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We present a novel approach to measure the attenuation curves of 485individual star-forming galaxies with M$_*$ $>$ 10$^{10}$ M$_{\odot}$ based ondeep optical spectra from the VLT/VIMOS LEGA-C survey and multi-band photometryin the COSMOS field. Most importantly, we find that the attenuation curves inthe rest-frame $3000-4500$A range are typically almost twice as steep as theMilky Way, LMC, SMC, and Calzetti attenuation curves, which is in agreementwith recent studies of the integrated light of present-day galaxies. Theattenuation at $4500$A and the slope strongly correlate with the galaxyinclination: face-on galaxies show less attenuation and steeper curves comparedto edge-on galaxies, suggesting that geometric effects dominate observedvariations in attenuation. Our new method produces $2175$A UV bump detectionsfor 260 individual galaxies. Even though obvious correlations between UV bumpstrength and global galaxy properties are absent, strong UV bumps are mostoften 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 spectralenergy distributions of high-redshift galaxies more accurately than commonlyused attenuation laws.

Dust Attenuation Curves at z $\sim$ 0.8 from LEGA-C: Precise Constraints on the Slope and 2175$\AA$ Bump Strength