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Fig. 2


Observed 1D spectra of AGNs in grey and best fit in red. From the top AGN5, BzK25, AGN26, z2LAE3. Vertical dashed lines represent the wavelengths of sky line residuals. The blue curve is the sky spectrum by Rousselot et al. (2000), which indicates the relative intensity of the OH emission lines. It has been scaled according to the panel axis to be visible. [OIII] doublet (Hα) wavelength ranges are presented in the left (right) panels.

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