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We investigate the dust attenuation in both stellar populations and ionizedgas in kpc-scale regions in nearby galaxies, using integral field spectroscopydata from MaNGA MPL-9. We identify star-forming (HII) and diffuse ionized gas(DIG) regions from MaNGA datacubes. From the stacked spectrum of each region,we measure the stellar attenuation, $E(B-V)_{\rm star}$, using the techniquedeveloped by Li et al.(2020), as well as the gas attenuation, $E(B-V)_{\rmgas}$, from the Balmer decrement. We then examine the correlation of$E(B-V)_{\rm star}$, $E(B-V)_{\rm gas}$, $E(B-V)_{\rm gas}-E(B-V)_{\rm star}$and $E(B-V)_{\rm star}/E(B-V)_{\rm gas}$ with 16 regional/global properties,and for regions with different $\rm H{\alpha}$ surface brightnesses($\Sigma_{\rm H\alpha}$). We find a stronger correlation between $E(B-V)_{\rmstar}$ and $E(B-V)_{\rm gas}$ in regions of higher $\Sigma_{\rm H\alpha}$.Luminosity-weighted age ($t_L$) is found to be the property that is the moststrongly correlated with $E(B-V)_{\rm star}$, and consequently with$E(B-V)_{\rm gas}-E(B-V)_{\rm star}$ and $E(B-V)_{\rm star}/E(B-V)_{\rm gas}$.At fixed $\Sigma_{\rm H\alpha}$, $\log_{10}t_L$ is linearly and negativelycorrelated with $E(B-V)_{\rm star}/E(B-V)_{\rm gas}$ at all ages. Gas-phasemetallicity and ionization level are important for the attenuation in the gas.Our results indicate that the ionizing source for DIG regions is likelydistributed in the outer-skirt of galaxies, while for HII regions our resultscan be well explained by the two-component dust model of Charlot & Fall (2000).

Estimating dust attenuation from galactic spectra. II. Stellar and gas attenuation in star-forming and diffuse ionized gas regions in MaNGA