The following document lists the file abstract/RLAUNHAR_CDSCAM.abs
from catalogue VI/111.
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In the course of our systematic study of Bok globules, it turned out that one of these low-mass star-forming cores is actually a very good candidate for an extremely early phase of a high-mass star. The object LBN 594-MM has a core-halo structure at 1.3mm dust continuum with a total mass of 570Mo and with most of the mass (450 Mo) in the core. Single-dish CS line data are indicative of infall motion what we presently check with completed interferometry measurements. The analysis of the CS line wings demonstrates the presence of a very dense bipolar outflow. Deep near-infrared images at 2.2 micron do not show any evidence for an embedded source, although the object was detected at all IRAS wavelengths and has IRAS colours typical for ultra-compact HII regions. However, the source structure at mid-infrared wavelengths seems to be complicated, with the 12 micron position shifted away from the 25/60/100 micron positions which are closer to the peak of the 1.3mm source. The IRAS data do not allow to check if the 12 micron emission is extended or comes from another, nearby point source. We propose ISOCAM mid-infrared imaging in order to get a detailed picture of the structure of one of the best candidates for an extremely young high-mass star or even protostar. The observations will demonstrate if even at 15 micron no object at the mm source position can be seen because it is too deeply embedded and if another warmer source lies close to the cold condensation. In addition, we will check if the high-mass protostellar clump is already associated with a cluster of low-mass stars. With the proposed ISOCAM observations, complemented by the ISOPHOT data of our guaranteed time programme (THENNING.YSOCDS) and the submm/mm data we already obtained, we will be able to construct a complete spectral energy distribution of this source which makes, together with the morphology information, a detailed radiative transfer modeling possible.