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We compare the magnetic field orientation for the young giant molecular cloudVela C inferred from 500-$\mu$m polarization maps made with the BLASTPolballoon-borne polarimeter to the orientation of structures in the integratedline emission maps from Mopra observations. Averaging over the entire cloud wefind that elongated structures in integrated line-intensity, or zeroth-momentmaps, for low density tracers such as $^{12}$CO and $^{13}$CO $J$ $\rightarrow$1 - 0 are statistically more likely to align parallel to the magnetic field,while intermediate or high density tracers show (on average) a tendency foralignment perpendicular to the magnetic field. This observation agrees withprevious studies of the change in relative orientation with column density inVela C, and supports a model where the magnetic field is strong enough to haveinfluenced the formation of dense gas structures within Vela C. The transitionfrom parallel to no preferred/perpendicular orientation appears to happenbetween the densities traced by $^{13}$CO and by C$^{18}$O $J$ $\rightarrow$ 1- 0. Using RADEX radiative transfer models to estimate the characteristicnumber density traced by each molecular line we find that the transition occursat a molecular hydrogen number density of approximately $10^3$ cm$^{-3}$. Wealso see that the Centre-Ridge (the highest column density and most activestar-forming region within Vela C) appears to have a transition at a lowernumber density, suggesting that this may depend on the evolutionary state ofthe cloud.

Relative Alignment Between the Magnetic Field and Molecular Gas Structure in the Vela C Giant Molecular Cloud using Low and High Density Tracers