stars ($F606W_0$$-$$F814W_0$$<$0.0 and $F814W_0$$\gtrsim$26 mag) that are likely young main sequence stars, along with a sequence of stars from 0.8$<$$F606W_0$$-$$F814W_0$$<$1.3 and 22$<$$F814W_0$$<$26 mag which are consistent with being red helium burning (RHeB) stars. There are only a handful of possible old, RGB stars (at $F606W_0$$-$$F814W_0$$>$0.4 and $F814W_0$$\gtrsim$27). The morphology of AGC226067 is broken up into several clumps with an approximate spatial extent of $\sim$20" ($\sim$1.6 kpc; Figure \[fig:image\]).

Also shown in Figure \[fig:cmds\], we overplot the CMDs of the secondary body (to be discussed in Section \[sec:secondary\]) and the new Virgo dwarf Dw J122147+132853, along with a 13.5 Gyr, \[Fe/H\]=$-$2 isochrone [@Bressan12]. There is no apparent overdensity of RGB stars associated with AGC 226067, signaling that any old stellar population must be small. This absence of RGB stars becomes more striking when compared with the CMD of Dw J122147+132853, which shows a large population of such stars (compatible with our adopted $D$=17 Mpc). A simple large-aperture analysis [see @Sand14 with masking of the nearby background spiral galaxy] indicates that Dw J122147+132853 has an absolute magnitude of $M_{F606W}$=$-$11.3$\pm$0.2 and $M_{F814W}$=$-$11.7$\pm$0.2; this is $M_{V}$=$-$11.4$\pm$0.2 using the transformations of @Sirianni05. The brightness of RHeB stars in optical CMDs is directly dependent on the 