2014AJ....148...48F

When observed with optical long-baseline interferometers, components of a binary star that are sufficiently separated produce their own interferometric fringe packets; these are referred to as separated fringe packet (SFP) binaries. These SFP binaries can overlap in angular separation with the regime of systems resolvable by speckle interferometry at single, large-aperture telescopes and can provide additional measurements for preliminary orbits lacking good phase coverage, help constrain elements of already established orbits, and locate new binaries in the undersampled regime between the bounds of spectroscopic surveys and speckle interferometry. In this process, a visibility calibration star is not needed, and the SFPs can provide an accurate vector separation. In this paper, we apply the SFP approach to ω Andromeda, HD 178911, and ξ Cephei with the CLIMB three-beam combiner at the CHARA Array. For these systems we determine component masses and parallax of 0.963±0.049 M_☉ and 0.860±0.051 M_☉ and 39.54±1.85 mas for ω Andromeda, for HD 178911 of 0.802±0.055 M_☉and 0.622±0.053 M_☉with 28.26±1.70 mas, and masses of 1.045±0.031 M_☉and 0.408±0.066 M_☉and 38.10±2.81 mas for ξ Cephei.