SAKAI N., CECCARELLI C., BOTTINELLI S., SAKAI T. and YAMAMOTO S.
Abstract (from CDS):
Distribution of the CH3 OH (JK= 2K-1K, 96.7 GHz) emission has been investigated toward NGC 1333 IRAS4B, a low-mass Class 0 protostar which harbors a hot corino, with Nobeyama Millimeter Array. The CH3 OH emission is found to be prominent in the shocked region caused by an impact of the molecular outflow from the protostars. The direction of the outflow which is responsible for the shock seems to be opposite to that of a compact outflow known previously in the CO (J = 2-1), HCN (J = 1-0), H2 CO (312-211), and CH3 OH (JK= 7K-6K) emissions, whereas it is the same as that of the faint second outflow found in the H2 CO emission. This double outflow structure can be interpreted most naturally by the existence of more than two protostars in IRAS4B. On the other hand, a centrally condensed component associated apparently with IRAS4B cannot be recognized in our CH3 OH observation. Our observation suggests that, in this source, the CH3 OH (JK= 2K-1_ K_) emission preferentially traces the shocked regions rather than the hot corino around the protostar.