Dense gas and exciting sources of the molecular outflow in the AFGL 437 star-forming region

Authors

  • G. Manjarrez,

    Corresponding author
    1. European Southern Observatory, Alonso de Cordova 3107, Vitacura, Casilla 19001, Santiago 19, Chile
    2. Centro de Radioastronomía y Astrofísica, UNAM, Morelia 58089, Mexico
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  • J. F. Gómez,

    Corresponding author
    1. Instituto de Astrofísica de Andalucía, CSIC, Apartado 3004, E-18080 Granada, Spain
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  • I. de Gregorio-Monsalvo

    1. European Southern Observatory, Alonso de Cordova 3107, Vitacura, Casilla 19001, Santiago 19, Chile
    2. Joint ALMA Observatory, Alonso de Cordova 3107, Vitacura, Casilla 19001, Santiago 19, Chile
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E-mail: gmanjarr@eso.org

On sabbatical leave at the Australia Telescope National Facility, CSIRO Astronomy and Space Science, Marsfield, NSW 2122, Australia.

ABSTRACT

We present Very Large Array (VLA) high-resolution observations of the NHinline image(1,1) and NHinline image(2,2) molecular transitions towards the high-mass star-forming region AFGL 437. Our aim was to investigate if the poorly collimated CO molecular outflow previously detected in the region is the result of a projection effect, with no intrinsic bipolarity, as suggested by Gómez et al. We complemented our observations with radio continuum archived data from the VLA at 2 and 3.6 cm, and with unpublished public data at 450 inline imagem taken with Submillimetre Common-User Bolometer Array at the James Clerk Maxwell Telescope. Ammonia emission was found mainly in three clumps located at the south and east of the position of the compact infrared cluster of AFGL 437, where the CO outflow seemed to have its origin. One of the NHinline image(1,1) clumps coincides with the maximum of NHinline image(2,2) and with a local peak of emission at 450 inline imagem. A near-infrared source (s11) is also found at that position. Our continuum map at 2 cm shows extended elongated emission associated with the infrared source AFGL 437W. This elongated morphology and its spectral index between 3.6 and 2 cm (inline image0.4) suggest the presence of a jet in AFGL 437W. We suggest that several molecular bipolar outflows may exist in the region. The observed CO outflow would be the superposition of those individual outflows, which would explain its low degree of collimation observed at larger scales.

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