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As part of our on-going survey we have carried out high-contrast imaging withVLT/SPHERE/IRDIS to obtain polarized and total intensity images of the young($11^{+16}_{-7}$Myr old) K3IV star Wray 15-788 within the Lower Centaurus Cruxsubgroup of Sco-Cen. For the total intensity images, we remove the stellar haloby an approach based on reference star differential imaging in combination withprincipal component analysis. Both total intensity and polarimetric dataresolve a disk around Wray 15-788. Modeling of the stellar spectral energydistribution suggests that this is a protoplanetary disk at a transition stage.We detect a bright, outer ring at a projected separation of $\sim$370mas($\approx$56au), hints for inner substructures at $\sim$170mas ($\approx$28au)and a gap in between. Only within a position angle range of$60^\circ<\varphi<240^\circ$, we are confident at 5$\sigma$ level to detectactual scattered light flux from the outer ring of the disk; the remaining partis indistinguishable from background noise. For the detected part of the outerring we determine a disk inclination of $i$=21$^\circ\pm$6$^\circ$ and aposition angle of $\varphi$=76$^\circ\pm$16$^\circ$. Furthermore, we find thatWray 15-788 is part of a binary system with the A2V star HD 98363 at aseparation of $\sim$50'' ($\approx$6900au). The detection of only half of theouter ring might be due to shadowing by a misaligned inner disk. A potentialsubstellar companion can cause the misalignment of the inner structures and canbe responsible for clearing the detected gap from scattering material. We cannot, however, rule out the possibility of a non-detection due to our limitedsignal to noise ratio, combined with brightness azimuthal asymmetry. From ourdata, we can exclude companions more massive than 10$M_\mathrm{jup}$ within thegap at a separation of $\sim$230mas ($\approx$35au).

Discovery of a directly imaged disk in scattered light around the Sco-Cen member Wray 15-788