Astronomy and Astrophysics – Astrophysics
Scientific paper
Oct 1998
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998a%26a...338..576o&link_type=abstract
Astronomy and Astrophysics, v.338, p.576-580 (1998)
Astronomy and Astrophysics
Astrophysics
4
Ism: Jets And Outflows, Ism: Clouds, Ism: Herbig-Haro Objects, Ism: Individual Objects: Hh 135/136, Stars: Pre-Main Sequence, Radio Lines: Ism
Scientific paper
We report CO (J=2-1) and (13) CO (J=2-1) observations of the HH 135 and 136 complex, which has been mapped with the SEST radio telescope. The (13) CO (J=2-1) emission does not peak at the IRAS position but about 12{\arcsec} 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_&sun;. 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 \cite{ogura}), 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.
Liljestroem Tarja
Nakano Masahiro
Ogura Katsuo
Sugitani Kenichiro
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