  Around the time of its perihelion passage the observability of
67P/Churyumov-Gerasimenko from Earth was limited to very short windows each
morning from any given site, due to the low solar elongation of the comet. The
peak in the comet's activity was therefore difficult to observe with
conventionally scheduled telescopes, but was possible where service/queue
scheduled mode was possible, and with robotic telescopes. We describe the
robotic observations that allowed us to measure the total activity of the comet
around perihelion, via photometry (dust) and spectroscopy (gas), and compare
these results with the measurements at this time by Rosetta's instruments. The
peak of activity occurred approximately two weeks after perihelion. The total
brightness (dust) largely followed the predictions from Snodgrass et al. 2013,
with no significant change in total activity levels from previous apparitions.
The CN gas production rate matched previous orbits near perihelion, but
appeared to be relatively low later in the year.
