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tokens: the BT-SETTL model grid (Allard 2014 ), where 100,000 linear combinations of three synthetic spectra were used to find the best-fit linear combination. The final parameters of the best-fit model to the MDM spectrum were T eff = 3595K, log g = 4.9 dex, and [Fe/H] = −1.1 dex. For the STIS spectrum, we found T eff = 3500 K, log g = 4.83 dex, and [Fe/H] = −1.3 dex. We trust that the temperature and gravity measurements from the model fit to the broad optical spectra because the method is well-calibrated throughout the subdwarf sequence (Lépine et al. 2007 ). 4. Metallicity. We calculated [Fe/H] for Wolf 1130A using the IRTF/SpeX spectrum and following the techniques outlined by Mann et al. ( 2013a ). That paper presented empirical relations between strong atomic lines in near-infrared M dwarf spectra and overall metallicity. These relations were calibrated using wide binaries containing an FGK primary and an M dwarf companion under the assumption of identical metallicities between binary components. In this work we adopt the mean of the H - and K -band relations [Fe/H] = −0.70 ± 0.12 as the metallicity for Wolf 1130A. Uncertainties account for Poisson errors in the spectrum as well as the scatter in the Mann et al. ( 2013a ) calibrations. The metallicity values in the literature have a large scatter but are all significantly subsolar. As shown by Neves et al. ( 2012 ), most methods for determining metallicity diverge below −0.6 dex. Rojas-Ayala et al. ( 2012 ) derive [M/H] = −0.45 ± 0.12 and [Fe/H] =−0.64 ± 0.17 from K -band indices. Other [Fe/H] calculations include −0.80 dex (Woolf et al. 2009 ), −0.87 dex (Stauffer Hartmann 1986b ), −0.89 dex (Bonfils et al. 2005 ), and −1.02 dex (Schlaufman Laughlin 2010 ). Schmidt et al. ( 2009 ) compiled [Fe/H]= −0.62 ± 0.10 and [Ti/H] = −0.22 ± 0.09 abundances for Wolf 1130A from Woolf Wallerstein ( 2006 ), who used the MOOG spectral synthesis software (Sneden 1973 ). Additionally, Schmidt et al. ( 2009 ) derived [O/H] = −0.45 ± 0.11 from TiO lines in R ∼ 30,000 optical spectra. Overall, our methods are most similar to those of Rojas-Ayala et al. ( 2012 ) and Schmidt et al. ( 2009 ) and we include their measurements in Table 4 . Employing the current version of the MOOG synthesis software with a Python wrapper, 14 14 https://bitbucket.org/madamow/pymoogi.git , written by Monika Adamow. we measured abundances in the IGRINS infrared spectrum. For this synthesis we used the parameters already identified above ( T eff = 3600 K, log g = 5, [M/H] = −1, and microturbulence = 1.0 ) to select similar atmosphere models. Our synthetic spectra employed Kurucz ( 1979 , 2011 ) models that were broadened to the instrument resolution and v sin i = 15.0 and then modulated for different atomic abundances. Figure 9 shows the K -band Ca i triplet along with synthetic abundances of [Ca/H] = −0.2 ± 0.1 dex. The 10% depths of the Ca lines, relative to the continuum, are some of the deeper lines in the infrared spectrum of