2022A&A...664A.171V

Aims. Methanol is a ubiquitous species commonly found in the molecular interstellar medium. It is also a crucial seed species for the build-up of chemical complexity in star forming regions. Thus, understanding how its abundance evolves during the star formation process and whether it enriches the emerging planetary system is of paramount importance.
Methods. We used new data from the ALMA Large Program FAUST (Fifty AU STudy of the chemistry in the disc/envelope system of solar protostars) to study the methanol line emission towards the [BHB2007] 11 protobinary system (sources A and B), where a complex structure of filaments connecting the two sources with a larger circumbinary disc has previously been detected.
Results. Twelve methanol lines have been detected with upper energies in the [45-537] K range along with one ¹³CH₃OH transition and one methyl formate (CH₃OCHO) line blended with one of the methanol transitions. The methanol emission is compact (FWHM ∼ 0.5'') and encompasses both protostars, which are separated by only 0.2'' (28 au). In addition, the overall methanol line emission presents three velocity components, which are not spatially resolved by our observations. Nonetheless, a detailed analysis of the spatial origin of these three components suggests that they are associated with three different spatial regions, with two of them close to 11B and the third one associated with 11A. A radiative transfer analysis of the methanol lines gives a kinetic temperature of [100-140] K, an H₂ volume density of 10⁶-10⁷ cm^–3 and column density of a few 10¹⁸ cm^–2 in all three components with a source size of ∼0.15''. Thus, this hot and dense gas is highly enriched in methanol with an abundance as high as 10^–5. Using previous continuum data, we show that dust opacity can potentially completely absorb the methanol line emission from the two binary objects.
Conclusions. Although we cannot firmly exclude other possibilities, we suggest that the detected hot methanol is resulting from the shocked gas from the incoming filaments streaming towards [BHB2007] 11A and B, respectively. Higher spatial resolution observations are necessary to confirm this hypothesis.