Results of our spectro-astrometric analysis for HE 934+0119 from the MUSE IFU observations. We have mapped the surface brightness within the central 3″ for all spectral components in the brightest spectrum assuming fixed kinematics. Here we only show the measure light distribution from the BLR Hβ (left), broad [O III] wing (middle), and narrow [O III] core (right) component. Those 2D light distributions are fitted with a 2D Moffat profile. The red cross indicates the Moffat center for the best-fit elliptical Moffat model to the surface brightness map of the BLR Hβ. The green and red crosses indicate the Moffat centers for the best-fit elliptical Moffat models to the surface brightness maps of the [O III] wing and core, in which the amplitude and position of the Moffat model were varied only. The histograms show the distributions of the normalized residuals (residual/error) for both the core and wing components in comparison to the BLR Hβ one.