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We have mapped the distribution of young and old stars in the gaseous HI warpof NGC 4565. We find a clear correlation of young stars (<600 Myr) with thewarp, but no coincident old stars (>1 Gyr), which places an upper limit on theage of the structure. The formation rate of the young stars, which increased~300 Myr ago relative to the surrounding regions, is (6.3 +2.5/-1.5) x 10^-5M_sol/yr/kpc^2. This implies a ~60+/-20 Gyr depletion time of the HI warp,similar to the timescales calculated for the outer HI disks of nearby spiralgalaxies. While some stars associated with the warp fall into the asymptoticgiant branch (AGB) region of the color magnitude diagram, where stars could beas old as 1 Gyr, further investigation suggests that they may be interlopersrather than real AGB stars. We discuss the implications of these ageconstraints for the formation of HI warps, and the gas fueling of diskgalaxies.

Constraining the age of the NGC 4565 HI Disk Warp: Determining the Origin of Gas Warps