2006/11/02 by Thomas Stanke, T. Stanke, J. P. Williams +1 · 3 citations
Chemistry · Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics and Star Formation Studies #Fullerene Chemistry and Applications #astro-ph
paper · pdf · doi:10.1086/510619
published as Astron.J.133:1307-1320,2007 · 16 pages plus 10 figures accepted by AJ, full resolution version available at http://www.eso.org/~tstanke/preprints.html
arxiv created 2006/11/02 · openalex publication_date 2007/02/21 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/31
We present results of 1.3 mm interferometric and single-dish observations of the center of the L1641-N cluster in Orion. Single-dish wide-field continuum and CO(2-1) observations reveal the presence of several molecular outflows driven by deeply embedded protostellar sources. At higher angular resolution, the dominant millimeter source in the cluster center is resolved into a pair of protostars (L1641-N MM1 and L1641-N MM3), each driving a collimated outflow, and a more extended, clumpy core. Low-velocity CO line-wing emission is spread widely over much of the cluster area. We detect and map the distribution of several other molecular transitions ( 13 CO, C 18 O, 13 CS, SO, CH 3 OH, CH 3 CN, and OCS). CH 3 CN and OCS may indicate the presence of a hot corino around L1641-N MM1. We tentatively identify a velocity gradient over L1641-N MM1 in CH 3 CN and OCS, oriented roughly perpendicular to the outflow direction, perhaps indicative of a circumstellar disk. An analysis of the energy and momentum load of the CO outflows, along with the notion that apparently a large volume fraction is affected by the multiple outflow activity, suggests that outflows from a population of low-mass stars might have a significant impact on clustered (and potentially high-mass) star formation.