Melvyn Wright, Jun-Hui Zhao, Goran Sandell, Stuartt Corder, W. M. Goss, Lei Zhu
We present high angular resolution continuum observations of the high-mass
protostar NGC 7538S with BIMA and CARMA at 3 and 1.4 mm, VLA observations at
1.3, 2, 3.5 and 6 cm, and archive IRAC observations from the Spitzer Space
Observatory, which detect the star at 4.5, 5.8, and 8 $\mu$m. The star looks
rather unremarkable in the mid-IR. The excellent positional agreement of the
IRAC source with the VLA free-free emission, the OH, CH$_3$OH, H$_2$O masers,
and the dust continuum confirms that this is the most luminous object in the
NGC 7538S core. The continuum emission at millimeter wavelengths is dominated
by dust emission from the dense cold cloud core surrounding the protostar.
Including all array configurations, the emission is dominated by an elliptical
source with a size of ~ 8" x 3". If we filter out the extended emission we find
three compact mm-sources inside the elliptical core. The strongest one, $S_A$,
coincides with the VLA/IRAC source and resolves into a double source at 1.4 mm,
where we have sub-arcsecond resolution. The measured spectral index, $\alpha$,
between 3 and 1.4 mm is ~ 2.3, and steeper at longer wavelengths, suggesting a
low dust emissivity or that the dust is optically thick. We argue that the dust
in these accretion disks is optically thick and estimate a mass of an accretion
disk or infalling envelope surrounding S$_A$ to be ~ 60 solar masses.
View original:
http://arxiv.org/abs/1201.0944
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