  In protoplanetary disks, CO$_2$ is solid ice beyond its snow line at $\sim 10
\rm AU$. Due to its high abundance, it contributes heavily to the collisional
evolution in this region of the disk. For the first time, we carried out
laboratory collision experiments with CO$_2$ ice particles and a CO$_2$-covered
wall at a temperature of 80 K. Collision velocities varied between 0 - 2.5 m/s.
Particle sizes were on the order of $\sim$ 100 $\mu$m. We find a threshold
velocity between the sticking and the bouncing regime at 0.04 m/s. Particles
with greater velocities but below 1 m/s bounce off the wall. For yet greater
velocities, fragmentation occurs. We give analytical models for the
coefficients of restitution and fragmentation strength consistent with the
experimental data. Set in context, our data show that CO$_2$ ice and silicate
dust resemble each other in the collisional behavior. Compared to water ice the
sticking velocity is an order of magnitude smaller. One immediate consequence
as example is that water ice particles mantled by CO$_2$ ice lose any "sticking
advantage." In this case, preferential planetesimal growth attributed to the
sticking properties of water ice will be limited to the region between the
H$_2$O ice line and the CO$_2$ ice line.
