magnitudes are different among novae. This is the reason why @hac16kb did not find common tracks in the $(B-V)_0$-$M_V$ diagram. If we use the $(B-V)_0$-$(M_V-2.5\log f_{\rm s})$ diagram, we could find common tracks because the $(t/f_{\rm s})$-$(M_V-2.5\log f_{\rm s})$ light curves overlap each other after time-stretch.

In this work, we examine nova evolution in the time-stretched color-magnitude diagram. We adopt total 20 novae, including 12 novae that were already analyzed in Paper II, but reanalyzed here in a new light of the time-stretched color-magnitude diagram. Our aim is to provide a uniform set of 20 novae analyzed by the same time-stretched color-magnitude diagram method.

Our paper is organized as follows. First we describe our method for four well-studied novae in Section \[method\_example\]. Then, we apply this method to four recent novae V574 Pup, V679 Car, V1369 Cen, and V5666 Sgr to determine their various physical parameters in Sections \[v574\_pup\_cmd\], \[v679\_car\_cmd\], \[v1369\_cen\_cmd\], and \[v5666\_sgr\_cmd\], respectively. In Section \[twelve\_novae\], we reanalyze twelve novae, which were studied in Paper II on the usual color-magnitude diagram. We confirm that all the novae follow one of the two template tracks, V1500 Cyg or LV Vul, in the time-stretched color-magnitude diagram. In Section \[discussion\], we compared 