2015ApJ...799...75G

We report molecular line observations, made with ASTE and SEST, and dust continuum observations at 0.87 mm, made with APEX, toward the cold dust core G305.136+0.068. The molecular observations show that the core is isolated and roughly circularly symmetric and imply that it has a mass of 1.1x10³ M_☉. A simultaneous model fitting of the spectra observed in four transitions of CS, using a non-LTE radiative transfer code, indicates that the core is centrally condensed, with the density decreasing with radius as r.^–1.8, and that the turbulent velocity increases toward the center. The dust observations also indicate that the core is highly centrally condensed and that the average column density is 1.1 g/cm2, a value slightly above the theoretical threshold required for the formation of high-mass stars. A fit to the spectral energy distribution of the emission from the core indicates a dust temperature of 17±2 K, confirming that the core is cold. Spitzer images show that the core is seen in silhouette from 3.6 to 24.0 µm and that it is surrounded by an envelope of emission, presumably tracing an externally excited photo-dissociated region. We found two embedded sources within a region of 20'' centered at the peak of the core, one of which is young, has a luminosity of 66 L_☉, and is accreting mass with a high accretion rate of ∼1x10^–4 M_☉/yr. We suggest that this object corresponds to the seed of a high-mass protostar still in the process of formation. The present observations support the hypothesis that G305.136+0.068 is a massive and dense cold core in an early stage of evolution, in which the formation of a high-mass star has just started.