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We have analyzed data from a multi-site campaign to observe oscillations inthe F5 star Procyon. The data consist of high-precision velocities that weobtained over more than three weeks with eleven telescopes. A new method foradjusting the data weights allows us to suppress the sidelobes in the powerspectrum. Stacking the power spectrum in a so-called echelle diagram revealstwo clear ridges that we identify with even and odd values of the angulardegree (l=0 and 2, and l=1 and 3, respectively). We interpret a strong, narrowpeak at 446 muHz that lies close to the l=1 ridge as a mode with mixedcharacter. We show that the frequencies of the ridge centroids and theirseparations are useful diagnostics for asteroseismology. In particular,variations in the large separation appear to indicate a glitch in thesound-speed profile at an acoustic depth of about 1000 s. We list frequenciesfor 55 modes extracted from the data spanning 20 radial orders, a rangecomparable to the best solar data, which will provide valuable constraints fortheoretical models. A preliminary comparison with published models shows thatthe offset between observed and calculated frequencies for the radial modes isvery different for Procyon than for the Sun and other cool stars. We find themean lifetime of the modes in Procyon to be 1.29 +0.55/-0.49 days, which issignificantly shorter than the 2-4 days seen in the Sun.

A multi-site campaign to measure solar-like oscillations in Procyon. II. Mode frequencies