supernova searches [@Graham12]. The detected population may be the tip of the iceberg, as we likely missed less luminous examples, and older stellar populations are more difficult to find because their UV/blue flux fades. In the past, infalling gas-rich systems were likely more abundant than they are today, thus this process could contribute substantially to the observed population of intracluster stars.

Discussion {#sec:discuss}
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The properties of AGC 226067 and its immediate environs are intriguing. In this work, we have shown that the main body has an exclusively young stellar population, with age $\sim$7-50 Myr and \[Fe/H\]$\approx$$-$0.3, with a $M_{V}$$\approx$$-$11.3 and $M_{star}$$\approx$5$\times$10$^4$ $M_{\odot}$. There is a secondary group of stars located $\sim$1.5’ ($\sim$7.5 kpc) to the Northeast, which is sparse but has a stellar population consistent with the main body of AGC 226067. The entire stellar system hosts a complex of HII regions that have a nearly uniform metallicity, $\langle$12 + log(O/H)$\rangle$ = 8.37 (for the main body), higher than expected given the stellar luminosity if AGC 226067 were a dwarf galaxy [@Beccari16b]. The HII region velocities of the main and secondary bodies agree with the HI clouds and the overall system displays a weak velocity gradient that spans both 