CO and shocked H_2 in the highly collimated outflow from VLA 1623

Details CO and shocked H_2 in the highly collimated outflow from VLA 1623 CO and shocked H_2 in the highly collimated outflow from VLA 1623

Nov 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995mnras.277..193d&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 277, Issue 1, pp. 193-209.

Astronomy and Astrophysics

Astronomy

45

Stars: Formation, Stars: Individual: Vla 1623, Ism: Jets And Outflows, Infrared: Stars, Radio Lines: Stars

Scientific paper

We show large-scale ^12CO and H_2 images of the outflow from the proposed `class 0' young star VLA 1623. Shocked H_2 emission is clearly associated for the first time with this flow. Most of the H_2 lies in compact knots, each of which is downstream from a peak in the high-velocity CO. The total outflow mass derived from the CO data is 0.10 M_solar, most of which lies in the extended blueshifted south-east flow. The outflow in this direction is >=15 arcmin (0.7 pc) in length with an opening angle of <=1.˚6. It can be divided into two regions: the first, within 0.07 pc of the star, has a conical shape. Beyond this radius, the low-velocity CO has a limb-brightened morphology, with a narrower, centrally peaked lane at high velocities; this is indicative of flow along the walls of a cylindrical cavity. We suggest that most expansion of the outflow cavity occurs within the initial 0.07 pc of the source; beyond this, the molecular flow is confined to a cylinder of constant width ~0.03 pc. Comparison of the CO and H_2 results tends to suggest that the north-west side of VLA 1623 may contain two separate flows. The near-infrared continuum image shows the dense cloud around the VLA 1623 source in silhouette against a background nebula. There is no evidence of elongation perpendicular to the outflow direction, and the core has a sharp outer radius of ~0.02 pc, with no evidence of a surrounding lower density accreting envelope. Fits to the radial distribution of extinction indicate a Gaussian rather than shallow power-law density gradient.

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