SiO in G34.26: Outflows and shocks in a high mass star forming region

J. Hatchell, G.A. Fuller, TJ Millar

Research output: Contribution to journalArticlepeer-review

26 Citations (Scopus)


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 out ow 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 out ow activity. No strong SiO abundance enhancement was measured in either the out ow 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 0.4-2 x 10(-10), consistent with previous estimates for quiescent clouds.
Original languageEnglish
Pages (from-to)281-290
Number of pages10
JournalAstronomy and Astrophysics
Issue number1
Publication statusPublished - Jun 2001

ASJC Scopus subject areas

  • Space and Planetary Science


Dive into the research topics of 'SiO in G34.26: Outflows and shocks in a high mass star forming region'. Together they form a unique fingerprint.

Cite this