Astronomy and Astrophysics – Astronomy
Scientific paper
Jun 2000
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000apj...535..833s&link_type=abstract
The Astrophysical Journal, Volume 535, Issue 2, pp. 833-846.
Astronomy and Astrophysics
Astronomy
84
Ism: H Ii Regions, Ism: Jets And Outflows, Ism: Molecules, Stars: Formation
Scientific paper
We present images of the molecular gas in the IRAS 20126+4104 massive outflow and examine the interaction between the energetic outflowing material and the surrounding molecular cloud. Mosaic interferometric images in CO(1-0), 13CO(1-0), C18O(1-0), C17O(1-0), and millimeter continuum emission are compared with mid-infrared images at 12.5 and 17.9 μm, near-infrared images in the Ks band (2.17 μm) and H2 line emission, and optical Hα and [S II] images. We show that the molecular outflow is approximately 6×104 yr old with a mass of about 50-60 Msolar and mass outflow rate Mf~8×10-4 Msolar yr-1. The driving source is located near the center of the >~300 Msolar molecular cloud, and the mass of the disk plus circumstellar envelope traced by millimeter continuum emission is ~50 Msolar. The outflow appears to be bounded on most sides by higher density gas traced by C18O emission. Shocks identified by H2 and [S II] emission knots follow a NW-SE jet close to the young stellar object and then rotate more north-south along the edges of the CO flow. The most likely interpretation appears to be that the knots trace the working surfaces of a collimated jet that precesses through an angle of ~45°. Possible mechanisms that could produce the jet precession include tidal interactions between the disk and a companion star in a noncoplanar orbit or an anisotropic accretion event that dramatically altered the angular momentum vector of the disk.
Bally John
Shepherd Debra S.
Testi Leonard
Yu Ka Chun
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