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The observations carried out by the space missions CoRoT and Kepler provide alarge set of asteroseismic data. Their analysis requires an efficient procedurefirst to determine if the star is reliably showing solar-like oscillations,second to measure the so-called large separation, third to estimate theasteroseismic information that can be retrieved from the Fourier spectrum. Wedevelop in this paper a procedure, based on the autocorrelation of the seismicFourier spectrum. We have searched for criteria able to predict the output thatone can expect from the analysis by autocorrelation of a seismic time series.First, the autocorrelation is properly scaled for taking into account thecontribution of white noise. Then, we use the null hypothesis H0 test to assessthe reliability of the autocorrelation analysis. Calculations based on solarand CoRoT times series are performed in order to quantify the performance as afunction of the amplitude of the autocorrelation signal. We propose anautomated determination of the large separation, whose reliability isquantified by the H0 test. We apply this method to analyze a large set of redgiants observed by CoRoT. We estimate the expected performance for photometrictime series of the Kepler mission. Finally, we demonstrate that the methodmakes it possible to distinguish l=0 from l=1 modes. The envelopeautocorrelation function has proven to be very powerful for the determinationof the large separation in noisy asteroseismic data, since it enables us toquantify the precision of the performance of different measurements: mean largeseparation, variation of the large separation with frequency, small separationand degree identification.

On detecting the large separation in the autocorrelation of stellar oscillation times series