Near–infrared ( 2.2 µm ) long baseline interferometric observations of Vega are presented .
The stellar disk of the star has been resolved , and the data have been fitted with a limb darkened stellar disk of diameter \Theta _ { LD } = 3.28 \pm 0.01 mas .
The derived effective temperature is T _ { eff } = 9553 \pm 111 K. However , the residuals resulting from the stellar disk model appear to be significant and display organized structure .
Instrumental artifacts , stellar surface structure , stellar atmosphere structure , and extended emission/scattering from the debris disk are discussed as possible sources of the residuals .
While the current dataset can not uniquely determine the origin of the residuals , the debris disk is found to be the most likely source .
A simple debris disk model , with 3-6 % of Vega ’ s flux emanating from the disk at r \lesssim 4 AU , can explain the residuals .