We present the rotation velocities V and velocity dispersions \sigma along the principal axes of seven elliptical galaxies less luminous than M _ { B } = -19.5 .
These kinematics extend beyond the half-light radii for all systems in this photometrically selected sample .
At large radii the kinematics not only confirm that rotation and “ diskiness ” are important in faint ellipticals , as was previously known , but also demonstrate that in most sample galaxies the stars at large galactocentric distances have \bigl ( V / \sigma \bigr ) _ { max } \sim 2 , similar to the disks in bona-fide S0 galaxies .
Comparing this high degree of ordered stellar motion in all sample galaxies with numerical simulations of dissipationless mergers argues against mergers with mass ratios \leq 3 : 1 as an important mechanism in the final shaping of low-luminosity ellipticals , and favors instead the dissipative formation of a disk .