in this work can provide an important test of ram pressure models.

In Figure \[fig:environ\], we show AGC 226067 in relation to the M86 subgroup of the Virgo cluster, a major component of the ‘Low Velocity Cloud’ of Virgo galaxies with similar low heliocentric velocities as AGC 226067. AGC 226067 is $\sim$350 kpc in projection from M86. Overplotted are the Chandra surface brightness contours [@Randall08] and H$\alpha$ contours [@Kenney08] surrounding both M86 and NGC 4438 which show evidence for a previous interaction with each other [e.g. @Kenney08], and are likely undergoing a ram pressure stripping event as they fall into the larger Virgo cluster together [@Randall08; @Ehlert13 among others]. The stream of X-ray emitting gas and H$\alpha$ emission point in the general direction of AGC 226067, but the extent of the available datasets is not large enough to probe out to the necessary distances, as marked in Figure \[fig:environ\]. Given the suggestive stream pointing in the direction of AGC 226067, this interpretation of its origin is our preference, although future X-ray and H$\alpha$ mapping will be necessary to confirm this scenario.

@Beccari16b suggested that the interacting galaxy pair NGC 4299 ($v_{\odot}$$\approx$+230 km s$^{-1}$) and NGC 4294 ($v_{\odot}$$\approx$+350 km s$^{-1}$) were 