A rotating molecular jet in Orion

Abstract

We present CO(2-1), ${}^{13}$CO(2-1), CO(6-5), CO(7-6), and SO(6${}_5-5_4$) line observations made with the {\it IRAM 30 m} and {\it APEX} radiotelescopes and the {\it Submillimeter Array} toward the highly collimated and extended southwest lobe of the bipolar outflow {\it Ori-S6} located in the Orion South region. We report, for all these lines, the detection of velocity asymmetries about the flow axis, with velocity differences roughly on the order of 1 km s${}^{-1}$ over distances of about 5000 AU, 4 km s${}^{-1}$ over distances of about 2000 AU, and close to the source of between 7 and 11 km s${}^{-1}$ over smaller scales of about 1000 AU. We interpret these velocity differences as a signature of rotation but also discuss some alternatives which we recognize as unlikely in view of the asymmetries' large downstream continuation. This rotation across the {\it Ori-S6} outflow is observed out to (projected) distances beyond 2.5 $\times$ 10${}^4$ AU from the flow's presumed origin. Comparison of our large-scale and small-scale observations suggests the rotational velocity to decline not faster than 1/R with distance R from the axis; in the innermost few arcsecs an increase of rotational velocity with R is even indicated. The magnetic field lines threading the inner rotating CO shell may well be anchored in a disk of radius $\sim$ 50 AU; the field lines further out need a more extended rotating base.

Accepted by Astronomy and Astrophysics

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