2006/08/05 by Luis A. Zapata, Paul T. P. Ho, Luis F. Rodriguez +4 · 5 citations
Chemistry · Physics and Astronomy · #Astro and Planetary Science #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Atomic physics #Bipolar outflow #Cluster (spacecraft) #Excited state #Infrared #Line (geometry) #Millimeter #Molecular Spectroscopy and Structure #Molecular cloud #Optoelectronics #Outflow #Physics #Protostar #Silicon #Silicon monoxide #Star formation #Stars #Submillimeter Array #astro-ph
paper · pdf · doi:10.1086/508319
published as Astrophys.J.653:398-408,2006 · Accepted by the Astrophysical Journal
arxiv created 2006/08/05 · openalex publication_date 2006/12/05 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We present high angular resolution (2 8 × 1 7) SiO J = 5 → 4, v = 0 line observations of the OMC 1S region in the Orion Nebula made using the Submillimeter Array (SMA). We detect for the first time a cluster of four compact bipolar and monopolar outflows that show high-, moderate-, and low-velocity gas and appear to be energized by millimeter and infrared sources associated with this region. The SiO molecular outflows are compact (<3500 AU), and in most of the cases, they are located very close to their exciting sources. We thus propose that the SiO thermal emission is tracing the youngest and most highly excited parts of the outflows that cannot be detected by other molecules. Moreover, since the ambient cloud is weak in the SiO line emission, these observations can reveal flows that in other molecular transitions will be confused with the ambient velocity cloud emission. Analysis of their position-velocity diagrams show that some components of these outflows may be driven by wide-angle winds very close to the exciting object. Finally, we find that some of these SiO outflows seem to be the base of powerful Herbig-Haro jets and large-scale molecular flows that emanate from a few arcseconds around this zone. In particular, we find a strongly excited SiO bipolar outflow with a P.A. of ~100° that is likely energized by the luminous (~3 × 10 3 L ☉ ) infrared protostar "B" and could be the base of the remarkable object HH 269.