We present evidence for the existence of the splashback radius in galaxy clusters selected using the Sunyaev-Zeldovich 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 _ { sp } = 1.85 _ { -0.30 } ^ { +0.26 } h ^ { -1 } { Mpc } , where the cluster sample has an average halo mass M _ { 500 c } = 3.0 \times 10 ^ { 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 can not 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 .