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Table 2

Summary of key parameters of the binary systems observed.

Object M1 M2 incl Teff a Sp. Type RMS logg K1 Reference
(M) (M) (degs) (K) (R) (M2) (Residuals) (km s−1)
EC 10246-2707 0.45 0.12 80.0 28 900 0.84 M5/M6 1.60 5.64 71.6 −2.50 Barlow et al. (2013)
HS 0705+6700 0.48 0.13 84.4 28 800 0.81 M4/M5 19.89 5.40 85.8 −2.68 Drechsel et al. (2001)
HS 2231+2441 0.265 0.05 79.1 28 370 1.18 BD 2.47 5.39 49.1 −2.91 Ostensen et al. (2008)
J08205+0008 0.25 0.045 85.9 26 700 0.6 BD 1.13 5.48 47.4 Geier et al. (2011)
/0.47 /0.068 /1.1
NSVS 07826147 0.376 0.113 86.6 29 230 M5 2.41 5.58 71.1 For et al. (2010)
NSVS 14256825 0.35 0.097 82.5 42 300 0.74 M5/M7 20.95 5.50 73.4 −2.52 Almeida et al. (2012)
/0.46 /0.21 /35 250 /5.49 /−2.70 Kilkenny & Koen (2012)
NY Vir 0.39 0.11 80.7 31 300 0.72 M5 4.78/36.45 5.74 78.6 −2.91 Vuckovic et al. (2007)

Notes. The spectral types for these systems are not clearly defined, being indirectly determined from light curve parameters which themselves can be poorly constrained. The RMS of residuals for NY Vir is shown with two values. Utilising all data the value is 36.45, but eliminating the two Vuckovic data points, which Lee et al. (2014) reports with very low uncertainties, yields a value of 4.78.

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