Using the absolute magnitude of Dw J122147+132853 ($M_V=-11.4$), this translates to a limiting absolute magnitude for the old population of AGC 226067 of $M_{V}$$>$$-$8.8 mag, or $M_{stars}$$<$6$\times$10$^5$ $M_{\odot}$ [assuming a $M/L_V$=2 $M_{\odot}$/$L_{\odot}$ for an old stellar population; @Strader11; @Baumgardt17]. This limit on the old stellar population in AGC 226067 hinges on it being at the same distance as Dw J122147+132853; if it were at a greater relative distance, the old stellar populations limits would be weaker. Similarly, if any putative old stellar population in AGC 226067 were significantly more metal rich than in Dw J122147+132853 its RGB stars would be pushed to relatively redder colors, outside of our CMD selection box. This relative difference in metallicity would again cause us to underestimate the old stellar population in AGC 226067. Finally, if a population of older stars is associated with AGC 226067, but spread out over a larger area than the young stellar population, then our limits on an old stellar population would be proportionately brighter (assuming a constant stellar surface density).

We measure the integrated magnitude for the main body within an 11” radius around AGC 226067 (after masking background galaxies) of $M_{F606W,0}$=$-$11.3$\pm$0.3 and $M_{F814W,0}$=$-$11.2$\pm$0.3, translating to $M_{V}$=$-$11.3$\pm$0.3. For the 