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The goal is to test the structure of hot metallic stars, and in particularthe structure of a near-surface convection zone using asteroseismicmeasurements. Indeed, stellar models including a detailed treatement of theradiative diffusion predict the existence of a near-surface convection zone inorder to correctly reproduce the anomalies in surface abundances that areobserved in Am stars. The Am star HD 209625 was observed with the Harpsspectrograph mounted on the 3.6-m telescope at the ESO La Silla Observatory(Chile) during 9 nights in August 2005. This observing run allowed us tocollect 1243 radial velocity (RV) measurements, with a standard deviation of1.35 m/s. The power spectrum associated with these RV measurements does notpresent any excess. Therefore, either the structure of the external layers ofthis star does not allow excitation of solar-like oscillations, or theamplitudes of the oscillations remain below 20-30 cm/s (depending on theirfrequency range).

A search for solar-like oscillations in the Am star HD 209625