LV Vul as well as YY Dor (2004) and LMC N 2009a. The LV Vul data are the same as those in Figure 4 of Paper II. The light curves of YY Dor and LMC N 2009a are time-stretched against LV Vul. These two novae are analyzed by @hac18kb and the various properties are summarized in their Tables 1, 2, and 3. They determined the timescaling factors of YY Dor and LMC N 2009a against LV Vul, which are plotted in Figure \[lv\_vul\_yy\_dor\_lmcn\_2009a\_v\_b\_logscale\_2fig\]. In this case, we shift up/down the YY Dor and LMC N 2009a light curves in a step of $\delta(\Delta V)= 0.1$ mag (or $\delta(\Delta B)= 0.1$ mag) and find the best fit one by eye. We use all the part of the light curve if they overlap each other. If not, we use only the part of the optically thick wind phase before the nebular (or dust blackout) phase started. Fortunately, the three light curves of LV Vul, YY Dor, and LMC N 2009a broadly overlap each other even during the nebular phase as shown in Figure \[lv\_vul\_yy\_dor\_lmcn\_2009a\_v\_b\_logscale\_2fig\].

YY Dor and LMC N 2009a belong to the Large Magellanic Cloud (LMC) and their distances are well 