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The investigation of star forming regions have enormously benefited from therecent advent of the ALMA interferometer. More specifically, the unprecedentedcombination of high-sensitivity and high-angular resolution provided by ALMAallows one to shed light on the jet/disk systems associated with a Sun-likemass protostar. Also astrochemistry enjoyed the possibility to analyze complexspectra obtained using large bandwidths: several interstellar Complex OrganicMolecules (iCOMs; C-bearing species with at least 6 atoms) have been imagedaround protostars. This in turn boosted the study of the astrochemistry at workduring the earliest phases of star formation paving the way to the chemicalcomplexity in planetary systems where Life could emerge. There is mountingevidence that the observations of iCOMs can be used as unique tool to shedlight, on Solar System scales (< 50 au), on the molecular content ofprotostellar disk. The increase of iCOMs abundances occur only under veryselective physical conditions, such as those associated low-velocity shocksfound where the infalling envelope is impacting the rotating accretion disk.The imaging of these regions with simpler molecules such as CO or CS is indeedparadoxically hampered by their high abundances and consequently high lineopacities which do not allow the observers to disentangle all the emittingcomponents at these small scales. In this respect, we review the state-of-theart of the ALMA analysis about the standard Sun-like star forming region inOrion named HH 212. We show (i) how all the physical components involved in theformation of a Sun-like star can be revealed only by observing differentmolecular tracers, and (ii) how the observation of iCOMs emission, observed toinfer the chemical composition of star forming regions, can be used also asunique tracer to image protostellar disks on Solar System scales.

The HH 212 interstellar laboratory: astrochemistry as a tool to reveal protostellar disks on Solar System scales around a rising Sun