Top: position (l_MS) versus velocity (v_GSR) diagram showing the maximum brightness temperature distribution across −42.5° ≤ b_LMC ≤ 42.5° across the whole velocity range of interest (starting at T_B = 200   mK up to 3 K on a linear scale). On the righthand side the LMC Hi emission, while the Milky Way emission is visible towards the bottom. The narrowly confined high-velocity dispersion emission lines are associated with nearby galaxies covered by GASS. Obvious is a continuous velocity gradient of the Hi emission above the Galactic plane from the LMC systemic velocity to v_GSR = 0   km   s^-1. The location of clouds belonging to the Wannier complexes WA, WB, WC, and WD are annotated. Bottom: the colored circles denote the location of the individual LA catalog objects while the gray-scale figure represents the “edge objects”, the Milky Way and the LMC. Each color marks an individual LA cloud complex (the ID of the catalog – available at the CDS – entry is given), aiming to demonstrate the coherent velocity structure of the complexes. The circle diameter scales according to . The regression line marks the mass–weighted velocity gradient with its LMC value of v_GSR = 84.2 ± 7   km   s^-1 demonstrating that the LA gas most likely is released from the LMC gaseous body.