  We use the lensing potential map from Planck CMB lensing reconstruction
analysis and the "Public Cosmic Void Catalog" to measure the stacked void
lensing potential. In this profile, four parameters are needed to describe the
shape of voids with different characteristic radii $R_V$. However, we have
found that after reducing the background noise by subtracting the average
background, there is a residue lensing power left in the data. The inclusion of
the environment shifting parameter, $\gamma_V$, is necessary to get a better
fit to the data with the residue lensing power. We divide the voids into two
redshift bins: cmass1 ($0.45 < z < 0.5$) and cmass2 ($0.5 < z < 0.6$). Our
best-fit parameters are $\alpha = 1.989\pm0.149$, $\beta = 12.61\pm0.56$,
$\delta_c=-0.697\pm0.025$, $R_S/R_V=1.039\pm0.030$, $\gamma_v=(-7.034\pm0.150)
\times 10^{-2}$ for the cmass1 sample with 123 voids and $\alpha =
1.956\pm0.165$, $\beta = 12.91\pm0.60$, $\delta_c=-0.673\pm0.027$,
$R_S/R_V=1.115\pm0.032$, $\gamma_v=(-4.512\pm0.114) \times 10^{-2}$ for the
cmass2 sample with 393 voids at 68% C.L. The addition of the environment
parameter is consistent with the conjecture that the Sloan Digital Sky Survey
voids reside in an underdense region.
