Estimating Dust Attenuation From Galactic Spectra. III. Radial variations of dust attenuation scaling relations in MaNGA galaxies

Abstract: We investigate the radial dependence of the scaling relations of dust attenuation in nearby galaxies using integral field spectroscopy (IFS) data from MaNGA. We identify ionized gas regions of kpc sizes from MaNGA galaxies, and for each region we estimate both the stellar attenuation $E(B-V){\rm star}$ and gas attenuation $E(B-V){\rm gas}$. We then quantify the correlations of 15 regional/global properties with $E(B-V){\rm gas}$ and $E(B-V){\rm star}$, using both the feature importance obtained with the Random Forest regression technique and the Spearman correlation coefficients. The importance of stellar mass, metallicity and nebular velocity dispersion found previously from SDSS-based studies can be reproduced if our analysis is limited to the central region of galaxies. The scaling relations of both $E(B-V){\rm gas}$ and $E(B-V){\rm star}$ are found to strongly vary as one goes from the galactic center to outer regions, and from H$\alpha$-bright regions to H$\alpha$-faint regions. For $E(B-V){\rm gas}$, [NII]/[SII] is top ranked with a much higher correlation coefficient than any other property at $0<R\lesssim R_e$, while [OIII]/[OII] outperforms [NII]/[SII] as the leading property in the outermost region. For $E(B-V){\rm star}$, stellar age shows the strongest correlation with no/weak dependence on radial distance, although $\rm \Sigma_{H\alpha}$ and sSFR present similarly strong correlations with $E(B-V){\rm star}$ in the galactic center. We find H$\alpha$-bright regions to generally show stronger correlations with $E(B-V){\rm gas}$, while H$\alpha$-faint regions are more strongly correlated with $E(B-V)_{\rm star}$, although depending on individual properties and radial distance. The implications of our results on studies of high-$z$ galaxies are discussed.