along the line of sight, a velocity range in which they could plausibly be located given that Virgo’s Low Velocity cloud has $v_{lsr}$$\approx$0 km s$^{-1}$.

In a future contribution, we will present a full search of the NGVS dataset for similar blue, diffuse objects as well as followup optical/HI observations. The environment of these diffuse sources will also be investigated, although we note that NGVS-1+2 J122624+142327 is $\sim$28’ ($\sim$130 kpc) from NGC 4377 while NGVS-1+3 J122631+151026 is $\sim$10’ ($\sim$50 kpc) from NGC 4419, suggesting their possible association. Assuming a uniform distribution and given the relative ratio of the entire NGVS and our current search, we can expect to find a sample of $\sim$10-15 systems in total, including AGC 226067 and the newly identified objects. Taking our inferred star formation rate of the main body of AGC 226067 (1.1$\times$10$^{-3}$ $M_{\odot}$ yr$^{-1}$) as representative of the population as a whole, it implies an intracluster star formation rate of $\sim$0.01 $M_{\odot}$ yr$^{-1}$ in the Virgo cluster. The metallicity of the newly forming stars are comparable to the younger component of intracluster stars [@Williams07] and the inferred rate is consistent with the loose upper limit on the intracluster star formation rate found in cluster 