We demonstrate the importance of radio selection in probing heavily obscured galaxy populations. Using Evolutionary Map of the Universe (EMU) Early Science data in the Galaxy and Mass Assembly (GAMA) G23 field together with GAMA and Wide-field Infrared Survey Explorer (WISE) data, we demonstrate that the radio detected population has on average higher levels of obscuration than the parent optical sample. This arises through missing the lowest Balmer decrement (BD) and lowest mass galaxies, which are also the lower star formation rate (SFR) and metallicity systems. Possible explanations include speculation around steeper stellar initial mass functions in low mass, low SFR galaxies. 

We further investigate the link between dust obscuration and SFR estimators using Halpha luminosities and radio luminosities. We explore this by drawing on dust estimates using both the BD and the dust mass, demonstrating systematic underlying dependencies with the radio-to-Halpha ratio. Defining two novel dust geometry metrics by combining the BD and dust mass, we confirm their utility as a way to quantify dust geometry. We use this approach to establish an improved estimator for the Halpha SFR that accounts for optically thick dust. We also establish a strong correlation between specific SFR and the dust opacity and geometry in galaxies.

Additionally, we present a tool designed to model current astronomical fibre positioning systems. Through a systematic analysis of both observational and instrumentation parameter spaces, we evaluate fibre allocation efficiency across multiple visits. This analysis provides valuable insights for designing next-generation multi-object spectroscopy instrumentation for future telescopes.