vertically by $\Delta V$, we estimate the distance modulus of the target nova, $$(m-M)_{V,\rm target} 
= \left( (m-M)_V + \Delta V \right)_{\rm template} - 2.5 \log f_{\rm s}.
\label{distance_modulus_general_temp}$$ @hac10k called this method the time-stretching method. We usually increase/decrease the horizontal shift by a step of $\delta (\Delta \log t) = \delta (\log f_{\rm s}) = 0.01$ and the vertical shift by a step of $\delta (\Delta V)= 0.1$ mag, and determine the best one by eye. The model light curves obey the universal decline law. This phase corresponds to the optically thick wind phase before the nebular phase started. In fact, many novae show a good agreement with the model light curve in the optically thick phase. Moreover, we find that the $V$ light curve of a target nova often show a good agreement with that of a template nova even in the nebular (optically thin) phase. In such a case, we use all the phases to determine the timescaling factor (see, e.g., Figure \[lv\_vul\_yy\_dor\_lmcn\_2009a\_v\_b\_logscale\_2fig\]).\
[**3.**]{} Determine the WD mass and absolute brightness from the comparison with model light curves calculated by @hac10k [@hac15k; @hac16k]. These light curves are obtained for various WD masses and chemical compositions. The distance 