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Astron. Astrophys. 335, 654-660 (1998)

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29SiO (v =0) and 28SiO (v =1) J =2-1 maser emission from Orion IRc2

A. Baudry 1, F. Herpin 1 and R. Lucas 2

1 Observatoire de l'Université de Bordeaux, BP 89, F-33270 Floirac, France
2 Institut de Radioastronomie Millimétrique, 300 rue de la Piscine, F-38406 Saint Martin d'Hères, France

Received 11 December 1997 / Accepted 31 March 1998


We have observed with the IRAM interferometer at two different epochs and simultaneously the two transitions [FORMULA] and [FORMULA] of 29SiO and 28SiO in Orion IRc2. We have made the first maps of 29SiO [FORMULA] emission from Orion. These maps and properties of the 29SiO spectra attest to maser emission. Our 28SiO maps show the stable ring of maser spots observed in previous works. Combining our own data with published works we derive that the relative motion between the two ridges of the 28SiO emission ring is less than about 0.7 AU/yr over a period of 7 years. On the other hand, the weak high velocity maser features observed around 30 km s-1  seem to move with respect to the stable ring of 28SiO main emission. Our relative 29SiO ([FORMULA]) and 28SiO ([FORMULA]) spot maps show that most 29SiO and 28SiO emission features are closely related but have not the same spatial extent. We conclude that these masers are not excited in the same gas layers in agreement with pumping models which predict that various v state masers peak in different spatial regions. In addition, our maps of [FORMULA] and [FORMULA] emission suggest that local line overlaps due to turbulence and high gas temperature do not play a dominant role in the excitation of 28SiO and 29SiO, although excitation effects resulting from the overlap of Doppler-shifted ro-vibrational lines may still be significant.

Key words: line: profiles – masers – ISM: individual objects: Orion A – radio lines: ISM

Send offprint requests to: A. Baudry, (Baudry@observ.u-bordeaux.fr)

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© European Southern Observatory (ESO) 1998

Online publication: June 18, 1998