620083, Ekaterinburg, Lenin str. 51, Russia
e-mail: Svetlana.Salii@usu.ru, Andrej.Sobolev@usu.ru
2University of Tasmania, Hobart, Australia
3Monash University, Clayton, Australia
4Helsinki University, Helsinki, Finland
5Institute of Applied Physics, N.Novgorod, Russia
Abstract:
We present SEST observations of G345.01+1.79 in maser
and `quasi-thermal' lines of CH3OH, lines of SiO, CS and some
other shock tracing molecules. For the first time weak methanol
maser emission was detected at frequencies 165.05 and 165.06 GHz.
The observed `quasi-thermal' CH3OH and SiO (2-1) lines
display pronounced blue wings confined to the G345.01+1.79(S)
position. Velocities of CH3OH and OH maser features lie well
within the wing. So, there is a high probability that interaction
of the wind from the young star with ambient material is
responsible for the creation of masers and production of the blue
non-gaussian wing. Comparison of velocities for `quasi-thermal'
and maser lines shows that the bow shock velocity relative to the
bulk of cloud material is about 10 kms-1. So, most probably we are
dealing with the first clear example of an ultracompact HII region
moving through a molecular cloud. Modelling of CH3OH
`quasi-thermal' emission and consideration of maser profiles
shows that the cloud material is greatly inhomogeneous.
