Extreme scattering events in quasars suggest the existence of dark H _ { 2 } ~ { } clumps of mass \sim 10 ^ { -3 } ~ { } M _ { \odot } and size \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 H _ { 2 } ~ { } clump would experience a first infall during which its density increases by 10 ^ { 6 } in \sim 1 ~ { } Myr .
In this poster I begin to explore the phenomenology of mixed clumps made with 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 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 H _ { 2 } ~ { } and WIMPs , with a small fraction of HI produced by internal H _ { 2 } ~ { } collisions , in slightly dispersive clumpy clouds that may migrate from the halo towards inner parts of a galaxy and disk .