Although it is not sufficiently populated to confirm the presence of stars with age $<$10 Myr, it is likely the case given the secondary clump has several HII regions [@Beccari16b]. Again, there are few old RGB stars, in stark contrast to the nearby Virgo dwarf. We estimate the stellar mass in the secondary body identically to the technique employed on the main body and find $M_{stars}$=5.5$\pm$4.2$\times$10$^3$ $M_{\odot}$ (see Table 1).

Other possible stellar extensions of AGC 226067
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Two other regions around AGC 226067 have been discussed in the literature as possible physically-associated extensions, and we examine our [*HST*]{} photometry at these positions in more detail here.

The first is an additional clump of HI gas, discovered and dubbed AGC 229490 by @Adams15, which is physically separated from the main body of AGC 226067, but has a consistent HI-derived velocity (v$_{\odot}$=$-$123 and $-$142 km s$^{-1}$, respectively). We have constructed a CMD of AGC 229490 corresponding to the position of the gas cloud, and its rough dimensions [RA: 12:21:53.8, DEC: +13:29:08, with size 45“$\times$45”; @Adams15]. The CMD is largely consistent with several equal area background CMDs, possibly with an overdensity of $\sim$5 or fewer stars. Thus the secondary HI cloud, AGC 