Astrophys. J., 675, 454-463 (2008/March-1)
The CO molecular outflows of IRAS 16293-2422 probed by the submillimeter array.
YEH S.C.C., HIRANO N., BOURKE T.L., HO P.T.P., LEE C.-F., OHASHI N. and TAKAKUWA S.
Abstract (from CDS):
We have mapped the protobinary source IRAS 16293-2422 in CO 2-1, 13CO 2-1, and CO 3-2 with the Submillimeter Array (SMA). The maps with resolution of 1.5"-5" reveal a single small-scale (∼3000 AU) bipolar molecular outflow along the east-west direction. We found that the blueshifted emission of this small-scale outflow mainly extends to the east and the redshifted emission to the west from the position of IRAS 16293A. A comparison with the morphology of the large-scale outflows previously observed by single-dish telescopes at millimeter wavelengths suggests that the small-scale outflow may be the inner part of the large-scale (∼15,000 AU) east-west outflow. On the other hand, there is no clear counterpart of the large-scale northeast-southwest outflow in our SMA maps. Comparing analytical models to the data suggests that the morphology and kinematics of the small-scale outflow can be explained by a wide-angle wind with an inclination angle of ∼30°-40° with respect to the plane of the sky. The high-resolution CO maps show that there are two compact, bright spots in the blueshifted velocity range. An LVG analysis shows that the one located 1" to the east of source A is extremely dense, n(H2) ∼107/cm3, and warm, Tkin>55 K. The other one located 1" southeast of source B has a higher temperature of Tkin>65 K but slightly lower density of n(H2) ∼10^ 6^/cm3. It is likely that these bright spots are associated with the hot core-like emission observed toward IRAS 16293. Since both bright spots are blueshifted from the systemic velocity and are offset from the protostellar positions, they are likely formed by shocks.
ISM: Individual: Alphanumeric: IRAS 16293-2422 - ISM: Jets and Outflows - Stars: Formation
Fig.2: [YHB2008] IRAS 16293-2422 bN (Nos b1-b2).
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