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It has long been speculated that the observed periodic radial velocitypattern for the K giant Pollux might be explained in terms of an orbitingplanetary companion. We have collected 80 high-resolution spectra for Pollux atLick Observatory yielding precise radial velocities with a mean error of 3.8m/s, providing the most comprehensive and precise data set available for thisstar. Our data confirm the periodicity previously seen in the radialvelocities. We derive a period of 589.7+/-3.5 days and, assuming a primary massof 1.86 M_Sun, a minimum companion mass of 2.9+/-0.3 M_Jup, consistent withearlier determinations. No evidence for any periodicities is visible in ouranalysis of the shapes of the spectral lines via the bisector method, so thatwe conclude that evidence is accumulating and compelling for a planet aroundPollux. However, some last doubt remains about this interpretation, becausenon-radial pulsations which might be present in giant stars could in principlealso explain the observed radial velocities, while the accompanying bisectorvariations might be too small to be detectable with current data.Comment: 13 pages, 4 figures, accepted by Ap

Precise Radial Velocities of Giant Stars. II. Pollux and Its Planetary Companion