Table 2: Selected nova systems.
System $P_{\rm orb}$ $M_{\rm 2}$ $t_{\rm 3}$ $M_{\rm 1}$ q SH Reference
  [h] [ $M_{\rm\odot}$] [d] [ $M_{\rm\odot}$]      
RW UMi 1.418 0.07 140 0.64 0.11 N 1
CP Pup 1.474 0.08 8 1.19 0.07 Y 2
V1974 Cyg 1.950 0.14 42 0.90 0.16 Y 3, 4
RS Car 1.980 0.14 (58) 0.83 0.17 N 5
DD Cir 2.339 0.18 (10) 1.16 0.16 N 6
IM Nor 2.462 0.20 50 0.86 0.23 N 7, 8
QU Vul 2.682 0.23 40 0.91 0.25 N 9
V2214 Oph 2.804 0.24 100 0.71 0.34 N 10
V630 Sgr 2.830 0.25 11 1.14 0.22 Y 11
V351 Pup 2.837 0.25 (32) 0.95 0.26 N 11
V5116 Sgr 2.971 0.26 20.2 1.04 0.25 N this paper
V4633 Sgr 3.014 0.27 42 0.90 0.30 Y 12
DN Gem 3.068 0.28 37 0.92 0.30 N 13
V1494 Aql 3.231 0.30 16 1.08 0.28 N 14, 15, 16
V1668 Cyg 3.322 0.31 23 1.02 0.30 N 17
V603 Aql 3.324 0.31(0.29) 8 1.19(1.2) 0.26(0.24) Y 18
RR Cha 3.370 0.31 58 0.83 0.37 Y 5, 19
RR Pic 3.481 0.33(0.4) 150 0.62(0.95) 0.53(0.42) N 20, 21
V382 Vel 3.508 0.33 9 1.17 0.28 N 22, 23
V533 Her 3.530 0.33 44 0.89 0.37 N 24, 25
V2574 Oph 3.550 0.34 (33) 0.95 0.36 Y 26
OY Ara 3.731 0.36(0.34) ... (0.82) (0.41) N 27
V1493 Aql 3.740 0.36 7 1.21 0.30 N 14, 28
V849 Oph 4.146 0.41 175 0.59 0.69 N 29
DQ Her 4.647 0.48(0.40) 94 0.72(0.60) 0.67(0.67) N 30
T Aur 4.906 0.51(0.63) 100 0.71(0.68) 0.72(0.92) N 31
V4745 Sgr 4.987 0.52 32.8 0.95 0.55 N 32, 33
HR Del 5.140 0.54(0.55) 230 0.54(0.67) 1.00(0.82) N 34
V1425 Aql 6.139 0.57 39 0.91 0.63 N 14, 35
V4743 Sgr 6.718 0.74 15 1.10 0.67 N 36, 37
BY Cir 6.760 0.74 157 0.62 1.19 N 6
V2540 Oph 6.835 0.75 213 0.55 1.36 N 38
V838 Her 7.143 0.79(0.74) 3.2 1.29(0.87) 0.61(0.85) N 39
V2275 Cyg 7.548 0.84 7 1.21 0.69 N 40, 41
BT Mon 8.012 0.90(0.87) (213) 0.55(1.04) 1.64(0.84) N 42
V368 Aql 8.285 0.93 42 0.90 1.03 N 43
QZ Aur 8.580 0.97(1.05) 27 0.99(1.05) 0.98(1.00) N 44
Note: $P_{\rm orb}$ is the orbital period in hours, $M_{\rm 2}$ is the secondary mass in solar masses derived from Smith & Dhillon (1998) (from Ritter & Kolb 2003, in parentheses), $t_{\rm 3}$ is the decline time of three magnitudes from maximum (value in parentheses is the value estimated from the $t_{\rm 2}$ time using $t_{\rm 3} \simeq 2.75~t_{\rm 2}^{0.88}$ from Warner 1995), $M_{\rm 1}$ is the primary mass derived from Livio (1992) (from Ritter & Kolb 2003, in parentheses), q is the mass ratio, SH is the information about superhump detection (Y - yes, N - no), and Ref. is the reference.
References: 1 - Retter & Lipkin (2001), 2 - Patterson & Warner (1998), 3 - Skillman et al. (1997), 4 - Retter et al. (1997), 5 - Woudt & Warner (2002), 6 - Woudt & Warner (2003c), 7 - Woudt & Warner (2003b), 8 - Kato et al. (2002a), 9 - Shafter & Misselt (1995), 10 - Baptista et al. (1993), 11 - Woudt & Warner (2001), 12 - Lipkin et al. (2001), 13 - Retter et al. (1999), 14 - Arkhipova et al. (2002), 15 - Kato et al. (2004), 16 - Barsukova & Goranskii (2003), 17 - Kaluzny (1990), 18 - Retter & Naylor (2000), 19 - Hoffmeister (1959), 20 - Vogt (1975), 21 - Warner (1986), 22 - Balman et al. (2006), 23 - Della Valle et al. (2002), 24 - Patterson (1979b), 25 - Thorstensen & Cynthia (2000), 26 - Kang et al. (2006a), 27 - Zhao & McClintock (1997), 28 - Dobrotka et al. (2006b), 29 - Shafter et al. (1993), 30 - Walker (1961), 31 - Walker (1963), 32 - Csák et al. (2005), 33 - Dobrotka et al. (2006a), 34 - Kohoutek & Pauls (1980), 35 - Retter & Leibowitz (1998), 36 - Kang et al. (2006b), 37 - Kato et al. (2002b), 38 - Ak et al. (2005), 39 - Leibowitz et al. (1992), 40 - Balman et al. (2005), 41 - Kiss et al. (2002), 42 - Robinson et al. (1982), 43 - Diaz & Bruch (1994), 44 - Campbell & Shafter (1995).
Aditional sources for orbital period, $t_{\rm 2}$/$t_{\rm 3}$ time and catalogue masses: Duerbeck (1987), Warner (1986, 1995, 2002), Diaz & Bruch (1997), Ritter & Kolb (2003).

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