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We report the detection and analysis of the red giant branch luminosityfunction bump in a sample of isolated dwarf galaxies in the Local Group. Wehave designed a new analysis approach comparing the observed color-magnitudediagrams with theoretical best-fit color-magnitude diagrams derived fromprecise estimates of the star formation histories of each galaxy. This analysisis based on studying the difference between the V-magnitude of the RGB bump andthe horizontal branch at the level of the RR Lyrae instability strip(Delta_vhbb) and we discuss here a technique for reliably measuring thisquantity in complex stellar systems. By using this approach, we find that thedifference between the observed and predicted values of Delta_vhbb is +0.13 +/-0.14 mag. This is smaller, by about a factor of two, than the well-knowndiscrepancy between theory and observation at low metallicity commonly derivedfor Galactic globular clusters. This result is confirmed by a comparisonbetween the adopted theoretical framework and empirical estimates of theDelta_vhbb parameter for both a large database of Galactic globular clustersand for four other dSph galaxies for which this estimate is available in theliterature. We also investigate the strength of the red giant branch bumpfeature (R_bump), and find very good agreement between the observed andtheoretically predicted R_bump values. This agreement supports the reliabilityof the evolutionary lifetimes predicted by theoretical models of the evolutionof low-mass stars.

The ACS LCID project IV: detection of the RGB bump in isolated galaxies of the Local Group