  Extreme scattering events in quasars suggest the existence of dark $\rm H_2 $
clumps of mass $\rm \sim 10^{-3} M_\odot$ and size $\rm \sim 10 AU$. Such
clumps are extremely dense compared to WIMPs clumps of the same mass obtained
by N-body simulations. A WIMP clump gravitationally attracted by a central $\rm
H_2 $ clump would experience a first infall during which its density increases
by $\rm 10^6$ in $\rm \sim 1 Myr$. In this poster I begin to explore the
phenomenology of mixed clumps made with $\rm H_2 $ and WIMPs. Molecular clouds
built with clumps are efficient machines to transform smooth distributions of
WIMPs into concentrated networks. If WIMPs are neutralinos gravitationally
attracted in clumps of such molecular clouds, they may either enrich the baryon
sector over cosmological ages, or remain mixed with cold $\rm H_2 $ clouds
until the clumps evaporate either by collision or by stellar UV heating. A
phenomenological model based on an hypothetic dark baryonic component (DBC)
that was invoked in the past to explain one of the main drawbacks of CDM
profiles, their overly dense cores, is briefly revisited in this context. The
DBC is replaced by a mix of $\rm H_2 $ and WIMPs, with a small fraction of HI
produced by internal $\rm H_2 $ collisions, in slightly dispersive clumpy
clouds that may migrate from the halo towards inner parts of a galaxy and disk.
