Table 3.
Main parameters of known merger candidates.
| Outburst period | d | Etot(B − V) | MV, star | MV, prec | MV, 1peak | MV, 2peak | Source | |
|---|---|---|---|---|---|---|---|---|
| (kpc) | (mag) | (mag) | (mag) | (mag) | (mag) | des | ||
| Milky Way transients | ||||||||
| CK Vul (¶) | Jun 1670 to Jun 1671 | 0.7 | 2.2 | > −5.4 | – | −8.4 | −8.8 | 1;2;2 |
| V1148 Sgr (★) | ∼1943 | 2.7( ⊖ ) | 1.3 | – | – | −9.5 | – | 3;4;5 |
| V4332 Sgr (¶),(★) | 1994 | > 5.5 | 0.55 | < 2.65 | – | – | < −7.01 | 6;6;7–9 |
| V838 Mon(¶),(★),(□) | Jan 2002 to May 2002 | 6.1 | 0.85 | −1.06 | −6.68 | −9.79 | −9.46 | 10;11;12–16 |
| OGLE 2002−BLG-360(∇) | 2002 to 2006 | 8.2 | 2.00( † ) | −0.80 | −1.21 | −4.10 | −3.09 | 17;18;17 |
| V1309 Sco(¶),(★) | Jun 2008 to Mar 2010 | 3.5 | 0.55 | 3.80 | > − 0.93 | −6.56 | −5.02 | 19;20;19-21 |
| Extragalactic transients | ||||||||
| M31−RV | Jun 1988 to Oct 1988 | 0.78 | 0.12 | −5.04 | – | – | −8.69 | 23;22;22 |
| M31−LRN2015 | Jan 2015 to May 2015 | 0.78 | 0.35 | −2.13 | – | −10.16 | −8.93 | 23;23;23–25 |
| M 101−2015OT1 | < Feb 2015 to Mar 2016 | 6.4 | 0.01 | −7.19 | −10.10 | −12.70 | −11.46 | 26;4;27–29 |
| NGC 4490−2011OT1 | May 2011 to May 2012 | 9.6 | 0.32 | −7.32 | −9.18 | −14.35 | −14.54 | 30;31;23&30 |
| NGC 3437−2011OT1 | Jan 2011 to Jun 2011 | 20.9 | 0.02 | > −9.98 | > −10.83 | −13.06 | −13.33 | 32;4;29 |
| UGC 12307−2013OT1 | < Jun 2013 to Nov 2013 | 39.7 | 0.22 | > −11.88 | – | – | −15.03 | 29;4;29 |
| SN 1997bs (NGC 3627) | Apr 1997 to Jan 1998 | 9.2 | 0.21 | −7.61 | – | −13.34 | −11.51 | 29;33;29&33–35 |
| SNhunt248 (NGC 5806) | Apr 2014 to May 2015 | 22.5 | 0.04 | −8.99 | −11.18 | −14.87 | −14.07 | 36;37;37–38 |
| AT 2017jfs | Dec 2017 to Jul 2018 | 34.7 | 0.02 | > −11.26 | – | −15.46 | −14.38 | 39 |
Notes. References for the distance, reddening estimates and light curves, respectively, are identified by numbers in the last column. Additional information: (¶)
Özdönmez et al. (2016) (see their Tables 2 and 3) give the following alternative distance and reddening estimates for four Galactic RNe: d = 4.48 ± 0.24 kpc and E(B − V) = 0.75 ± 0.05 mag for CK Vul; d = 1.14 ± 1.00 kpc and E(B − V) = 0.32 ± 0.10 mag for V4332 Sgr; d = 2.5 ± 0.4 kpc and E(B − V) = 0.55 ± 0.05 mag for V1309 Sco; d ≥ 7 kpc and E(B − V) = 0.87 mag for V838 Mon. (★)As a consistency check, we also estimated the distance of Galactic RNe using the Gaia DR2 parallaxes (Gaia Collaboration et al. 2016, 2018), and obtained the following values: ω = 0.4306 ± 0.0591 mas and 
kpc for V1148 Sgr; ω = 0.0017 ± 0.2798 mas and 
kpc for V4332 Sgr; and ω = −0.0014 ± 0.1051 mas and 
kpc for V838 Mon. All of them are consistent (within the errors) with those reported in the table. ( ⊖ )We assume that V1148 Sgr is at the distance of the globular cluster NGC 6553. (▫)
Munari et al. (2005) estimated a similar reddening E(B − V) = 0.87 ± 0.02 mag, and a somewhat larger distance (d ∼ 10 kpc) to V838 Mon. ( † )Following Kochanek et al. (2014), we adopt a total reddening comprising both a Milky Way component (E(B − V)MS = 1 mag, with RV = 2.5, following Nataf et al. 2013), and a circumstellar dust component (E(B − V)CSD = 1 mag, with a standard reddening law RV = 3.1). (∇)As only the I-band light curve is well monitored at all phases, the V-band peak magnitudes were computed from the I-band magnitudes, adopting the available V − I colour information.
References. 1 = Hajduk et al. (2007); 2 = Shara et al. (1985); 3 = Minniti (1995); 4 = Schlafly & Finkbeiner (2011); 5 = Mayall (1949); 6 = Tylenda et al. (2015); 7 = Martini et al. (1999); 8 = Goranskij & Barsukova (2007, and references therein); 9 = Kimeswenger (2006); 10 = Sparks et al. (2008); 11 = Afşar & Bond (2007); 12 = Munari et al. (2002); 13 = Goranskij et al. (2002); 14 = Kimeswenger et al. (2002); 15 = Crause et al. (2003); 16 = Crause et al. (2005); 17 = Tylenda et al. (2013); 18 = Kochanek et al. (2014); 19 = Tylenda et al. (2011); 20 = Mason et al. (2010); 21 = Walter et al. (2012); 22 = Boschi & Munari (2004); 23 = Kurtenkov et al. (2015); 24 = Williams et al. (2015); 25 = From Astronomer’s Telegrams; 26 = Shappee & Stanek (2011); 27 = Goranskij et al. (2016, and references therein); 28 = Blagorodnova et al. (2017); 29 = this paper; 30 = Smith et al. (2016b); 31 = Pastorello et al. (2008); 32 = Sorce et al. (2014); 33 = Van Dyk et al. (2000); 34 = Li et al. (2002); 35 = Adams & Kochanek (2015); 36 = Tully et al. (2009); 37 = Kankare et al. (2015); 38 = Mauerhan et al. (2015); 39 = Pastorello et al. (2019).
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