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The surface brightness - color relationship (SBCR) is a poweful tool fordetermining the angular diameter of stars from photometry. It was for instanceused to derive the distance of eclipsing binaries in the Large Magellanic Cloud(LMC), which led to its distance determination with an accuracy of 1%. Wecalibrate the SBCR for red giant stars in the 2.1 < V-K < 2.5 color range usinghomogeneous VEGA/CHARA interferometric data secured in the visible domain, andcompare it to the relation based on infrared interferometric observations,which were used to derive the distance to the LMC. Observations of eight G-Kgiants were obtained with the VEGA/CHARA instrument. The derived limb-darkenedangular diameters were combined with a homogeneous set of infrared magnitudesin order to constrain the SBCR. The average precision we obtain on thelimb-darkened angular diameters of the eight stars in our sample is 2.4%. Forthe four stars in common observed by both VEGA/CHARA and PIONIER/VLTI, we finda 1 sigma agreement for the angular diameters. The SBCR we obtain in thevisible has a dispersion of 0.04 magnitude and is consistent with the onederived in the infrared (0.018 magnitude). The consistency of the infrared andvisible angular diameters and SBCR reinforces the result of 1% precision andaccuracy recently achieved on the distance of the LMC using theeclipsing-binary technique. It also indicates that it is possible to combineinterferometric observations at different wavelengths when the SBCR iscalibrated.

astronomy and astrophysics

Calibrating the surface brightness - color relation for late-type red  giants stars in the visible domain using VEGA/CHARA interferometric  observations