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Methanol is a ubiquitous species commonly found in the molecular interstellarmedium. It is also a crucial seed species for the building-up of the chemicalcomplexity in star forming regions. Thus, understanding how its abundanceevolves during the star formation process and whether it enriches the emergingplanetary system is of paramount importance. We used new data from the ALMALarge Program FAUST (Fifty AU STudy of the chemistry in the disk/envelopesystem of Solar-like protostars) to study the methanol line emission towardsthe [BHB2007] 11 protobinary system (sources A and B), where a complexstructure of filaments connecting the two sources with a larger circumbinarydisk has been previously detected. Twelve methanol lines have been detectedwith upper energies in the range [45-537] K along with one 13CH3OH transition.The methanol emission is compact and encompasses both protostars, separated byonly 28 au and presents three velocity components, not spatially resolved byour observations, associated with three different spatial regions, with two ofthem close to 11B and the third one associated with 11A. A non-LTE radiativetransfer analysis of the methanol lines concludes that the gas is hot and denseand highly enriched in methanol with an abundance as high as 1e-5. Usingprevious continuum data, we show that dust opacity can potentially completelyabsorb the methanol line emission from the two binary objects. Although wecannot firmly exclude other possibilities, we suggest that the detected hotmethanol is resulting from the shocked gas from the incoming filamentsstreaming towards [BHB2007] 11 A and B, respectively. Higher spatial resolutionobservations are necessary to confirm this hypothesis.

Hot methanol in the [BHB2007] 11 protobinary system: hot corino versus shock origin? : FAUST V