Table 4.
Photometric parameters for the complete LRN sample.
| LRN name | Host | thost | Distance | E(B − V)tot | MV(prog) | MV(CE) | Mpk1 | Mpk2 | Lpk1/Lpk2 | Δt1 dex | Mprog |
|---|---|---|---|---|---|---|---|---|---|---|---|
| galaxy | (Mpc) | (mag) | (mag) | (mag) | (mag) | (mag) | optical | (days) | (M⊙) | ||
| AT 2021afy | UGC 10043 | 4.2 ± 0.7 | 49.2 ± 8.0 | 0.43 ± 0.11 | > − 11.66 ± 0.56 | > − 13.20 ± 0.56 | −14.44 ± 0.57 | −14.57 ± 0.56 | 1.0 | 120 |
 |
| UGC12307-2013OT1 | UGC 12307 | 9.8 ± 1.0 | 39.7 ± 2.8 | 0.22 ± 0.02 | > − 11.88 ± 0.17 | – | – | −15.03 ± 0.42 | – | – |
 |
| AT 2017jfs | NGC 4470 | 1.9 ± 2.1 | 35.2 ± 2.7 | 0.02 ± 0.01 | > − 11.26 ± 0.17 | – | −15.46 ± 0.46 | −14.38 ± 0.17 | 2.6 | 157 |
 |
| SNhunt248 | NGC 5806 | 3.2 ± 0.8 | 22.5 ± 3.8 | 0.04 ± 0.01 | −8.99 ± 0.36 | −11.18 ± 0.36 | −14.87 ± 0.36 | −14.07 ± 0.36 | 2.1 | 169 | 58 ± 2 ( ⋆ ) |
| AT 2020kog | NGC 6106 | 5.3 ± 0.6 | 22.5 ± 4.7 | 0.37 ± 0.07 | > − 9.82 ± 0.50 | −11.17 ± 0.53 | −13.17 ± 0.51 | −12.68 ± 0.51 | 2.0 | > 100 |
 |
| AT 2018hso | NGC 3729 | 1.3 ± 0.8 | 21.3 ± 0.6 | 0.30 ± 0.08 | −9.05 ± 0.25 | – | −13.89 ± 0.28 | −12.16 ± 0.26 | 3.7 | 201 |
 |
| NGC3437-2011OT1 | NGC 3437 | 5.2 ± 0.5 | 20.9 ± 4.2 | 0.02 ± 0.01 | > − 9.98 ± 0.43 | > − 10.83 ± 0.43 | −13.06 ± 0.48 | −13.33 ± 0.43 | 0.9 | 174 |
 |
| AT 2014ej | NGC 7552 | 2.4 ± 0.7 | 20.6 ± 1.5 | 0.31 ± 0.15 | > − 8.22 ± 0.50 | – | > − 14.70 ± 0.50 | −14.36 ± 0.50 | > 2.2 | > 98 |
 |
| NGC4490-2011OT1 | NGC 4490 | 7.0 ± 0.4 | 9.6 ± 1.3 | 0.32 ± 0.32 |
 |
 |
 |
 |
0.9 | 200 |
 |
| AT 1997bs | NGC 3627 | 3.1 ± 0.4 | 9.2 ± 0.3 | 0.21 ± 0.04 | −7.61 ± 0.21 | – | −13.34 ± 0.15 | −11.51 ± 0.17 | 3.2 | 62 |
 |
| AT 2021blu | UGC 5829 | 9.8 ± 0.6 | 8.64 ± 0.61 | 0.02 ± 0.01 | −6.72 ± 0.30 | −8.33 ± 0.43 | −13.06 ± 0.15 | −12.26 ± 0.15 | 2.4 | 242 |
 |
| AT 2021biy | NGC 4631 | 6.5 ± 0.7 | 7.46 ± 0.50 | 0.27 ± 0.02 | −7.93 ± 0.17 | −8.78 ± 0.20 | −13.81 ± 0.16 | −12.65 ± 0.16 | 2.7 | 375 | 20.5 ± 3.5 ( ⋆ ) |
| AT 2018bwo | NGC 45 | 7.8 ± 0.7 | 6.79 ± 1.13 | 0.02 ± 0.01 | −5.92 ± 0.36 | −7.47 ± 0.36 | – | −10.14 ± 0.45 | – | > 72 |
 |
| AT 2015dl | M 101 | 5.9 ± 0.3 | 6.43 ± 0.57 | 0.01 ± 0.01 | −7.19 ± 0.36 | −10.10 ± 0.47 | −12.70 ± 0.21 | −11.46 ± 0.31 | 2.0 | 229 | 18 ± 1 ( ⋆ ) |
| AT 2020hat | NGC 5068 | 6.0 ± 0.4 | 5.16 ± 0.21 | 0.09 ± 0.01 | −2.99 ± 0.09 | −8.87 ± 0.76 | −10.72 ± 0.27 | −10.08 ± 0.26 | 1.5 | 131 |
 |
| AT 2019zhd | M 31 | 3.0 ± 0.4 | 0.785 ± 0.009 | 0.055 ± 0.005 | 0.17 ± 0.14 | −5.74 ± 0.28 | −9.08 ± 0.13 | −7.59 ± 0.32 | 5.1 | 27 |
 |
| M31LRN2015 | M 31 | 3.0 ± 0.4 | 0.785 ± 0.009 | 0.35 ± 0.11 | −2.25 ± 0.47 | −5.41 ± 0.42 | −10.12 ± 0.42 | −9.13 ± 0.42 | 2.4 | 62 |
 |
| M31RV | M 31 | 3.0 ± 0.4 | 0.785 ± 0.009 | 0.12 ± 0.02 | −5.04 ± 0.32 | > − 7.04 ± 0.15 | −9.54 ± 0.15 | −8.66 ± 0.15 | 2.0 | 110 |
 |
| CK Vul( † ) | Galaxy | – |
 |
0.80 ± 0.15 |
 |
– |
 |
 |
0.7 | 400 | – |
| V838 Mon | Galaxy | – | 6.1(±0.6)×10−3 | 0.85 ± 0.02 | −1.29 ± 0.22 | −6.67 ± 0.22 | −9.76 ± 0.22 | −9.43 ± 0.22 | 1.7 | 82 | 8 ± 3 ( ⋆ ) |
| V4332 Sgr | Galaxy | – |
 |
0.32 ± 0.10 |
 |
– | – |
 |
– | – | 1.0 ± 0.5 ( ⋆ ) |
| V1309 Sco | Galaxy | – | 3.5(±1.5)×10−3 | 0.70 ± 0.15 | 3.33 ± 1.04 | −1.39 ± 1.04 | −7.02 ± 1.04 | −5.48 ± 1.04 | 3.1 | 29 | 1.54 ± 0.5 ( ⋆ ) |
| OGLE-2002-BLG-360 | Galaxy | – | 8.20(±0.15)×10−3 | 1.0 ± 0.2 (‡) | 2.23 ± 0.50 | −1.43 ± 0.54 | 0.10 ± 0.54 | 0.79 ± 0.65 | 1.0 | 837 |
 |
| OGLE-2002-BLG-360 | Galaxy | – | 8.20(±0.15)×10−3 | 1.0 ± 0.2 (‡) | 1.13 ± 0.28 | −3.54 ± 0.28 | −4.56 ± 0.28 | −4.65 ± 0.30 | 1.0 | 837 | – |
Notes. The table reports the LRN name (Col. 1); the host-galaxy name (Col. 2) and its morphological type code (from Hyperleda; Col. 3); the distance (Col. 4); the total colour excess (Col. 5); the V-band absolute magnitude of the quiescent progenitor (Col. 6), the brightest V absolute magnitude of the pre-outburst phase (Col. 7), the first light-curve peak (Col. 8), and the second light-curve peak (Col. 9); the optical luminosity ratio of the first to the second light-curve peak (Col. 10); time taken by the LRN to decrease its luminosity by one order of magnitude from the peak (Col. 11); and the progenitor mass estimate using Eq. (1) or taken from Cai et al. (2022b; Col. 12). ( ⋆ )Mass estimates obtained through the direct detection of the progenitor or via light-curve modelling, as adopted by Cai et al. (2022b). ( ‡ ) The Milky Way reddening towards OGLE-2002-BLG-360 follows a non-standard reddening law (E(B − V)MW = 1 mag, with RV = 2.5; Nataf et al. 2013). While the parameters for the I-band photometry are robust, those inferred for V photometry are uncertain owing to the low-cadence follow-up observations in that filter. The V magnitudes are obtained through an interpolation of the V − I colour curve at the epochs of the I-band peaks. (†) In this table, the parameters for CK Vul are taken from Banerjee et al. (2020).
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