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We present VLT/VIMOS IFU observations of an occulting galaxy pair previouslydiscovered in HST observations. The foreground galaxy is a low-inclinationspiral disk, which causes clear attenuation features seen against the brightbulge and disk of the background galaxy. We find redshifts of $z=0.064\pm0.003$ and z=0.065 for the foreground and background galaxy respectively.This relatively small difference does not rule out gravitational interactionbetween the two galaxies. Emission line ratios point to a star-forming, notAGN-dominated foreground galaxy.  We fit the Cardelli, Clayton & Mathis (CCM) extinction law to the spectra ofindividual fibres to derive slope ($R_V$) and normalization ($A_V$). Thenormalization agrees with the HST attenuation map and the slope is lower thanthe Milky Way relation ($R_V<3.1$), which is likely linked to the spatialsampling of the disk. We speculate that the values of $R_V$ point to eithercoherent ISM structures in the disk larger than usual ($\sim9$ kpc) or higherstarting values of $R_V$, indicative of recent processing of the dust.  The foreground galaxy is a low stellar mass spiral ($M_* \sim 3 \times 10^9M_\odot$) with a high dust content ($M_{\rm dust} \sim 0.5 \times 10^6M_\odot$). The dust disk geometry visible in the HST image would explain theobserved SED properties of smaller galaxies: a lower mean dust temperature, ahigh dust-to-stellar mass ratio but relatively little optical attenuation.Ongoing efforts to find occulting pairs with a small foreground galaxies willshow how common this geometry is.

VLT/VIMOS Observations of an Occulting Galaxy Pair: Redshifts and Effective Extinction Curve