Fig. 3
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TUES, GHRS, and IUE observations compared with our final model normalized to the 2MASS H magnitude. EB−v = 0.038 ± 0.010 is applied. In addition, the B and V magnitudes (Landolt & Uomoto 2007) as well as the 2MASS J, H, and Ks magnitudes (Cutri et al. 2003) are shown. For clarity, TUES and GHRS spectra are convolved with a Gaussian with a full width at half maximum (FWHM) of 7Å.
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