Integrated column density and Doppler velocity map of M 31 and its environment. Left panel: HI emission exceeding the EBHIS 5σ sensitivity threshold across the radial velocity range −600 km s^-1 ≤ v_LSR ≤ −95 km s^-1 is displayed. The plane of the Milky Way Galaxy is visible along the top, and M 33 is seen in the lower left corner. At the distance of M 31, the extent of the map corresponds to 400 kpc. Right panel: intensity weighted Doppler velocity map of the area of interest. Using the radial velocity information, it is feasible to distinguish between individual coherent HI structures. The rotation of both local group spiral galaxies, as well as HI emission of so-called high-velocity clouds complex H (Simon et al. 2006; Blitz et al. 1999; v_LSR ≃ −200 km s^-1) next to the Milky Way Galaxy emission, can be identified.