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G11.92-0.61 MM1: A Keplerian disc around a massive young proto-O star | | J. D. Ilee
; C. J. Cyganowski
; P. Nazari
; T. R. Hunter
; C. L. Brogan
; D. H. Forgan
; Q. Zhang
; | | Date: |
19 Aug 2016 | | Abstract: | The formation process of massive stars is not well understood, and
advancement in our understanding benefits from high resolution observations and
modelling of the gas and dust surrounding individual high-mass (proto)stars.
Here we report sub-arcsecond (<1550 au) resolution observations of the young
massive star G11.92-0.61 MM1 with the SMA and VLA. Our 1.3 mm SMA observations
reveal consistent velocity gradients in compact molecular line emission from
species such as CH$_3$CN, CH$_3$OH, OCS, HNCO, H$_2$CO, DCN and CH$_3$CH$_2$CN,
oriented perpendicular to the previously reported bipolar molecular outflow
from MM1. Modelling of the compact gas kinematics suggests a structure
undergoing rotation around the peak of the dust continuum emission. The
rotational profile can be well fit by a model of a Keplerian disc, including
infall, surrounding an enclosed mass of 30-60M$_{odot}$, of which
2-3M$_{odot}$ is attributed to the disc. From modelling the CH$_3$CN emission,
we determine that two temperature components, of 150 K and 230 K, are required
to adequately reproduce the spectra. Our 0.9 and 3.0cm VLA continuum data
exhibit an excess above the level expected from dust emission; the full
centimetre-submillimetre wavelength spectral energy distribution of MM1 is well
reproduced by a model including dust emission, an unresolved hypercompact
H{i}{i} region, and a compact ionised jet. In combination, our results
suggest that MM1 is an example of a massive proto-O star forming via disc
accretion, in a similar way to that of lower mass stars. | | Source: | arXiv, 1608.5561 | | Services: | Forum | Review | PDF | Favorites | |
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