A novel approach to measure dust attenuation at z~1

The distribution and properties of dust in galaxies, and its evolution with cosmic time remains a debated topic. We present a novel approach to measure the attenuation of z~1 galaxies: we reconstruct intrinsic stellar spectra based on deep optical spectra from the VLT/VIMOS LEGA-C survey and measure attenuation through a comparison with the multi-band photometry. We present the variation of the dust attenuation law slope and strength of the UV bump feature with galaxy orientation, specific star-formation rate (sSFR) and stellar mass for a sample of star-forming galaxies. We find diversity in dust attenuation law properties: attenuation A(4500A) increases with sSFR and stellar mass, while slope and UV bump exhibit no trends. Face-on galaxies are less attenuated, with steeper slope values, and an indication for a strong bump at low-masses. Additionally, we do not find a trend between the slope and the UV bump strength, in contrast to some local and high-redshift dust attenuation studies.