  Methanol is a ubiquitous species commonly found in the molecular interstellar
medium. It is also a crucial seed species for the building-up of the 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. We used new data from the ALMA
Large Program FAUST (Fifty AU STudy of the chemistry in the disk/envelope
system of Solar-like 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
disk has been previously detected. Twelve methanol lines have been detected
with upper energies in the range [45-537] K along with one 13CH3OH transition.
The methanol emission is compact and encompasses both protostars, separated by
only 28 au and presents three velocity components, not spatially resolved by
our observations, associated with three different spatial regions, with two of
them close to 11B and the third one associated with 11A. A non-LTE radiative
transfer analysis of the methanol lines concludes that the gas is hot and dense
and highly enriched in methanol with an abundance as high as 1e-5. Using
previous continuum data, we show that dust opacity can potentially completely
absorb the methanol line emission from the two binary objects. 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] 11 A and B, respectively. Higher spatial resolution
observations are necessary to confirm this hypothesis.
