Table 2
Known WDs in the solar neighbourhood that are part of triples and quadruples.
| Distance [pc] | Spectral | Mass [M⊙] | log L/L⊙ | Companion | Spectral | Angular | References | |
| type | name | type | separation [′′] | |||||
|
|
||||||||
| 0101+048 | 21.3 (1.7) | DA6.3 | 0.36 (0.05) | –2.96 | – | DC | see text | 1, 2, 3, 4 |
| HD 6101 | K3+K8 | 1276 | ||||||
| 0326−273 | 17.4 (4.3) | DA5.9 | 0.45 (0.18) | –2.97 | – | DC8 | P = 1.88d | 4, 5, 6 |
| GB 1060B | M3.5 | 7 | ||||||
| 0413−077 | 4.984 (0.006) | DA3.1 | 0.59 (0.03) | –1.85 | 40 Eri A | K0.5 | 83.4 | 7, 8, 9, 10 |
| 40 Eri C | M4.5 | 11.9 | ||||||
| 0433+270 | 17.48 (0.13) | DA9 | 0.62 (0.02) | –3.87 | V833 Tau | K214 | 123.9 | 4, 8, 11, 12, 13, 14 |
| 0727+482A | 11.1 (0.1) | DC10 | 0.51 (0.01) | –4.01 | WD0727+482B | DC10.1 | 0.656 | 9, 15, 16, 17 |
| G107–69 | M5∗ | 103.2 | ||||||
| 0743−336 | 15.2 (0.1) | DC10.6 | 0.55 (0.01) | –4.23 | 171 Pup A | F9 | 870 | 8, 18, 19, 20 |
| 1633+572 | 14.4 (0.5) | DQpec8.1 | 0.57 (0.04) | –3.75 | CM draconis | M4.5∗ | 26 | 20, 21 |
| 2054−050 | 16.09 (0.14) | DC11.6 | 0.37 (0.06) | –4.11 | Ross 193 | M3.0 | 15.1 | 4, 10, 11, 12, 22, 23 |
| 2351−335 | 22.90 (0.75)9,25 | DA5.7 | 0.58 (0.03) | –3.03 | LDS826B | M3.5 | 6.6 | 4, 6, 24, 25, 26 |
| LDS826C | M8.5 | 103 | ||||||
Notes. The distances, spectral types, masses, and luminosities are taken from Giammichele et al. (2012). For the unresolved systems, the period P is given instead of angular separation. 1Saffer et al. (1998); 2Maxted et al. (2000); 3Caballero (2009); 4Giammichele et al. (2012); 5Nelemans et al. (2005); 6Luyten (1949); 7Holberg et al. (2012); 8Holberg et al. (2013); 9Sion et al. (2014); 10 Discovery and Evaluation of Nearby Stellar Embers (DENSE) project, http://www.DenseProject.com; 11Tremblay et al. (2017); 12Gaia Collaboration (2016); 13Hartmann et al. (1981); 14Tokovinin et al. (2006); 15Strand et al. (1976); 16Harrington et al. (1981); 17Buscombe & Foster (1998); 18Hartkopf et al. (2012); 19Tokovinin et al. (2012); 20Limoges et al. (2015); 21Morales et al. (2009); 22van Biesbroeck (1961); 23Tamazian & Malkov (2014); 24Scholz et al. (2004); 25Farihi et al. (2005); 26Subasavage et al. (2009); (∗) Spectral type corresponds to an unresolved binary.
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