cloud structures observed in the interstellar medium. For example, Figure \[distance\_reddening\_lv\_vul\_v1500\_cyg\_v1668\_cyg\_v1974\_cyg\](a) shows a large discrepancy among the various relations. The orange line [@gre18] is quite consistent with our values, i.e., the crossing point of $(m-M)_V=11.85$ (blue line) and $E(B-V)=0.60$ (vertical solid red line). This will be discussed in detail in Section \[lv\_vul\].

Template nova light curves {#template_novae}
--------------------------

Here, we reexamine the four template novae LV Vul, V1500 Cyg, V1668 Cyg, and V1974 Cyg, with the new distance-reddening relations [@gre18; @chen18] and fix the distances and extinctions for later use.

### LV Vul 1968\#1 {#lv_vul}

The reddening toward LV Vul was estimated by @fer69 to be $E(B-V)=0.6\pm 0.2$ from the color excesses of 14 B stars near the line of sight. @tem72 obtained $E(B-V)=0.55$ from the color at optical maximum; i.e., $E(B-V)=(B-V)_{\rm max} - (B-V)_{0, \rm max}= 
0.9 - 0.35 = 0.55$. He adopted $(B-V)_{0, \rm max}= + 0.35$ [@sch57] instead of $(B-V)_{0, \rm max}=+0.23$ [@van87]. @hac14k obtained $E(B-V)=0.60\pm0.05$ by fitting with the typical color-color evolution track of nova outbursts. @sla95 obtained the distance toward LV Vul to be $d=0.92\pm 0.08$ kpc by a nebular expansion parallax method.

Figure \[lv\_vul\_yy\_dor\_lmcn\_2009a\_v\_b\_logscale\_2fig\] shows the (a) $V$ and (b) $B$ light curves of 