We present a polarimetric investigation of the protoplanetary nebula Frosty Leo performed with the Submillimeter Array .
We were able to detect , in the low continuum level ( peak at 14.4 mJy beam ^ { -1 } ) , a marginal polarization at \sim 2.6 \sigma .
The molecular line investigation based on the CO J = 3 \rightarrow 2 emission shows a peak emission of 68.1 Jy beam ^ { -1 } km s ^ { -1 } and the polarization detection in this CO line is also marginal , with a peak at \sim 3.8 \sigma .
In both cases , it was therefore not possible to use the electric vector maps ( \bmath { E } -field ) to accurately trace the magnetic field ( \bmath { B } -field ) within the PPN.The spatio-kinematic modelling realised with the different velocity channel maps indicates three main structures : a distorted torus accompanied by a bipolar outflow or jet aligned with its axis and a flattened spherical ‘ ‘ cap ’ ’ .
The comparison of the CO polarization segments with our model suggests that the polarized emission probably arises in the first two components .