age range of 7-50 Myr, the @BC03 models suggest $M/L_V$=0.013–0.06 $M_{\odot}$/$L_{\odot}$; this suggests a stellar mass of $M_{stars}$=4-17$\times$10$^4$ $M_{\odot}$, consistent with our measurement of $M_{stars}$= 5.4$\pm$1.3$\times$10$^4$ $M_{\odot}$ in Section \[sec:stellarpops\]. This measured absolute magnitude is fully consistent with previous ground-based data [e.g. @Adams15], but is $\sim$2-$\sigma$ brighter than @Beccari16b.

We also subtracted the point sources in our [Dolphot]{} catalog from the F606W and F814W ACS mosaic images, and have analyzed the remaining diffuse light to constrain an old stellar population. Using this image and the same 11” annulus, we measure a diffuse, star-subtracted magnitude of $M_{F606W,0}$=$-$9.8$\pm$0.4 and $M_{F814W,0}$=$-$10.0$\pm$0.5, which corresponds to $M_{V}$=$-$9.8 $\pm$0.5 mag. The errors on these measurements include the range of values obtained using direct galaxy removal and background annulus subtraction.

We can compare the amount of diffuse light to that expected from the faint unresolved stars of the $\sim$7-50 Myr stellar population revealed in the CMD, but below the detection limit of the ACS data. To estimate this, we first calculated the total magnitude of resolved stars consistent with this population in the main body of AGC 226067 and used it as an anchor for integrating the luminosity function below our ACS detection limit, assuming a 7–50 