bodies [@Adams15; @Beccari16b]. Perhaps most intriguingly, there is no old stellar population associated with AGC 226067, as the entire diffuse light budget can be accounted for by the expected faint-end luminosity function of the visible $\sim$7-50 Myr stellar population. Given the metallicity and lack of old stellar population, AGC 226067 is a strong tidal dwarf candidate, and its extreme isolation makes it a unique example of this class of objects.

In understanding the origin of AGC 226067 we must also keep in mind that there seem to be other stellar systems of similar appearance in the NGVS dataset (Section \[sec:search\]), and perhaps a yet larger population of older, undetectable systems, as well as Virgo HI cloud complexes that have no stellar counterpart at all [e.g. @Kent10; @Taylor12] – there is plausibly a continuum of objects that are HI-rich and star-poor [see also the ‘Almost Dark’ objects; @Cannon15]. Recent theoretical effort has sought to understand the physics [e.g. @Burkhart16] and possible origins of these clouds [e.g. @Taylor16]; here we suggest that AGC 226067 is a stripped remnant of the numerous interactions in the Virgo cluster environment, most plausibly associated with the M86 subgroup.

A remnant of M86 subgroup interactions
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The 