Separated Fringe Packet Observations with the CHARA Array. II. Omega Andromeda, HD 178911, and Xi Cephei
NAVAL OBSERVATORY WASHINGTON DC
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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 Omega Andromeda, HD 178911, and xi Cephei with the CLIMB three-beam combiner at the CHARA Array. For these systems we determine component masses and parallax of 0.963 or - 0.049 solar mass and 0.860 or - 0.051 solar mass and 39.54 or - 1.85 mas for omega Andromeda, for HD 178911 of 0.802 or - 0.055 solar mass and 0.622 or - 0.053 solar mass with 28.26 or - 1.70 mas, and masses of 1.045 or - 0.031 solar mass and 0.408 or - 0.066 solar mass and 38.10 or - 2.81 mas for Xi Cephei.