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We present the direct detection of the splashback feature using the sample ofmassive galaxy clusters from the Local Cluster Substructure Survey (LoCuSS).This feature is clearly detected (above $5\sigma$) in the stacked luminositydensity profile obtained using the K-band magnitudes of spectroscopicallyconfirmed cluster members. We obtained the best-fit model by means of Bayesianinference, which ranked models including the splashback feature as moredescriptive of the data with respect to models that do not allow for thistransition. In addition, we have assessed the impact of the cluster dynamicalstate on the occurrence of the splashback feature. We exploited the extensivemulti-wavelength LoCuSS dataset to test a wide range of proxies for the clusterformation history, finding the most significant dependence of the splashbackfeature location and scale according to the presence or absence of X-rayemitting galaxy groups in the cluster infall regions. In particular, we reportfor the first time that clusters that do not show massive infalling groupspresent the splashback feature at a smaller clustercentric radius $r_{\rm{sp}}/r_{\rm{200,m}} = 1.158 \pm 0.071$ than clusters that are activelyaccreting groups $r_{\rm{sp}}/r_{\rm{200,m}} = 1.291 \pm 0.062$. The differencebetween these two sub-samples is significant at $4.2\sigma$, suggesting acorrelation between the properties of the cluster potential and its accretionrate and merger history. Similarly, clusters that are classified as old anddynamically inactive present stronger signatures of the splashback feature,with respect to younger, more active clusters. We are directly observing howfundamental dynamical properties of clusters reverberate across vastlydifferent physical scales.

LoCuSS: The splashback radius of massive galaxy clusters and its dependence on cluster merger history