28SiO j=1-0, v=1, 2 & 3 maser emission from AGB stars
Paper i proceeding, 2012

The v=1, 2 J=1–0 and v=1 J=2–1 are intense SiO masers, often mapped in AGB stars. Their distribution displays ring-like structures in the regions close to the star. The distribution of the v=1, 2 J=1–0 masers are similar, but the spots are rarely coincident. The v=1 J=2–1 maser ar-rises, however, from a well separated region. It has been argued that this difference can only be explained by models including overlap of two IR lines of SiO and H2O. The v=3 J=1–0 line is not expected to be affected by any line overlap, and its spot structure should be that predicted by the standard models. Our first results on the relative positions of the three lines are surprising but yet consistent with current models including line overlap.


J. F. Desmurs

Observatorio Astronómico Nacional (OAN)

V. Bujarrabal

Observatorio Astronómico Nacional (OAN)

Michael Lindqvist

Chalmers, Rymd- och geovetenskap, Onsala rymdobservatorium

J. Alcolea

Observatorio Astronómico Nacional (OAN)

R. Soria-Ruiz

Observatorio Astronómico Nacional (OAN)

Per Bergman

Chalmers, Rymd- och geovetenskap, Onsala rymdobservatorium

Proceedings of Science

18248039 (eISSN)

Vol. 2012-October

11th European VLBI Network Symposium and Users Meeting, EVN Symposium 2012
Bordeaux, France,


Meteorologi och atmosfärforskning

Astronomi, astrofysik och kosmologi


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