Fig. 11.
From left to right: Brγ, H2(1–0)S(1)λ2.122 μm, and [Fe II] emission line fits detected in the nuclear aperture of radius 
. The original spectra are shown in black, the fitted model in blue, and the residuals are shown in grey. For the Brγ emission line a double-Gaussian fit is used as explained in Sect. 3.5.2. The stellar continuum is not subtracted in the spectra shown.
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