  iCOMs are species commonly found in the interstellar medium. They are
believed to be crucial seed species for the build-up of chemical complexity in
star forming regions as well as our own Solar System. Thus, understanding how
their abundances evolve during the star formation process and whether it
enriches the emerging planetary system is of paramount importance. We use data
from the ALMA Large Program FAUST to study the compact line emission towards
the [BHB2007] 11 proto-binary system (sources A and B), where a complex
structure of filaments connecting the two sources with a larger circumbinary
disk has previously been detected. More than 45 CH3OCHO lines are clearly
detected, as well as 8 CH3OCH3 transitions , 1 H2CCO transition and 4 t-HCOOH
transitions. We compute the abundance ratios with respect to CH3OH for CH3OCHO,
CH3OCH3, H2CCO, t-HCOOH (as well as an upper limit for CH3CHO) through a
radiative transfer analysis. We also report the upper limits on the column
densities of nitrogen bearing iCOMs, N(C2H5CN) and N(C2H3CN). The emission from
the detected iCOMs and their precursors is compact and encompasses both
protostars, which are separated by only 0.2" (~ 28 au). The integrated
intensities tend to align with the Southern filament, revealed by the high
spatial resolution observations of the dust emission at 1.3 mm. A PV and 2D
analysis are performed on the strongest and uncontaminated CH3OCH3 transition
and show three different spatial and velocity regions, two of them being close
to 11B (Southern filament) and the third one near 11A. All our observations
suggest that the detected methanol, as well as the other iCOMs, are generated
by the shocked gas from the incoming filaments streaming towards [BHB2007] 11A
and 11B, respectively, making this source one of the few where chemical
enrichment of the gas caused by the streaming material is observed.
