Light curves and color evolutions of two classical novae can be largely overlapped if we properly squeeze or stretch the timescale of a target nova against that of a template nova by . Then, the brightness of the target nova is related to the brightness of the template nova by , where M[t] is the absolute magnitude and a function of time t, and f _s is the ratio of timescales between the target and template novae. In the previous papers of this series, we show that many novae broadly overlap in the time-stretched (B − V)₀– color–magnitude diagram. In the present paper, we propose two other (U − B)₀– and (V − I)₀– diagrams and show that their tracks overlap for 16 and 52 novae, respectively. Here (U − B)₀, (B − V)₀, and (V − I)₀ are the intrinsic U − B, B − V, and V − I colors and not changed by the time stretch, and M _B , M _V , and M _I are the absolute B, V, and I magnitudes. Using these properties, we considerably refine the previous estimates of their distance and reddening. The obtained distances are in reasonable agreement with those of the Gaia Data Release 2 catalog.

如果我们适当地将目标新星的时间尺度相对于模板新星的时间尺度压缩或拉伸 0.0 倍，那么两个经典新星的光变曲线和颜色演化可能会在很大程度上重叠。然后，目标新星的亮度与模板新星的亮度相关，其中M [ t ] 是绝对星等，是时间t的函数，f _s是目标和模板新星之间的时间尺度比。在本系列的前几篇论文中，我们展示了许多新星在时间拉伸 ( B - V ) ₀ -颜色-星等图中广泛重叠。在本文中，我们提出了另外两个（U- B ) ₀ -和 ( V - I ) ₀ -图并显示它们的轨道分别重叠了 16 颗和 52 颗新星。这里 ( U − B ) ₀、 ( B − V ) ₀和 ( V − I ) ₀是固有的U − B、B − V和V − I颜色并且不会随时间拉伸而改变，并且M _B、中号_V , 和M _I是绝对的B、V和I量级。使用这些属性，我们大大改进了之前对它们的距离和变红的估计。获得的距离与 Gaia Data Release 2 目录中的距离合理一致。