STAR CLUSTER POPULATIONS IN THE OUTER DISKS OF NEARBY GALAXIES

We present a Large Binocular Telescope imaging study that characterizes the star cluster component of nearby galaxy outer disks (beyond the optical radius R-25). Expanding on the pilot project of Herbert-Fort et al., we present deep (similar to 27.5 mag V-band point-source limiting magnitude) U- and V-band imaging of six galaxies: IC 4182, NGC 3351, NGC 4736, NGC 4826, NGC 5474, and NGC 6503. We find that the outer disk of each galaxy is populated with marginally resolved star clusters with masses similar to 10(3) M-circle dot and ages up to similar to 1 Gyr (masses and ages are limited by the depth of our imaging and uncertainties are large given how photometry can be strongly affected by the presence or absence of a few stars in such low-mass systems), and that they are typically found out to at least 2 R-25 but sometimes as far as 3-4 R-25-even beyond the apparent H I disk. The mean rate of cluster formation for 1 R-25 <= R <= 1.5 R-25 is at least one every similar to 2.5 Myr and the clusters are spatially correlated with the H I, most strongly with higher density gas near the periphery of the optical disk and with lower density neutral gas at the H I disk periphery. We hypothesize that the clusters near the edge of the optical disk are formed in the extension of spiral structure from the inner disk and are a fairly consistent phenomenon and that the clusters formed at the periphery of the H I disk are the result of accretion episodes.