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We investigate the idea that the interaction of Dark Matter (DM) sub-haloswith the gaseous disk of galaxies can be the origin for the observed holes andshells found in their neutral hydrogen (HI) distributions. We use highresolution hydrodynamic simulations to show that pure DM sub-halos impacting agalactic disk are not able to produce holes; on the contrary, they result inhigh density regions in the disk. However, sub-halos containing a small amountof gas (a few percent of the total DM mass of the sub-halo) are able todisplace the gas in the disk and form holes and shells. The size and lifetimeof these holes depend on the sub-halo gas mass, density and impact velocity. ADM sub-halo of mass $10^8$ $M_{\odot}$ and a gas mass fraction of $\sim 3$%, isable to create a kpc scale hole, with a lifetime similar to those observed innearby galaxies. We also register an increase in the star formation rate at therim of the hole, again in agreement with observations. Even though theproperties off these simulated structures resemble those found in observationswe find that the number of predicted holes (based on mass and orbitaldistributions of DM halos derived from cosmological N-body simulations) fallsshort compared to the observations. Only a handful of holes are produced perGiga year. This leads us to conclude that DM halo impact is not the majorchannel through which these holes are formed.

Interaction between dark matter sub-halos & galactic gaseous disk