SIMBAD references

Pulsation frequencies of a pulsating star appear as peaks in the frequency spectra of the star. The uncertainties of the detected frequencies may be expressed in terms of error limits based on the spectral resolution. Usually, amplitude A and phase φ of a given pulsation mode, as well as their respective standard deviations, σ_A and σ_φ, are calculated from linear sinusoidal fit. In this work we discuss the use of Monte Carlo simulations in the determination of σ_ν, σ_A and σ_φ. We show that the values of σ_A and σ_φ derived from LSINF underestimate the actual values, which can endanger the correct interpretation of the statistical significance of data and results.