Probing star formation and ISM properties using galaxy disk inclination
  II: Testing typical FUV attenuation corrections out to z$\sim$0.7
  We evaluate dust-corrected far ultraviolet (FUV) star formation rates (SFRs)
for samples of star-forming galaxies at $z\sim0$ and $z\sim0.7$ and find
significant differences between values obtained through corrections based on UV
colour, from a hybrid mid-infrared (MIR) plus FUV relation, and from a
radiative transfer based attenuation correction method. The performances of the
attenuation correction methods are assessed by their ability to remove the
dependency of the corrected SFR on inclination, as well as returning, on
average, the expected population mean SFR. We find that combining MIR
(rest-frame $\sim$13$\mu$m) and FUV luminosities gives the most inclination
independent SFRs and reduces the intrinsic SFR scatter out of the methods
tested. However, applying the radiative transfer based method of Tuffs et al.
gives corrections to the FUV SFR that are inclination independent and in
agreement with the expected SFRs at both $z\sim0$ and $z\sim0.7$. SFR
corrections based on the UV-slope perform worse than the other two methods
tested. For our local sample, the UV-slope method works on average but does not
remove inclination biases. At $z\sim$0.7 we find that the UV-slope correction
used locally flattens the inclination dependence compared to the raw FUV
measurements but was not sufficient to correct for the large attenuation
observed at $z\sim$0.7.
