  We present evidence for the existence of the splashback radius in galaxy
clusters selected using the Sunyaev-Zel'dovich effect. We show that the
deprojected cross-correlation of galaxy clusters found in the Planck survey
with galaxies detected photometrically in the Pan-STARRS survey, shows a sharp
steepening feature (a logarithmic slope steeper than $-3$), which we associate
with the splashback radius. We infer the three-dimensional splashback radius
for the SZ cluster sample to be $r_{\rm sp}=1.85_{-0.30}^{+0.26}$ $h^{-1}$Mpc,
where the cluster sample has an average halo mass
$M_{500c}=3.0\times10^{14}h^{-1}M_\odot$ at an average redshift of $z=0.18$.
The inferred value of the splashback radius appears consistent with the
expected location for dark matter halos in the standard cold dark matter
paradigm. However, given the limited precision of our measurements, we cannot
conclusively rule out the smaller splashback radius measured so far in the
literature for optically selected galaxy clusters. We show that the splashback
radius does not depend upon the galaxy magnitude for galaxies fainter than
$M_i-5\log h=-19.44$, and is present at a consistent location in galaxy
populations divided by color. The presence of the splashback radius in the
star-forming galaxy population could potentially be used to put lower limits on
the quenching timescales for galaxies. We can marginally rule out the
contamination of the star-forming galaxy sample by quenched galaxies, but the
results would need further verification with deeper datasets.
