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Table 2

White dwarfs in which weak fields may be present.

Star names Spectral T eff log g Field detected? Ref. Field detected? strength range
type (K) (prev. work) (this work) (kG)

WD 0413−077 40 Eri B DA3 17 100 7.95 P FVB03 NA NA
WD 0446−789 BPM 3523 DA3 23 627 7.69 Y AJN04 Y −2.5 to −5.7
WD 1105−048 LTT 4099 DA3 15 142 7.85 Y AJN04, VBF06 P −7.9 to 3.3
WD 1620−391 CD–38 10980 DA2 24 231 8.07 P JAN07 N
WD 2007−303 LTT 7987 DA4 14 454 7.86 P JAN07 N
WD 2039−202 LTT 8189 DA2.5 19 188 7.93 P JAN07 N
WD 2105−820 LTT 8381 DA6 10 794 8.19 Y t.w. Y 8.1 to 11.4
WD 2359−434 LTT 9857 DA5 8544 8.44 Y AJN04 Y 3.1 to 4.1

References. Effective temperatures from Lajoie & Bergeron (2007) or Koester et al. (2009). References for the magnetic field detections are as follow: FVB03: Fabrika et al. (2003); AJN04: Aznar Cuadrado et al. (2004); VBF06: Valyavin et al. (2006); JAN07: Jordan et al. (2007); t.w.: this work.

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