  The splashback radius $r_\text{sp}$ separates the physical regimes of
collapsed and infalling material around massive dark matter haloes. In
cosmological simulations, this location is associated with a steepening of the
spherically averaged density profile $\rho(r)$. In this work, we measure the
splashback feature in the stacked weak gravitational lensing signal of $27$
massive clusters from the Cluster Canadian Comparison Project with careful
control of residual systematics effects. We find that the shear introduced by
the presence of additional structure along the line of sight significantly
affects the noise at large clustercentric distances. Although we do not detect
a significant steepening, the use of a simple parametric model enables us to
measure both $r_\text{sp}=3.5^{+1.1}_{-0.7}$ comoving Mpc and the value of the
logarithmic slope $\gamma = \log \rho / \log r$ at this point,
$\gamma(r_\text{sp}) = -4.3^{+1.0}_{-1.5}$.
