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The potential of the Surface Brightness Fluctuations (SBF) method todetermine the membership of dwarf elliptical galaxies (dEs) in nearby galaxyclusters is investigated. Extensive simulations for SBF measurements on dEs inthe I-band for various combinations of distance modulus, seeing and integrationtime are presented, based on average VLT FORS1 and FORS2 zero points. Theseshow that for distances up to 20 Mpc (Fornax or Virgo cluster distance),reliable membership determination of dEs can be obtained down to very faintmagnitudes -10<M_V<-12 mag (25 mag / arcsec^2) within integration times of theorder of 1 hour and with good seeing. Comparing the limiting magnitudes of themethod for the different simulated observing conditions we derive some simplerules to calculate integration time and seeing needed to reach a determinedlimiting magnitude at a given distance modulus for observing conditionsdifferent to the ones adopted in the simulations. Our simulations show a smalloffset of the order of 0.15 mag towards measuring too faint SBF. It is shownthat this is due to loss of fluctuation signal when recovering pixel-to-pixelfluctuations from a seeing convolved image. To check whether our simulationsrepresent well the behaviour of real data, SBF measurements for a real andsimulated sample of bright Centaurus Cluster dEs are presented. They show thatour simulations are in good agreement with the achievable S/N of SBFmeasurements on real galaxies.Comment: 12 pages, 8 figures, accepted by A&A, replaced by version with  non-abridged bottom page limi

Potential of the Surface Brightness Fluctuations method to measure distances to dwarf elliptical galaxies in nearby clusters