  We obtained the absolute magnitudes, distances, and white dwarf (WD) masses
of 32 recent galactic novae based on the time-stretching method for nova light
curves. A large part of the light/color curves of two classical novae often
overlap each other if we properly squeeze/stretch their timescales. Then, a
target nova brightness is related to the other template nova brightness by
$(M_V[t])_{\rm template} = (M_V[t/f_{\rm s}] - 2.5 \log f_{\rm s})_{\rm
target}$, where $t$ is the time, $M_V[t]$ is the absolute $V$ magnitude, and
$f_{\rm s}$ is their timescaling ratio. Moreover, when these two time-stretched
light curves, $(t/f_{\rm s})$-$(M_V-2.5 \log f_{\rm s})$, overlap each other,
$(t/f_{\rm s})$-$(B-V)_0$ do too, where $(B-V)_0$ is the intrinsic $B-V$ color.
Thus, the two nova tracks overlap each other in the $(B-V)_0$-$(M_V-2.5 \log
f_{\rm s})$ diagram. Inversely using these properties, we obtain/confirm the
distance and reddening by comparing each nova light/color curves with the well
calibrated template novae. We classify the 32 novae into two types, LV Vul and
V1500 Cyg types, in the time-stretched $(B-V)_0$-$(M_V-2.5 \log f_{\rm s})$
color-magnitude diagram. The WD mass is obtained by direct comparison of the
model $V$ light curves with the observation. Thus, we obtain a uniform set of
32 galactic classical novae that provides the distances and WD masses from a
single method. Many novae broadly follow the universal decline law and the
present method can be applied to them, while some novae largely deviate from
the universal decline law and so the method cannot be directly applied to them.
We discuss such examples.
