1998A&A...338..576O

We report CO (J=2-1) and ¹³CO (J=2-1) observations of the HH 135 and 136 complex, which has been mapped with the SEST radio telescope. The ¹³CO (J=2-1) emission does not peak at the IRAS position but about 12" away from it, probably due to a displacement of the density peak caused by radiation-driven implosion. The mass estimate of the cloud core associated with the HH complex is some 150 M_☉. The position-velocity diagram of the CO (J=2-1) line emission reveals high velocity wings in the vicinity of the power source IRAS 11101-5829. The redshifted and blueshifted CO wing emission overlaps spatially and shows only a slight indication of bipolarity. This can be explained by a combination of a wide opening angle of the molecular outflow and the large beam size compared to its extent. In order to explain the complicated velocity structure reported for the optical outflow (Ogura & Walsh, 1992ApJ...400..248O) we propose a model in which the jetlike outflow from IRAS 11101-5829 is collisionally deflected by the cloud core. This view appears to be supported by the slight misalignment of HH136 knots and a possible temperature enhancement around the suspected point of impact.