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The young stellar population of a star-forming galaxy is the primary enginedriving its radiative properties. As a result, the age of a galaxy's youngestgeneration of stars is critical for a detailed understanding of its starformation history, stellar content, and evolutionary state. Here we presentpredicted equivalent widths for the H-beta, H-alpha, and Br-gamma recombinationlines as a function of stellar population age. The equivalent widths areproduced by the latest generations of stellar evolutionary tracks and theStarburst99 stellar population synthesis code, and are the first to fullyaccount for the combined effects of both nebular emission and continuumabsorption produced by the synthetic stellar population. Our grid of modelstellar populations spans six metallicities (0.001 < Z < 0.04), two treatmentsof star formation history (a 10^6 Mo instantaneous burst and a continuous starformation rate of 1 Mo/yr), and two different treatments of initial rotationrate (v_rot = 0.0v_crit and 0.4v_crit). We also investigate the effects ofvarying the initial mass function. Given constraints on galaxy metallicity, ourpredicted equivalent widths can be applied to observations of star-forminggalaxies to approximate the age of their young stellar populations.

Modeling Tracers of Young Stellar Population Age in Star-Forming Galaxies