Bolometric light curves (top), black-body temperature profile (middle), and black-body radius profile (bottom) of SN 2016adj. Using broadband photometry corrected for both Milky Way and host-galaxy reddening, bolometric light curves were computed by: (i) integrating the best-fit Planck function to the SEDs (dashed line denoted by L_BB), (ii) trapezoidal integration of the SEDs (filled squares denoted by L_∫) and (iii) through the combination of the g- and i-band photometry combined with the bolometric corrections presented by Lyman et al. (2014, filled circles denoted L_BC, Lyman). We adopted our best host-reddening estimate, that is, a FTZ99 reddening law with $R_V^{\text{host}}$ = 5.7 ± 0.7 and $A_V^{\mathrm{host}}=6.3\pm 0.2$ mag. The uncertainties reported for R_BB and T_BB correspond to the BB fit errors, while those of L_BC, Lyman account for the uncertainties of the adopted reddening and distance to Centaurus A.