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We present results from a detailed spectrophotometric analysis of the bluecompact dwarf galaxy Mrk 35 (Haro 3), based on deep optical (B,V,R,I) andnear-IR (J,H,K) imaging, Halpha narrow-band observations and long-slitspectroscopy. The optical emission of the galaxy is dominated by a centralyoung starburst, with a bar-like shape, while an underlying component of stars,with elliptical isophotes and red colors, extends more than 4 kpc from thegalaxy center. High resolution Halpha and color maps allow us to identify thestar-forming regions, to spatially discriminate them from the older stars, andto recognize several dust patches. We derive colors and Halpha parameters forall the identified star-forming knots. Observables derived for each knot arecorrected for the contribution of the underlying older stellar population, thecontribution by emission lines, and from interstellar extinction, and comparedwith evolutionary synthesis models. We find that the contributions of thesethree factors are by no means negligible and that they significantly varyacross the galaxy. Therefore, careful quantification and subtraction ofemission lines, galaxy host contribution, and interstellar reddening at everygalaxy position, are essential to derive the properties of the young stars inBCDs. We find that we can reproduce the colors of all the knots with aninstantaneous burst of star formation and the Salpeter initial mass functionwith an upper mass limit of 100 M_solar. In all cases the knots are just a fewMyr old. The underlying population of stars has colors consistent with beingseveral Gyr old.

Spectrophotometric investigations of Blue Compact Dwarf Galaxies: Markarian 35