Left: Gas particles in the model NGC 7715 tail (﹩t=120﹩ Myr), with representative contours to mark the location of the galaxy disks. All gas particles with coordinate values ﹩z\geq 0.63﹩ or ﹩x\geq 0.37﹩ were included. Most tail particles satisfy these constraints, while particles in the disks and other components do not (see Fig. 7). Right: As in Fig. 11, the same gas particles at a time (﹩t=0.0﹩ Myr) just before closest approach in the x‐z view. It suggests that a large fraction of the outer NGC 7715 disk is pulled out in the tail (26% of all gas particles). Note that the galaxy B contours at the earlier time primarily show the dense mass transfer stream; the B disk is shown in part by the dots.