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(Abridged) In this paper, we use the Tuffs et al. attenuation - inclinationmodels in ultraviolet (UV), optical, and near-infrared (NIR) bands toinvestigate the average global dust properties in galaxies as a function ofstellar mass $M_{*}$, stellar mass surface density $\mu_{*}$, star-formationrate $SFR$, specific star-formation rate $sSFR$, star-formation main-sequenceoffset $dMS$, and star-formation rate surface density $\Sigma_{SFR}$ atredshifts $z \sim 0$ and $z \sim 0.7$. We use star-forming galaxies from SDSS($\sim$ 20000) and GAMA ($\sim$ 2000) to form our low-z sample at $0.04 < z <0.1$ and star-forming galaxies from COSMOS ($\sim$ 2000) for the sample at $0.6<z < 0.8$. We find that galaxies at $z \sim 0.7$ have higher optical depth$\tau_{B}^{f}$ and clumpiness $F$ than galaxies at $z \sim 0$. The increase in$F$ hints that the stars of $z \sim 0.7$ galaxies are less likely to escapetheir birth cloud, which might indicate that the birth clouds are larger. Wealso found that $\tau_{B}^{f}$ increases with $M_{*}$ and $\mu_{*}$independentof sample and therefore redshift. We found no clear trends in $\tau_{B}^{f}$ or$F$ with $SFR$, which could imply that the dust mass distribution isindependent of $SFR$. In turn, this would imply that the balance of dustformation and destruction is independent of the $SFR$. Based on an analysis ofthe inclination-dependence of the Balmer decrement, we find that reproducingthe Balmer line emission requires not only a completely optically thick dustcomponent associated with star forming regions, as in the standard Tuffs et al.model, but an extra component of optically thin dust within the birth clouds.This new component implies the existence of dust inside HII regions thatattenuates the Balmer emission before it escapes through gaps in the birthcloud and we find it is more important in high-mass galaxies.

astronomy and astrophysics

Probing star formation and ISM properties using galaxy disk inclination  III: Evolution in dust opacity and clumpiness between redshift 0.0 < z < 0.7  constrained from UV to NIR