Journal
ASTROPHYSICAL JOURNAL LETTERS
Volume 673, Issue 1, Pages L55-L58Publisher
IOP PUBLISHING LTD
DOI: 10.1086/527434
Keywords
stars : early-type; stars : formation; stars : individual (IRAS 18089-1732)
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Characterizing rotation, infall, and accretion disks around high-mass protostars is an important topic in massive star formation research. With the Australia Telescope Compact Array and the Very Large Array, we studied a massive disk candidate at high angular resolution in ammonia [NH3( 4, 4) and ( 5, 5)] tracing the warm disk but not the envelope. The observations resolved at similar to 0.4 resolution ( corresponding to similar to 1400 AU) a velocity gradient indicative of rotation perpendicular to the molecular outflow. Assuming a Keplerian accretion disk, the estimated protostar-disk mass would be high, similar to the protostellar mass. Furthermore, the position-velocity diagram exhibits additional deviation from a Keplerian rotation profile that may be caused by infalling gas and/or a self-gravitating disk. Moreover, a large fraction of the rotating gas is at temperatures > 100 K, markedly different from typical low-mass accretion disks. In addition, we resolve a central double-lobe centimeter continuum structure perpendicular to the rotation. We identify this with an ionized, optically thick jet.
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