  We present a novel approach to measure the attenuation curves of 485
individual star-forming galaxies with M$_*$ $>$ 10$^{10}$ M$_{\odot}$ based on
deep optical spectra from the VLT/VIMOS LEGA-C survey and multi-band photometry
in the COSMOS field. Most importantly, we find that the attenuation curves in
the rest-frame $3000-4500$A range are typically almost twice as steep as the
Milky Way, LMC, SMC, and Calzetti attenuation curves, which is in agreement
with recent studies of the integrated light of present-day galaxies. The
attenuation at $4500$A and the slope strongly correlate with the galaxy
inclination: face-on galaxies show less attenuation and steeper curves compared
to edge-on galaxies, suggesting that geometric effects dominate observed
variations in attenuation. Our new method produces $2175$A UV bump detections
for 260 individual galaxies. Even though obvious correlations between UV bump
strength and global galaxy properties are absent, strong UV bumps are most
often seen in face-on, lower-mass galaxies (10 $<$
log$_{10}$(M$_*$/M$_{\odot}$) $<$ 10.5) with low overall attenuation. Finally,
we produce a typical attenuation curve for star-forming galaxies at $z\sim0.8$;
this prescription represents the effect of dust on the integrated spectral
energy distributions of high-redshift galaxies more accurately than commonly
used attenuation laws.
