Volume 555, July 2013
|Number of page(s)||6|
|Section||Interstellar and circumstellar matter|
|Published online||02 July 2013|
ALMA detection of the rotating molecular disk wind from the young star HD 163296
Leiden Observatory, Leiden University, PO Box 9513
2300 RA, Leiden, The Netherlands
2 Joint ALMA Observatory, Alonso de Cordova 3107, Vitacura, Santiago, Chile
3 European Southern Observatory, Karl Schwarzschild Str 2, 85748 Garching, Germany
4 Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstrasse 1, 85748 Garching, Germany
5 Academia Sinica Institute of Astronomy and Astrophysics, PO Box 23-141, 10617 Taipei, Taiwan
6 National Astronomical Observatory of Japan (NAOJ), 2-21-1 Osawa, Mitaka, 181-8588 Tokyo, Japan
7 NRAO, 520 Edgemont Road, Charlottesville, VA 22903, USA
8 INAF–Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy
Received: 18 January 2013
Accepted: 4 May 2013
Disk winds have been postulated as a mechanism for angular momentum release in protostellar systems for decades. HD 163296 is a Herbig Ae star surrounded by a disk and has been shown to host a series of HH knots (HH 409) with bow shocks associated with the farthest knots. Here we present ALMA science verification data of CO J = 2–1 and J = 3–2 emission, which are spatially coincident with the blue shifted jet of HH knots, and offset from the disk by −18.6 km s-1. The emission has a double corkscrew morphology and extends more than 10′′ from the disk with embedded emission clumps coincident with jet knots. We interpret this double corkscrew as emission from material in a molecular disk wind, and that the compact emission near the jet knots is being heated by the jet that is moving at much higher velocities. We show that the J = 3–2 emission is likely heavily filtered by the interferometer, but the J = 2–1 emission suffers less due to the larger beam and sensitivity to larger scale structures. Excitation analysis suggests temperatures exceeding 900 K in these compact features, with the wind mass, momentum and energy being of order 10-5 M⊙, 10-4 M⊙ km s-1 and 1040 erg, respectively. The high mass loss rate suggests that this star is dispersing the disk faster than it is funneling mass onto the star.
Key words: stars: pre-main sequence / ISM: jets and outflows / ISM: kinematics and dynamics / stars: individual: HD 163296
© ESO, 2013
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