Notes. The distances to the cluster centre are those given by R18 (which they determined using the coordinates of the centre of 47 Tuc determined by Goldsbury et al. 2010) for their sources with which our UV transients are associated. The observed outburst amplitudes (taken from the brightest observed uvm2 magnitude compared with the cluster background brightness at the source location) are lower limits because the true uvm2 quiescent magnitude of our transients could not be measured owing to the high cluster background, and because the outbursts are unlikely to be caught at maximum brightness. To determine a better constraint for the outburst amplitudes, we compared the uvm2 detections with the U300 magnitude measured by R18 (using HST) from the most likely quiescent counterpart of our sources, although these are still lower limits as the transients may not have been observed at during the peak of their outbursts in the UVOT observations. Photometric errors for the U300 magnitude (taken from R18) values are given in parentheses.