the MUSE spectra [@Beccari17_error].

We can also look at the nature of star formation in this object by examining where it falls on a Kennicutt-Schmidt relation of SFR density ($\Sigma_{SFR}$) vs. gas density. Assuming our SFR estimate for the main body and a radius of 1.1 kpc (Table \[table:properties\]), we get a $\Sigma_{SFR}$$=$2.9$\times$10$^{-4}$ M$_\odot$/yr/kpc$^2$. The main body has an estimated HI mass of 1.5$\times$10$^{7}$ M$_\odot$ in a deconvolved area of 3.08$\times$10$^7$ pc$^2$ [@Adams15], giving a gas surface density of 0.49 M$_\odot$/pc$^2$. These values suggest the star formation in AGC 226067 is occurring at the low end of gas surface densities in comparison to nearby galaxy disks [@Bigiel08], and is slightly more efficient than that typically seen in the outer regions of nearby spirals and dwarfs [@Bigiel10].

The Secondary Body {#sec:secondary}
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Several previous works have also pointed out a secondary clump of blue stars (Figure \[fig:image\]), located $\sim$1.6’ ($\sim$8 kpc) to the Northeast of the main body of AGC 226067 [@Sand15; @Adams15; @Beccari16; @Beccari16b]. A CMD of this region is shown in the middle-left panel at the top of Figure \[fig:cmds\]. The stars in this secondary knot are consistent with the stellar population of the main body of AGC 226067. 