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When observed with optical long-baseline interferometers (OLBI), componentsof a binary star which are sufficiently separated produce their owninterferometric fringe packets; these are referred to as Separated FringePacket (SFP) binaries. These SFP binaries can overlap in angular separationwith the regime of systems resolvable by speckle interferometry at single,large-aperture telescopes and can provide additional measurements forpreliminary orbits lacking good phase coverage, help constrain elements ofalready established orbits, and locate new binaries in the undersampled regimebetween the bounds of spectroscopic surveys and speckle interferometry. In thisprocess, a visibility calibration star is not needed, and the separated fringepackets can provide an accurate vector separation. In this paper, we apply theSFP approach to {\omega} Andromeda, HD 178911, and {\xi} Cephei with the CLIMBthree-beam combiner at the CHARA Array. For these systems we determinecomponent masses and parallax of 0.963${\pm}$0.049 $M_{\odot}$ and0.860${\pm}$0.051 $M_{\odot}$ and 39.54${\pm}$1.85 milliarcseconds (mas) for{\omega} Andromeda, for HD 178911 of 0.802${\pm}$0.055 $M_{\odot}$ and0.622${\pm}$0.053 $M_{\odot}$ with 28.26${\pm}$1.70 mas, and masses of1.045${\pm}$0.031 $M_{\odot}$ and 0.408${\pm}$0.066 $M_{\odot}$ and38.10${\pm}$2.81 mas for {\xi} Cephei.

Separated Fringe Packet Observations with the CHARA Array II: $\omega$ Andromeda, HD 178911, and {\xi} Cephei