uncertainties associated with internal mixing, stellar rotation and mass loss; @DP02; @McQuinn11]. The age of the youngest population of stars is consistent with the observation that AGC 226067 has HII regions.

We estimate the stellar mass of the main body of AGC 226067 by directly comparing the relative number of RHeB stars to that of our simulated 1$\times$10$^6$ $M_{\odot}$ stellar population, subtracting a background derived from outlying regions of the ACS field of view. We find $M_{stars}$= 5.4$\pm$1.3$\times$10$^4$ $M_{\odot}$ (where the error bar includes the effects of Poisson statistics and background subtraction, but not variations in stellar models or star formation histories), which is consistent with our finding from direct aperture photometry on the main body (Section \[sec:pop\]). Note that the photometric completeness at the faint end of the RHeB sequence is $>$95%, and so cannot effect our results. This and other properties of AGC 226067 are shown in Table \[table:properties\].

We can use this stellar mass to obtain an estimate of the star formation rate (SFR) of the main body; assuming uniform star formation over the past 50 Myr, we obtain a SFR of 1.1$\times$10$^{-3}$ M$_\odot$/yr. This is in general agreement with revised values of the SFR based off 