CARBON-MONOXIDE OBSERVATIONS OF THE HH 135 136 COMPLEX/

We report CO (J=2-1) and (CO)-C-13 (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 pea k caused by radiation-driven implosion. The mass estimate of the cloud core associated with the HH complex is some 150 Mg. The position-velo city diagram of the. CO (J=2-1) line emission reveals high velocity wi ngs in the vicinity of the power source IRAS 11101-5829. The redshifte d and blueshifted CO wing emission overlaps spatially and shows only a slight indication of bipolarity. This can be explained by a combinati on of a wide opening angle of the molecular outflow and the large beam size compared to its extent. In order to explain the complicated velo city structure reported for the optical outflow (Ogura & Walsh 1992), we propose a model in which the jetlike outflow from IRAS 11101-5829 i s collisionally deflected by the cloud core. This view appears to be s upported by the slight misalignment of HH136 knots and a possible temp erature enhancement around the suspected point of impact.