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Using a sample of dwarf irregular galaxies selected from the ALFALFA blindHI-survey and observed using the VIMOS IFU, we investigate the relationshipbetween H$\alpha$ emission and Balmer optical depth ($\tau_{\text{b}}$). Wefind a positive correlation between H$\alpha$ luminosity surface density andBalmer optical depth in 8 of 11 at $\geq$ 0.8$\sigma$ significance (6 of 11 at$\geq$ 1.0$\sigma$) galaxies. Our spaxels have physical scales ranging from 30to 80 pc, demonstrating that the correlation between these two variablescontinues to hold down to spatial scales as low as 30 pc. Using the Spearman'srank correlation coefficient to test for correlation between$\Sigma_{\text{H}\alpha}$ and $\tau_{\text{b}}$ in all the galaxies combined,we find $\rho = 0.39$, indicating a positive correlation at 4$\sigma$significance. Our low stellar-mass galaxy results are in agreement withobservations of emission line regions in larger spiral galaxies, indicatingthat this relationship is independent of the size of the galaxy hosting theemission line region. The positive correlation between H$\alpha$ luminosity andBalmer optical depth within spaxels is consistent with the hypothesis thatyoung star-forming regions are surrounded by dusty birth-clouds.

Spatial Correlation Between Dust and H$\alpha$ Emission in Dwarf Irregular Galaxies