Distribution of the line ratios for all LIRGs in the log(FeII]1.64 μm/Brγ) − log(H₂2.12 μm/Brγ) plane for different types of regions: high surface brightness clumps and nucleus (left panel), for the diffuse, AGN and non-AGN, extended regions (central panel), and for the compact and diffuse AGN medium in LIRGs and low-z Seyferts (right panel). The blue and green lines indicate new upper limits for young star-forming regions and Seyferts as derived from the compact, high surface brightness regions in our LIRG prototypes (see Fig. 5). For comparison, the two broken lines represent the limits for the starbursts and Seyferts previously identified by Riffel and coworkers (Riffel et al. 2013a) based on 1D spectroscopy. Contours contain 25%, 50%, 75%, and 90% of the points for each class.