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tokens: uvm2 − u and u − v colors of ASASSN-15lh. The SN begins as quite blue but reddens with time until the rebrightening, during which the SN becomes bluer in the MUV–NUV. Bottom panel: the integrated luminosity (in units of erg s −1 ) of ASASSN-15lh between 1600 and 6000 Å. Overplotted is the integrated luminosity of the SLSN II SN 2008es, which is of comparable brightness to the rebrightening event, as well as a bright SN IIn and a normal SN Ia. Table 1 Swift /UVOT Photometry of ASASSN-15lh Note. Magnitudes are given in the UVOT/Vega system for easier comparison with other SNe published in that system (see Brown et al. 2014 for a review). The 3 σ upper limits and lower (saturation) limits come from the exposure and background parameters. Most of the photometry of ASASSN-15lh is not close to either of these limits, but they are given for completeness and easy comparison with other SN photometry tables from the Swift Optical/Ultraviolet Supernova Archive (SOUSA; Brown et al. 2014 ). This table gives a portion of the data. (This table is available in its entirety in machine-readable form.) Only a portion of this table is shown here to demonstrate its form and content. A machine-readable version of the full table is available. One might be concerned about the effect of the optical tails of the uvw2 and uvw1 filters (sometimes referred to as the “red leaks”), which still have 1/1000 of the peak transmission all the way to 5000 Å (see Breeveld et al. 2011 and Brown et al. 2010 for graphical descriptions of the revised filter throughput curves). To estimate the contribution from the optical tails, we compare the count rates to those expected through synthetic filters similar to uvw2 and uvw1 but cutting off sharply to zero throughput at 2500 and 3300 Å (Brown et al. 2010 ). Using a blackbody spectrum corresponding to 16,000 K (the hottest estimated below), the counts coming from the redder portion correspond to 12% and 3 % of the total in the uvw2 and uvw1 filters, respectively. Using a blackbody spectrum corresponding to 10,770 K (the coolest estimated below), the extra counts coming from the redder portion correspond to 20% and 5 % of the total in the uvw2 and uvw1 filters, respectively. Thus the contribution from the red tails increases as the SN reddens, but never contributes a large fraction of the counts. The wavelengths beyond which are considered to be part of a red leak (as opposed to just the long wavelength edge of the filter) can be arbitrary and require a spectral model as well as the filter curves to quantify. Even if the red leak contributed a significant fraction of the observed count rate in the UV filters, the analysis below takes the red leaks into account. For example, blackbody fits are performed by comparing the observed count rates to those predicted from blackbody spectra through the whole filter. Brown et al. (2016, AJ accepted) give a detailed description of issues involved with the conversion of Swift /UVOT broadband