Studying the chemical composition in the ISM is vital for understanding galaxy evolution. In nearby galaxies, direct methods are commonly used to measure metallicities. However, the non-uniform electron temperature (Te) in the ISM poses challenges with spatial variations. This leads to an overestimation of Te and underestimation of abundance, causing abundance discrepancy, when averaging across entire nebulae. We need to study close, resolved objects to address this issue. The LVM survey provides detailed view of the galaxy ISM for this research. To explore the LVM instrument's capabilities, identify suitable diagnostics and regions of interest. Using LVM data simulator, I analyzed Te-sensitive ratios by generating mock observations of simulated nebulae and successfully reconstructed the large-scale Te profile of nebulae. Investigation of the Te structure shows that low-ionization species ([NII], [SII], [OII]) primarily trace the outer regions but fail to capture Te gradients, while, high-ionization species ([OIII], [SIII]) effectively trace the inner Te gradient. The chemical composition is also found to be sensitive to errors and fluctuations in Te, hence, to recover small-scale variations I introduce fluctuations at a smaller scale to relevant lines’ emissivity in the data cube. Combining these fluctuations with the true Te-sensitive lines’ emissivity data cube allows visualizing the impact of Te structure variations on integrated chemical abundances of the nebulae in 3D.
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