Submillimeter emission from the hot molecular jet HH 211

A. Palau, P. T.P. Ho, Q. Zhang, R. Estalella, N. Hirano, H. Shang, C. F. Lee, T. L. Bourke, H. Beuther, Y. J. Kuan

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    49 Citations (Scopus)

    Abstract

    We observed the HH 211 jet in the submillimeter continuum and the CO (3-2) and SiO (8-7) transitions with the Submillimeter Array. The continuum source detected at the center of the outflow shows an elongated morphology, perpendicular to the direction of the outflow axis. The high-velocity emission of both molecules shows a knotty and highly collimated structure. The SiO (8-7) emission at the base of the outflow, close to the driving source, spans a wide range of velocities, from -20 up to 40 km s-1. This suggests that a wide-angle wind may be the driving mechanism of the HH 211 outflow. For distances ≥5″ (∼1500 AU) from the driving source, emission from both transitions follows a Hubble-law behavior, with SiO (8-7) reaching higher velocities than CO (3-2) and being located upstream of the CO (3-2) knots. This indicates that the SiO (8-7) emission is likely tracing entrained gas very close to the primary jet, while the CO (3-2) is tracing less dense entrained gas. From the SiO (5-4) data of Hirano et al., we find that the SiO (8-7)/SiO (5-4) brightness temperature ratio along the jet decreases for knots far from the driving source. This is consistent with the density decreasing along the jet, from (3-10) × 106 cm-3 at 500 AU to (0.8-4) × 106 cm-3 at 5000 AU from the driving source.

    Original languageEnglish
    Pages (from-to)L137-L140
    JournalAstrophysical Journal
    Volume636
    Issue number2 II
    DOIs
    Publication statusPublished - 2006 Jan 10

    Keywords

    • ISM: individual (HH 211)
    • ISM: jets and outflows
    • Stars: formation

    ASJC Scopus subject areas

    • Astronomy and Astrophysics
    • Space and Planetary Science

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