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We investigate the role of stellar mass in shaping the intrinsic thickness offaint systems by determining the probability distribution of apparent axisratios for two different samples that probe the faint end of the galaxyluminosity function (M_B < -8). We find that the (b/a) distribution is a strongfunction of M*, and identify a limiting stellar mass M* ~ 2x10^9 Msun belowwhich galaxies start to be systematically thicker. We argue that this is theresult of the complex interplay between galaxy mass, specific angular momentumand stellar feedback effects: the increasing importance of turbulent motions inlower mass galaxies leads to the formation of thicker systems. We find a goodagreement between our results and the latest numerical simulations of dwarfgalaxy formation, and discuss several further implications of this finding--including the formation of bars and spirals in faint galaxies, thedeprojection of HI line profiles and simulations of environmental effects ondwarf galaxies.

Thin discs, thick dwarfs, and the importance of feedback effects