Spectroscopic observations of 51 Pegasi and tau Bootis show no periodi
c changes in the shapes of their line profiles; these results for 51 P
eg are in significant conflict with those reported by Gray & Hatzes. O
ur detection limits are small enough to rule out nonradial pulsations
as the cause of the variability in tau Boo, but not in 51 Peg. The abs
ence of line shape changes is consistent with these stars' radial velo
city variability arising from planetary mass companions.