age of the star [@McQuinn11], which we will use to constrain the stellar population in AGC 226067. In the bottom panel of Figure \[fig:cmds\], we show the results of simulating a constant star formation history 1$\times$10$^6$ $M_{\odot}$ stellar population with ages between $\sim$7–50 Myr and a \[Fe/H\]=$-$0.3 [corresponding to the gas-phase metallicity found by @Beccari16b assuming the solar abundance of @Grevesse07] at a distance of 17 Mpc (we assumed a Kroupa initial mass function; @Kroupa01). We have convolved the simulated data set with our measured photometric uncertainties. When compared with the CMD of AGC 226067’s main body, the dimmest RHeB stars correspond to an age of $\sim$50 Myr, while the two bright stars at the top of the sequence ($F814W_0$$\approx$22-22.5) correspond to RHeB stars of $\sim$7-8 Myr – we infer an approximate stellar population with age range of $\sim$7-50 Myr for AGC 226067. Star formation could have continued to the present day at a similar rate, but our CMDs can’t constrain this due to low number statistics. The simulated stellar population is not a perfect match to the colors of the observed CMD, but this is likely due to known limitations of stellar evolution models at these young ages [i.e. 