Fitting to the observed spectrum of HR3126 with the central star and dust emission components. The solid black and orange lines represent the spectrum obtained with AMBER and the model spectrum, respectively. The flux of the central star and dust at the inner rim (with a dust temperature of 1400 K) predicted by the model is shown with the solid blue and red lines, respectively. The model spectra are calculated only up to 2.42 μm, beyond which the IRTF spectrum of the proxy star of HR3126 is not available.