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Spectroscopic observations of 51 Pegasi and tau Bootis show no periodicchanges in the shapes of their line profiles; these results for 51 Peg are insignificant conflict with those reported by Gray and Hatzes (1997). Ourdetection limits are small enough to rule out nonradial pulsations as the causeof the variability in tau Boo, but not in 51 Peg. The absence of line shapechanges is consistent with these stars' radial velocity variability arisingfrom planetary-mass companions.Comment: 10 pages, 2 figures, plain TeX, accepted for publication in ApJ

A Search for Line Shape and Depth Variations in 51 Pegasi and τ Bootis