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28 June 2006 The star 12 Persei and separated fringe packet binaries (SFPB)
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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, an example of a Separated Fringe Packet Binary. We describe the data reduction process involved. By using a technique we have developed of 'side-lobe verniering', we can obtain an improved precision in separation of up to 25 micro-arcsec along a given baseline. For this object we find a semi-major axis 0.3 of Barlow, Scarfe, and Fekel (1998) [BSF], but with an increased inclination angle. The revised masses are therefore almost 6% greater than those of BSF. 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%. We expect that improved RVs and improved absolute calibration can bring down the mass errors to below 1%.
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William G. Bagnuolo Jr., Theo A. ten Brummelaar, H. A. McAlister, Douglas R. Gies, and Stephen T. Ridgway "The star 12 Persei and separated fringe packet binaries (SFPB)", Proc. SPIE 6268, Advances in Stellar Interferometry, 62682T (28 June 2006); https://doi.org/10.1117/12.672275
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