First Results from the CHARA Array. V. Binary Star Astrometry: The Case of 12 Persei

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Abstract

We have obtained high-resolution orbital data with the CHARA Array for the bright star 12 Persei, a resolved double-lined spectroscopic binary. We describe the data reduction process, which can give precision in separation of up to 25 μas along a given baseline. For this object we find a semimajor axis of a = 53.18 ± 0.15 mas, which is 0.3% smaller than that of Barlow and coworkers, but with much improved precision. The inclination angle i increases to 12817 ± 014, compared to 12677 ± 056 of Barlow and coworkers, again with better precision. We also found an intensity ratio for the components in the K' band (λ = 2.13 μm) of r = 0.72 ± 0.01, or ΔK' = 0.409 ± 0.013, after allowing for the partial resolution of the components. Assuming the spectral types of the components, we find that Pub Lclchangemark="ins">ΔV = 0.51, as compared to 0.57 by Barlow and coworkers. The revised masses (Pub Lclchangemark="ins">Mp = 1.382 ± 0.019 and Ms = 1.240 ± 0.017 M⊙) are found to be 5.8% larger than those of Barlow and coworkers, and the components are thus even more overmassive. The overall accuracy in the masses is about 1.3%, now primarily limited by the spectroscopically determined radial velocities. The precision of the masses due to the interferometrically derived "visual" orbit alone is only about 0.2%.

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