  We present the radial distribution of the dark matter in two massive, X-ray
luminous galaxy clusters, Abell~2142 and Abell~2319, and compare it with the
quantity predicted as apparent manifestation of the baryonic mass in the
context of the "Emergent Gravity" scenario, recently suggested from Verlinde
(2016). Thanks to the observational strategy of the \xmm\ Cluster Outskirt
Programme (X-COP), using the X-ray emission mapped with \xmm\ and the SZ signal
in the Planck survey, we recover the gas density, temperature and thermal
pressure profiles up to $\sim R_{200}$, allowing to constrain at unprecedented
level the total mass through the hydrostatic equilibrium equation. We show
that, also including systematic uncertainties related to the X-ray based mass
modelling, the apparent "dark" matter shows a radial profile that has a shape
different from the traditional dark matter distribution, with larger
discrepancies (by a factor 2--3) in the inner ($r<200$ kpc) cluster's regions
and a remarkable agreement only across $R_{500}$.
