2026AJ....171..193S

Theoretical models of low-mass stars continue to be discrepant with observations when used to examine the mass-radius relationship and other physical parameters of individual stars. High-resolution spectroscopy that leads to dynamical measurements of binary stars can directly improve these models. We have been using the Habitable-Zone Planet Finder spectrograph to monitor binary stars with M dwarf components. Here, we measure the orbital and stellar parameters for three such systems: LSPM J0515+5911, NLTT 43564, and NLTT 45468. Each system has dozens of spectra obtained over a baseline of several years. None of the systems appear to be eclipsing, so our ability to turn them into true benchmark binaries with purely dynamical measurements is limited. We use literature photometry to estimate each system's spectral energy distribution and utilize models in combination with detection limits of our spectroscopic measurements to probe characteristics of the companions. LSPM J0515+5911 is a double-lined spectroscopic binary with a period of 126.948 ± 0.029 days and derived minimum masses, ${M}_{1}{\sin }^{3}i=0.058\pm 0.002$M_⊙ and ${M}_{2}{\sin }^{3}i=0.046\pm 0.001$M_⊙for the primary and secondary components, respectively. We solved NLTT 43564 with a period of 1877 ± 24 days and NLTT 45468 with a period of 9.686 ± 0.001 days as single lined systems and modeled the primary masses to be M₁ = 0.32 ± 0.02 M_⊙ and ${M}_{1}=0.3{5}_{-0.07}^{+0.02}$M_⊙, respectively.