removal of gas from cluster galaxies due to the hot intracluster medium (ICM) via ram pressure stripping [@Gunn72] is one plausible mechanism that could explain the origin of AGC 226067. Recent simulations of ram pressure stripping have shown that small amounts of star formation in the stripped tail of ablated gas can be seen up to hundreds of kiloparsecs from the galaxy of origin [@Kapferer09; @Tonnesen12]. This star formation is not from stripped molecular clouds of gas from the parent galaxy, but is low density stripped gas that cools and condenses in the turbulent wake of the stripping, a process that takes $\sim$300–750 Myr at the pressure of the Virgo ICM. Individual star forming knots contain up to $M_{stars}$$\sim$10$^{5-6}$$M_{\odot}$, similar to AGC 226067, and is not expected to contribute significantly to the total intracluster light budget [@Kapferer09; @Tonnesen12]. There are examples of intracluster star formation (or implied star formation from H$\alpha$ emission) due to ram pressure stripping in nearby galaxy clusters [e.g. @Kenney99; @Cortese07; @Yoshida08; @Sun10; @Yagi10; @Kenney14 among others], but to our knowledge none have been uncovered at such large projected distances ($D$$\sim$350 kpc) from their point of origin as AGC 226067; systems such as this and those uncovered 