Volume 432, Number 1, March II 2005
|Page(s)||161 - 173|
|Section||Interstellar and circumstellar matter|
|Published online||22 February 2005|
Kinematics of H2O masers in high-mass star forming regions
INAF, Osservatorio Astronomico di Cagliari, Loc. Poggio dei Pini, Str. 54, 09012 Capoterra (CA), Italy e-mail: firstname.lastname@example.org
2 Dipartimento di Fisica, Università degli Studi di Cagliari, S.P. Monserrato-Sestu Km 0.7, 09042 Cagliari, Italy
3 Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
4 Istituto di Radioastronomia CNR, via Gobetti 101, 40129 Bologna, Italy
Accepted: 30 October 2004
We have conducted multi-epoch EVN observations of the 22.2 GHz water masers towards four high-mass star forming regions (Sh 2-255 IR, IRAS 23139+5939, WB89-234, and OMC2). The (three) observing epochs span 6 months. In each region, the H2O maser emission likely originates close (within a few hundred AU) to a forming high-mass YSO. Several maser features (~10) have been detected for each source and, for those features persistent over the three epochs, proper motions have been derived. The amplitudes of the proper motions are found to be larger than the range of variation of the line-of-sight velocities and in each of the observed sources the proper motion orientation seems to indicate expansion. The gas kinematics traced by the 22.2 GHz H2O masers is compatible with the shock-excited nature of water maser emission. Three different kinematic models (a spherical expanding shell, a Keplerian rotating disk and a conical outflow) were fitted to the 3-dimensional velocity field of the detected maser features. The results of these fits, together with the comparison of the VLBI maps with the highest-resolution images of the sources in several thermal tracers, suggest that the water maser features most likely trace the inner portion of the molecular outflows detected at much larger scales.
Key words: masers / stars: formation / ISM: kinematics and dynamics / radio lines: ISM
© ESO, 2005
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