Probing star formation and ISM properties using galaxy disk inclination
  I: Evolution in disk opacity since $z\sim0.7$
  Disk galaxies at intermediate redshift ($z\sim0.7$) have been found in
previous work to display more optically thick behaviour than their local
counterparts in the rest-frame B-band surface brightness, suggesting an
evolution in dust properties over the past $\sim$6 Gyr. We compare the measured
luminosities of face-on and edge-on star-forming galaxies at different
wavelengths (Ultraviolet (UV), mid-infrared (MIR), far-infrared (FIR), and
radio) for two well-matched samples of disk-dominated galaxies: a local Sloan
Digital Sky Survey (SDSS)-selected sample at $z\sim0.07$ and a sample of disks
at $z\sim0.7$ drawn from Cosmic Evolution Survey (COSMOS). We have derived
correction factors to account for the inclination dependence of the parameters
used for sample selection. We find that typical galaxies are transparent at MIR
wavelengths at both redshifts and that the FIR and radio emission is also
transparent as expected. However, reduced sensitivity at these wavelengths
limits our analysis; we cannot rule out opacity in the FIR or radio.
Ultra-violet attenuation has increased between $z\sim0$ and $z\sim0.7$, with
the $z\sim0.7$ sample being a factor of $\sim$3.4 more attenuated. The larger
UV attenuation at $z\sim0.7$ can be explained by more clumpy dust around
nascent star-forming regions. There is good agreement between the fitted
evolution of the normalisation of the SFR$_{\text{UV}}$ versus 1-cos(i) trend
(interpreted as the clumpiness fraction) and the molecular gas fraction/dust
fraction evolution of galaxies found out to $z<1$.
