  Photometric monitoring of Beta Pictoris in 1981 showed anomalous fluctuations
of up to 4% over several days, consistent with foreground material transiting
the stellar disk. The subsequent discovery of the gas giant planet Beta
Pictoris b and the predicted transit of its Hill sphere to within 0.1 au
projected distance of the planet provided an opportunity to search for the
transit of a circumplanetary disk in this $21\pm 4$ Myr-old planetary system.
  Continuous broadband photometric monitoring of Beta Pictoris requires
ground-based observatories at multiple longitudes to provide redundancy and to
provide triggers for rapid spectroscopic followup. These observatories include
the dedicated Beta Pictoris monitoring observatory bRing at Sutherland and
Siding Springs, the ASTEP400 telescope at Concordia, and observations from the
space observatories BRITE and Hubble Space Telescope.
  We search the combined light curves for evidence of short period transient
events caused by rings and for longer term photometric variability due to
diffuse circumplanetary material. We find no photometric event that matches
with the event seen in November 1981, and there is no systematic photometric
dimming of the star as a function of the Hill sphere radius. We conclude that
the 1981 event was not caused by the transit of a circumplanetary disk around
Beta Pictoris b.
  The upper limit on the long term variability of Beta Pictoris places an upper
limit of $1.8\times 10^{22}$ g of dust within the Hill sphere. Circumplanetary
material is either condensed into a non-transiting disk, is condensed into a
disk with moons that has a small obliquity, or is below our detection
threshold. This is the first time that a dedicated international campaign has
mapped the Hill sphere transit of a gas giant extrasolar planet at 10 au.
