Myr stellar population with \[Fe/H\]=$-$0.3 and the associated Padova luminosity function [@Bressan12] and a Chabrier initial mass function. Depending on the choice of age of the stellar population, and the filter, our resolved stellar sources should make up $\sim$45-70% of the total luminosity of AGC 226067, implying a diffuse stellar component from the young stellar population with $M_{V}$=$-$10.4$\pm$0.2 mag (where the error bars encapsulate the allowed range when varying the age of the stellar population). Thus, the observed diffuse component of AGC 226067 (directly measured as $M_{V}$=$-$9.8 $\pm$0.5 mag) is fully consistent with a stellar population belonging solely to the apparent young stellar population, with no need to invoke any associated older population. Given the apparent lack of an old stellar population, AGC 226067 cannot be considered a typical dwarf irregular-like galaxy as these systems all have an old RGB population at [*HST*]{} depths [e.g. @McQuinn14]. This strongly suggests that AGC 226067 is analogous to so-called ‘tidal dwarfs’ [see @Duc12 for a recent review] even if its origin is not from direct tidal interactions (see Section 5 for a discussion). Unlike previous examples of tidal dwarfs, AGC 226067 is extremely isolated, $\sim$350 kpc projected distance from the nearest large galaxies.

