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We have developed an observing program using deep, multiband imaging to probethe chaotic regions of tidal tails in search of an underlying stellarpopulation, using NGC 3256's 400 Myr twin tidal tails as a case study. Thesetails have different colours of $u - g = 1.05 \pm 0.07$ and $r - i = 0.13 \pm0.07$ for NGC 3256W, and $u - g = 1.26 \pm 0.07$ and $r - i = 0.26 \pm 0.07$for NGC 3256E, indicating different stellar populations. These colourscorrespond to simple stellar population ages of $288^{+11}_{-54}$ Myr and$841^{+125}_{-157}$ Myr for NGC 3256W and NGC 3256E, respectively, suggestingNGC 3256W's diffuse light is dominated by stars formed after the interaction,while light in NGC 3256E is primarily from stars that originated in the hostgalaxy. Using a mixed stellar population model, we break our diffuse light intotwo populations: one at 10 Gyr, representing stars pulled from the hostgalaxies, and a younger component, whose age is determined by fitting the modelto the data. We find similar ages for the young populations of both tails,($195^{-13}_{+0}$ and $170^{-70}_{+44}$ Myr for NGC 3256W and NGC 3256E,respectively), but a larger percentage of mass in the 10 Gyr population for NGC3256E ($98^{+1}_{-3}\%$ vs $90^{+5}_{-6}\%$). Additionally, we detect 31 starcluster candidates in NGC 3256W and 19 in NGC 2356E, with median ages of 141Myr and 91 Myr, respectively. NGC 3256E contains several young (< 10 Myr), lowmass objects with strong nebular emission, indicating a small, recent burst ofstar formation.

A Tale of Two Tails: Exploring Stellar Populations in the Tidal Tails of NGC 3256