Abstract Accurate spatially resolved dust corrections are critical for interpreting the structure and evolution of star-forming galaxies (SFGs). We present an empirical model for predicting spatially resolved dust attenuation (AV) in SFGs using integral field spectroscopy from the Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) survey. Using a sample of 5 155 galaxies over 7. 20 M_* 11. 14 and 0. 0002 z 0. 1444, we derive AV maps from the Balmer decrement across more than 1 898 954 star-forming spaxels. Using local star formation rate surface density (ₒ₅ₑ) as a predictor, the model achieves R² = 0. 69 and RMSE =0. 22 mag, with residuals that are approximately Gaussian and centred near zero. It predicts AV within a factor of 1. 3 on kpc scales. We also demonstrate that the relation can be applied iteratively to recover dust–corrected ₒ₅ₑ from uncorrected values, converging by the fourth iteration with minimal residual bias (-0. 01 mag) and low RMSE (0. 42 mag). The model accurately reproduces AV maps across diverse morphologies and orientations, including edge-on systems. It also recovers the observed radial AV profiles, capturing their dependence on stellar mass and relative star formation activity, with more massive and more strongly star-forming galaxies showing steeper gradients.
Mailvaganam et al. (Thu,) studied this question.