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Fig. 9

image

Theoretical spectra convolved and re-binned at different resolutions (Spitzer, IRS, R = 600; JWST MIRI, R = 3000 at 5.5 μm; VLT VISIR, R = 25 000), and zoom in the 26 μm region. The ranges adopted are the same as the instruments spectrographs. VISIR is ground-based, and the main limits are due to atmospheric transmission: we plotted only the region in which the transmissivity is 80%. The Spitzer spectrum with noise is also plotted in magenta. The strong feature at 12.93 μm in the VISIR modelled spectrum of a T Tauri star disk is due to H2 (J = 7−6, v = 0). Water lines contributing to the blends at 26 μm are indicated by vertical red arrows.

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