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We have used 4000 \AA\ break and H$\delta_A$ indices in combination withSFR/M* derived from emission line flux measurements, to constrain the recentstar formation histories of galaxies with stellar masses in the range10**8-10**10 Msol. The fraction of the total SFR density in galaxies withongoing bursts is a strong function of stellar mass, declining from 0.85 at astellar mass of 10**8 Msol to 0.25 for galaxies with M* = 10**10 Msol. Low massgalaxies are not all young. The distribution of half mass formation times forgalaxies with stellar masses less than 10**9 Msol is broad, spanning the range1-10 Gyr. The peak-to-trough variation in star formation rate among thebursting population ranges lies in the range 10-25. In low mass galaxies, theaverage duration of the burst is comparable to the dynamical time of thegalaxy. Galaxy structure is correlated with estimated burst mass fraction, butin different ways in low and in high mass galaxies. High mass galaxies withlarge burst mass fractions are more centrally concentrated, indicating thatbulge formation is at work. In low mass galaxies, stellar surface massdensities decrease as a function of F_{burst}. These results are in goodagreement with the observational predictions of Teyssier et al (2013) and lendfurther credence to the idea that the cuspy halo problem can be solved byenergy input from multiple starbursts over the lifetime of the galaxy. We notethat there is no compelling evidence for IMF variations in the population ofstar-forming galaxies in the local Universe.

Quantitative constraints on starburst cycles in galaxies with stellar masses in the range 10**8-10**10 Msol

Quantitative constraints on starburst cycles in galaxies with stellar masses in the range 108-1010 Msol