(2470 s) on 2015 July 7. The WFC3 F275W data contained only a handful of low S/N sources, and we will not consider it further. For the $F606W$ and $F814W$ data, multiple exposures were taken in each filter to remove cosmic rays, but we did not dither to fill in the chip gaps, as this was not necessary to fully image AGC 226067.

Point spread function photometry was performed using the software package [Dolphot]{} [@Dolphin00] on the individual charge transfer efficiency corrected ACS images (the [flc]{} files), with input parameters similar to @Williams14. Sources with (sharp$_{F606W}$ + sharp$_{F814W}$)$^2$$>$0.1 and (crowd$_{F606W}$ + crowd$_{F814W}$)$^2$$>$1.0 were culled, and only those remaining sources with a signal to noise ratio (SNR) greater than 4 in both the F606W and F814W bands were kept for further analysis. Artificial star tests were also run to quantify our photometric uncertainties and completeness; the 50% completeness limits are shown in Figure \[fig:cmds\]. The final photometric catalog was corrected for Galactic extinction [@Schlafly11] corresponding to the position of the main body of AGC 226067, with an adopted value of $E(B-V)=0.057$. All magnitudes presented in this work have this correction applied. All results are presented in the [vegamag]{} system.

To create 