When observed with optical long-baseline interferometers ( OLBI ) , components of a binary star which 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 separated fringe packets 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 \pm 0.049 M _ { \odot } and 0.860 \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 } and 0.622 \pm 0.053 M _ { \odot } with 28.26 \pm 1.70 mas , and masses of 1.045 \pm 0.031 M _ { \odot } and 0.408 \pm 0.066 M _ { \odot } and 38.10 \pm 2.81 mas for \xi  Cephei .