TRACING THE BIPOLAR OUTFLOW FROM ORION SOURCE I

Journal Article · Sat Oct 10 00:00:00 EDT 2009 · Astrophysical Journal (Online)

DOI:https://doi.org/10.1088/0004-637X/704/1/L25· OSTI ID:21367444

Plambeck, R L; Wright, M C. H. ^[1]; Friedel, D N ^[2]; Widicus Weaver, S L ^[3]; Bolatto, A D; Pound, M W ^[4]; Woody, D P; Lamb, J W; Scott, S L ^[5]

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1. Radio Astronomy Laboratory, 601 Campbell Hall, University of California, Berkeley, CA 94720 (United States)
2. Department of Astronomy, 1002 W. Green St., University of Illinois, Urbana, IL 61801 (United States)
3. Department of Chemistry, Emory University, Atlanta, GA 30322 (United States)
4. Department of Astronomy, University of Maryland, College Park, MD 20742 (United States)
5. Owens Valley Radio Observatory, California Institute of Technology, P.O. Box 968, Big Pine, CA 93513 (United States)

Using CARMA, we imaged the 87 GHz SiO v = 0 J = 2-1 line toward Orion-KL with 0.''45 angular resolution. The maps indicate that radio source I drives a bipolar outflow into the surrounding molecular cloud along a NE-SW axis, in agreement with the model of Greenhill et al. The extended high-velocity outflow from Orion-KL appears to be a continuation of this compact outflow. High-velocity gas extends farthest along a NW-SE axis, suggesting that the outflow direction changes on timescales of a few hundred years.

• OSTI ID: 21367444
• Journal Information: Astrophysical Journal (Online), Vol. 704, Issue 1; Other Information: DOI: 10.1088/0004-637X/704/1/L25; ISSN 1538-4357
• Country of Publication: United States
• Language: English

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