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We report molecular line observations of the G34.26+0.15/34.24+0.13 complex, which contains a bright molecular core and a proto-B-star. ATCA observations show that both objects are closely associated with 6.7 GHz class II methanol masers. Methanol line series at 96, 157 and 241 GHz towards the protostar position were observed at SEST. Modelling of the methanol data shows that the molecular core embedding protostar is not greatly influenced by the outflow from the young stellar object. Molecular line mapping at Onsala reveals the presence of a cavity and two compact clumps to the southeast of the bright molecular core. The protostar is situated at the edge of one compact clump. It is very likely that the material outflowing from the protostar freely escapes towards the cavity. Comparison of the line profiles of different molecules shows substantial chemical inhomogeneity within the region.

Keywords: ISM:individual (G34.3); Molecules; Radio line:ISM; Star-forming regions

Document Type: Research Article


Affiliations: 1: Astronomical Observatory, Ural State University, 620083 Ekaterinburg, Russia 2: School of Mathematics and Physics, University of Tasmania, Hobart, Tasmania 7001, Australia 3: Institute of Applied Physics, Nizhny Novgorod 603950, Russia 4: Onsala Space Observatory, 439 92 Onsala, Sweden 5: University of Illinois, 1002 W. Green Street, Urbana, Illinois 61801, USA

Publication date: February 1, 2003

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