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Despite the shallow convective envelopes of delta Scuti pulsators, solar-likeoscillations are theoretically predicted to be excited in those stars as well.To search for such stochastic oscillations we organised a spectroscopicmulti-site campaign for the bright, metal-rich delta Sct star rho Puppis. Weobtained a total of 2763 high-resolution spectra using four telescopes. Wediscuss the reduction and analysis with the iodine cell technique, developedfor searching for low-amplitude radial velocity variations, in the presence ofhigh-amplitude variability. Furthermore, we have determined the angulardiameter of rho Puppis to be 1.68 \pm 0.03 mas, translating into a radius of3.52 \pm 0.07Rsun. Using this value, the frequency of maximum power of possiblesolar-like oscillations, is expected at ~43 \pm 2 c/d (498 \pm 23 muHz). Thedominant delta Scuti-type pulsation mode of rho Puppis is known to be theradial fundamental mode which allows us to determine the mean density of thestar, and therefore an expected large frequency separation of 2.73 c/d (31.6muHz). We conclude that 1) the radial velocity amplitudes of the delta Scutipulsations are different for different spectral lines; 2) we can excludesolar-like oscillations to be present in rho Puppis with an amplitude perradial mode larger than 0.5 m/s.

Searching for solar-like oscillations in the delta Scuti star rho Puppis