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A. S. Font (Dept. of Physics and Astronomy, University of Victoria), G. Sandell (NASA Ames Research Center, USRA/SOFIA), G. F. Mitchell (Dept. of Astronomy and Physics, Saint Mary's University)
New observations, using molecular CO (13CO J=3-2 and C18O J=3-2) and sub-millimeter (450\mum and 850\mum) emissions, are presented for the NGC 7129 star-forming region.
Both the submillimeter and the 13CO emission show a similar morphology, displaying a sharp boundary towards the cavity near the star LkH\alpha234. The new 450 and 850\mum observations are combined with previous continuum observations of the three compact far-infrared sources in the field, IRS6, NGC7129 SMM2 and NGC7129 FIRS 2, in order to make fits to the spectral energy distributions and to obtain the source sizes, dust temperatures, luminosities, and masses. The SMM2 source was not clearly seen in any earlier data set. Present data show that SMM2 is either a pre-stellar core or possibly a protostar. Also, the highest continuum peak emission is identified with the deeply embedded source IRS6 a few arcseconds away from LkH\alpha 234. From our isothermal modeling, IRS6 is determined to be either an early B-star or a young Herbig Be star, and responsible for the CO outflow. Our SCUBA data also give a more accurate position for the protostellar source NGC 7129 FIRS2 ans new estimates for its dust properties.
A comparison between the gas masses and the masses derived from the sub-millimeter fluxes shows that those are consistent, implying little or no CO depletion onto grains. The dust emissivity index is found to be low towards the dense compact sources, \beta ~1 - 1.6, and high, \beta ~ 2.0, in the surrounding cloud.
The author(s) of this abstract have provided an email address for comments about the abstract: afont@noir.phys.uvic.ca