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Astron. Astrophys. 338, 576-580 (1998)

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Carbon monoxide observations of the HH 135/136 complex

K. Ogura 1, M. Nakano 2, K. Sugitani 3 and T. Liljeström 4, 5

1 Kokugakuin University, Higashi, Shibuya-ku, Tokyo 150-8440, Japan (ogura@kokugakuin.ac.jp)
2 Oita University, Oita 870-1192, Japan (mnakano@cc.oita-u.ac.jp)
3 Institute of Natural Sciences, Nagoya-City University, Mizuho-ku, Nagoya 467-0862, Japan (sugitani@nsc.nagoya-cu.ac.jp)
4 Metsahovi Radio Research Station, Helsinki University of Technology, Otakaari 5.A, FIN-02150 Espoo, Finland (tarja.liljestrom@hut.fi)
5 Observatory, P.O. Box 14, FIN-00014 University of Helsinki, Finland

Received 10 March 1998 / Accepted 30 June 1998


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 [FORMULA] 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 [FORMULA]. 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 1992), 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.

Key words: ISM: jets and outflows – ISM: clouds – ISM: Herbig-Haro objects – ISM: individual objects: HH 135/136 – stars: pre-main sequence – radio lines: ISM

Send offprint requests to: K. Ogura

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© European Southern Observatory (ESO) 1998

Online publication: September 14, 1998