Dark matter on department scale

The direct detection of dark matter on Earth depends on its density and its velocity in the Solar neighbourhood. Unforunately, it is uncertain whether the dark matter distribution on the relevant physical scales (milliparsec) is homogeneous or not. Traditional N-body simulations cannot achieve the required resolution, so we have developed an ingenious method, able to achieve virtually any arbitrary resolution at almost no computational cost. This method allowed us to study in detail the ultra-fine distribution of dark matter in the Solar neighbourhood, investigating the implications for the current and next generation of dark matter directional detectors. The method is applied first to the merger of a single dark matter halo with a Milky Way-like one, and then to a cosmologically-based merger tree with a Galaxy-like endpoint. We conclude that the dark matter distribution on the relevant scale is smooth.