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We investigate the origin of complex organic molecules (COMs) in the gasphase around the low-mass Class~0 protostar NGC1333-IRAS2A, to determine if theCOM emission lines trace an embedded disk, shocks from the protostellar jet, orthe warm inner parts of the protostellar envelope. In the framework of theCALYPSO (Continuum And Lines in Young ProtoStellar Objects) IRAM Plateau deBure survey, we obtained large bandwidth spectra at sub-arcsecond resolutiontowards NGC 1333-IRAS2A. We identify the emission lines towards the centralprotostar and perform Gaussian fits to constrain the size of the emittingregion for each of these lines, tracing various physical conditions and scales.The emission of numerous COMs such as methanol, ethylene glycol, and methylformate is spatially resolved by our observations. This allows us to measure,for the first time, the size of the COM emission inside the protostellarenvelope, finding that it originates from a region of radius 40-100 AU,centered on the NGC 1333-IRAS2A protostellar object. Our analysis shows nopreferential elongation of the COM emission along the jet axis, and thereforedoes not support the hypothesis that COM emission arises from shocked envelopematerial at the base of the jet. Down to similar sizes, the dust continuumemission is well reproduced with a single envelope model, and therefore doesnot favor the hypothesis that COM emission arises from the thermal sublimationof grains embedded in a circumstellar disk. Finally, the typical scale $\sim$60AU observed for COM emission is consistent with the size of the inner envelopewhere $T_{\rm{dust}} > 100$ K is expected. Our data therefore strongly suggestthat the COM emission traces the hot corino in IRAS2A, i.e., the warm innerenvelope material where the icy mantles of dust grains evaporate because theyare passively heated by the central protostellar object.

First results from the CALYPSO IRAM-PdBI survey. II. Resolving the hot corino in the Class 0 protostar NGC 1333-IRAS2A