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Fig. 2.


Portion of MANGA integrated spectra of Mkn 848, for the NW and SE regions, with superimposed best-fitting components. Top panels: [O III]+Hβ emission lines from the NW (left panel) and SE (right panel) regions. Central panels: He I emission line and Na ID absorption line system. Bottom panels: [N II], Hα and [S II] lines. The different sets of Gaussian components are shown with solid green curves (NC), dashed and dot-dashed blue lines (OC). Stellar continuum emission has been previously modelled with the pPXF routine and subtracted. The dotted lines mark the wavelengths of Hβ and [O III]λλ4959,5007, in the top panels, He I and Na ID doublet lines in the central panels, and [N II]λ6548, Hα, [N II]λ6581 and [S II] doublet lines in the bottom panels. The systemic redshift is defined on the basis of the best-fit solution for the NC in the NW integrated spectrum. The SE systemic lines show a velocity offset of ∼90 km s−1. The best-fits reproduce all but the Na ID NC in the NW integrated spectrum with high significance.

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