in the higher J transitions of both species, suggesting that they are sampling somewhat higher density gas. The 1.2mm dust continuum on the other hand is more extended suggesting that either an increase in excitation or in abundances is causing the  and (3–2) line emission to increase in relative strength toward the dust peak. Notable also are the large aspect ratios (1.6–1.9) observed in  suggesting an ellipsoidal or triaxial form for the high density core.

[lcccccc]{} line & Int. & $\Delta\alpha$& $\Delta\delta$ & Maj. Axis &Min. Axis & P.A.\
& & & & & &\
1.2mm & & -8 & 2 & 127 & 77 & -25\
(1-0) & 5.82 & -12 & 1 & 110 & 90 & -18\
(3-2) & 0.68 & -7 & 1 & 90 & 67 & +30\
(2-1) & 1.02 & -9 & 4 & 90 & 46 & -9\
(3-2) & 0.34 & -11 & 5 & 63 & 38 & -33\
\
\
\
\

\[gauss2d\]

Density and mass distribution {#sdensity}
-----------------------------

We expect the observed continuum emission at mm wavelengths to be optically thin and can relate the 1.2mm flux to the  column density under the approximation of constant dust emissivity 