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We present observations and analysis of the massive molecular outflowG331.512-0.103, obtained with ALMA band 7, continuing the work from Merello etal. (2013). Several lines were identified in the observed bandwidth, consistingof two groups: lines with narrow profiles, tracing the emission from the coreambient medium; and lines with broad velocity wings, tracing the outflow andshocked gas emission. The physical and chemical conditions, such as density,temperature, and fractional abundances are calculated. The ambient medium, orcore, has a mean density of $\sim 5\times 10^6$ cm$^{-3}$ and a temperature of$\sim 70$ K. The SiO and SO$_2$ emission trace the very dense and hot part ofthe shocked outflow, with values of $n_{\rm H_2}\sim10^9$ cm$^{-3}$ and $T \sim160-200$ K. The interpretation of the molecular emission suggests an expandingcavity geometry powered by stellar winds from a new-born UCHII region,alongside a massive and high-velocity molecular outflow. This scenario, alongwith the estimated physical conditions, is modeled using the 3D geometryradiative transfer code MOLLIE for the SiO(J$=8-7$) molecular line. The mainfeatures of the outflow and the expanding shell are reproduced by the model.

ALMA Observations of the massive molecular outflow G331.512-0.103 II: physical properties, kinematics, and geometry modeling