PDR, jet) in complex environment of star-forming regions (SFRs) ispoorly understood. We investigate the contribution of jet and PDR emission, andof absorption to the [OI]63micron line towards the ultra-compact H{\sc ii}region G5.89--0.39 and study its far-IR line luminosity in different velocityregimes through [OI], [CII], CO, OH, and H2O. We mapped G5.89--0.39 in [OI] andin CO(16--15) with the GREAT receiver onboard SOFIA. We observed the centralposition of the source in the OH^2\Pi_{3/2}, J=5/2\toJ=3/2 and ^2\Pi_{1/2},J=3/2\toJ=1/2 lines. These data were complemented with APEX CO(6-5) and CO(7-6)and HIFI maps and single-pointing observations in [CII], H2O, and HF. The [OI]spectra in G5.89--0.39 are severely contaminated by absorptions from theenvelope and from different clouds along the line of sight. Emission isdetected only at HV, clearly associated with the compact north-south outflowstraced by extremely HV low-J CO. The mass-loss rate and energetics of derivedfrom [OI] agree well with estimates from CO, suggesting that the molecularoutflows in G5.89--0.39 are driven by the jet system seen in [OI]. The far-IRline luminosity of G5.89--0.39 is dominated by [OI] at HV; the second coolantin this velocity regime is CO, while [CII], OH and H2O are minor contributorsto the cooling in the outflow. Our study shows the importance ofspectroscopically resolved data of [OI]63micron for using this line asdiagnostic of SFRs. While this was not possible until now, the GREAT receiveronboard SOFIA has recently opened the possibility of detailed studies of thisline to investigate its potential for probing different environments.

Spectroscopically resolved far-IR observations of the massive star-forming region G5.89--0.39