Volume 372, Number 1, June II 2001
|Page(s)||281 - 290|
|Published online||15 June 2001|
SiO in G34.26: Outflows and shocks in a high mass star forming region
Astrophysics Group, UMIST, PO Box 88, Sackville Street, Manchester M60 1QD, UK
2 Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
Corresponding author: J. Hatchell, firstname.lastname@example.org
Accepted: 26 March 2001
We have looked for SiO emission as evidence of shocks in the high mass star formation region G34.26+0.15. JCMT, VLA and FCRAO observations show that SiO emission is widespread across the region. The SiO emission highlights a massive, collimated outflow and other regions where stellar winds are interacting with molecular clumps. As in other star forming regions, there is also SiO at ambient velocities which is related to the outflow activity. No strong SiO abundance enhancement was measured in either the outflow or the low velocity gas, though abundances up to 10-8 are possible if the SiO is locally enhanced in clumps and optically thick. SiO emission is not detected from the hot core itself, indicating either that SiO is not strongly enhanced in the hot core or that column densities in the region where grain mantle evaporation has taken place are low. In line of sight spiral arm clouds, we measure a SiO abundance of , consistent with previous estimates for quiescent clouds.
Key words: stars: formation / ISM: abundances / ISM: G34.26+0.15 / ISM: jets and outflows / ISM: molecules / radio lines: ISM
© ESO, 2001
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.