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First Results from the CHARA Array. VII. Long‐Baseline Interferometric Measurements of Vega Consistent with a Pole‐On, Rapidly Rotating Star

  • Authors: J. P. Aufdenberg, A. Mérand, V. Coudé du Foresto, O. Absil, E. Di Folco, P. Kervella, S. T. Ridgway, D. H. Berger, T. A. ten Brummelaar, H. A. McAlister, J. Sturmann, L. Sturmann, and N. H. Turner

Aufdenberg et al. 2006 The Astrophysical Journal 645 664.

  • Provider: AAS Journals

Caption: Fig. 6.

Constraints on model parameters from the CHARA/FLUOR data. (a) Reduced ﹩\chi ^{2}﹩ values ﹩\chi ^{2}_{\nu }﹩ from the Roche‐von Zeipel model fit to the squared visibility data as a function the fraction of the critical angular break‐up rate, ﹩\omega =\Omega / \Omega _{\mathrm{crit}\,}﹩, for fixed values of the polar effective temperature ﹩T^{\mathrm{pole}\,}_{\mathrm{eff}\,}﹩ and polar surface gravity ﹩\mathrm{log}\,\left(g\right)_{\mathrm{pole}\,}﹩. The dashed line denotes the 1 ﹩\sigma ﹩ confidence region for ﹩\omega ﹩ from the ﹩F﹩ test for 24 degrees of freedom relative to the best fit at ﹩\chi ^{2}_{\nu }=1.31﹩. For each ﹩\omega ﹩, ﹩\chi ^{2}_{\nu }﹩ values are plotted for 18 position angles ﹩\psi ﹩ (0° to 170° in 10° steps; see Fig. 4). (b) Relationship between the best‐fit equatorial angular diameter ﹩\theta _{\mathrm{equ}\,}﹩ at each ﹩\omega ﹩ for the range of position angles. The dashed lines provide an estimate for the 1 ﹩\sigma ﹩ range in ﹩\omega ﹩ and the corresponding range in the equatorial angular diameter.

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