The G5.89-0.39 UC HII Region: Kinematics and Millimeter Aperture Synthesis Maps

Details The G5.89-0.39 UC HII Region: Kinematics and Millimeter Aperture Synthesis Maps The G5.89-0.39 UC HII Region: Kinematics and Millimeter Aperture Synthesis Maps

Dec 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...181.2206w&link_type=abstract

American Astronomical Society, 181st AAS Meeting, #22.06; Bulletin of the American Astronomical Society, Vol. 24, p.1157

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We present multi-line interferometer and single dish observations toward the G5.89-0.39 ultracompact HII region. This source is particularly well suited to detailed study because it is nearby (distance ~ 3 kpc), very luminous (L ~ 3*E(5) L_&sun;), and morphologically simple (shell type, isolated). Nine transitions in five molecular species (HCO(+) , H(13) CN, SO, CH3CN, (12) CO) and the H41alpha recombination line were mapped using the Hat Creek and Nobeyama arrays with 2(''}-8({'')) angular resolution and ~ 1 km/s velocity resolution. These observations show that the HII region is rapidly expanding into the surrounding warm (T>50 K), massive (M ~ 1000 M_&sun;) molecular core and confirm that the associated bipolar outflow is the most energetic yet discovered. The HCO(+) J=1-0 spectrum towards the HII region shows an inverse P-Cygni profile that is most simply interpreted as evidence for remnant infall. We have modelled the detailed velocity and density structure of the cloud using a spherically symmetric, multi-level, non-LTE radiative transfer code and find that the observed HCO(+) J=1-0 and J=3-2 spectra and spatial distributions are successfully reproduced by an overall collapse of the molecular core.

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