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We present a deep imaging survey of the Virgo Cluster, designed to study theconnection between cluster galaxies and Virgo's diffuse intracluster light(ICL). Our observations span roughly 16 square degrees and reach a 3-sigmadepth of mu(B)=29.5 and mu(V)=28.5 mag/arcsec^2. At these depths, the limitingsystematic uncertainties are astrophysical: scattered starlight from foregroundGalactic dust, and variations in faint background sources. The dust-scatteredstarlight is well-traced by deep far-infrared imaging, making itdistinguishable from true Virgo diffuse light. Our imaging maps the Virgo corearound M87 and the adjacent M86/M84 region, in subcluster B around M49, and inthe more distant W' cloud around NGC 4365. Most of the detected ICL is found inthe Virgo core and within the W' cloud, with little evidence for extensive ICLin subcluster B. The large amount of diffuse light seen in the infalling W'cloud likely illustrates the importance of the group environment for generatingICL. The bulk of the detected ICL is fairly red (B-V=0.7-0.9), indicative ofold stellar populations. We estimate a total Virgo ICL fraction of 7-15%,somewhat smaller than expected for massive, evolved clusters, suggesting thatVirgo is still growing its ICL component. We trace M87's extremely boxy haloout to ~ 150 kpc, and show that the current stripping rate of low luminositygalaxies is insufficient to have built M87's outer halo over a Hubble time.Finally, we identify another large ultra-diffuse galaxy in Virgo, likely in theprocess of being shredded by the cluster tidal field.

The Burrell Schmidt Deep Virgo Survey: Tidal Debris, Galaxy Halos, and Diffuse Intracluster Light in the Virgo Cluster