Properties such as the star-formation rates and gas metallicities in star-forming galaxies are often derived from nebular emission lines. However, this light is strongly attenuated by dust within these galaxies. The work we are undertaking aims to accurately correct for the presence of this dust in MaNGA spirals, and measure its spatial distribution. In our sample of galaxies, we select regions where star formation is the principle source of line emission; and use the Balmer decrement as a diagnostic to quantify the dust extinction in each galaxy. We also compare extinction values derived from this dust with extinction due to the stellar populations in the MaNGA spirals. Preliminary analysis, which is presented in this poster, indicates that the ionised gas in predominantly star-forming galaxies exhibits significantly lower dust extinction than in AGN or LI(N)ER dominated ones; whereas the dust extinction measured from analysis of stellar populations is not significantly affected by the rate of star formation within a galaxy.