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The Vela-D region, according to the nomenclature given by Murphy & May(1991), of the star forming complex known as the Vela Molecular Ridge (VMR),has been recently analyzed in details by Olmi et al. (2009), who studied thephysical properties of 141 pre- and proto-stellar cold dust cores, detected bythe ``Balloon-borne Large-Aperture Submillimeter Telescope'' (BLAST) during amuch larger (55 sq. degree) Galactic Plane survey encompassing the whole VMR.This survey's primary goal was to identify the coldest, dense dust corespossibly associated with the earliest phases of star formation. In this work,the dynamical state of the Vela-D cores is analyzed. Comparison to dynamicalmasses of a sub-sample of the Vela-D cores estimated from the 13CO survey ofElia et al. (2007), is complicated by the fact that the 13CO linewidths arelikely to trace the lower density intercore material, in addition to the densegas associated with the compact cores observed by BLAST. In fact, the totalinternal pressure of these cores, if estimated using the 13CO linewidths,appears to be higher than the cloud ambient pressure. If this were the case,then self-gravity and surface pressure would be insufficient to bind thesecores and an additional source of external confinement (e.g., magnetic fieldpressure) would be required. However, if one attempts to scale down the 13COlinewidths, according to the observations of high-density tracers in a smallsample of sources, then most proto-stellar cores would result effectivelygravitationally bound.

The BLAST Survey of the Vela Molecular Cloud: Dynamical Properties of the Dense Cores in Vela-D