Context : Protoplanetary disks are the birth environments of planetary systems .
Therefore , the study of young , circumstellar environments is essential to understanding the processes taking place in planet formation and the evolution of planetary systems .

Aims : We detect and characterize circumstellar disks and potential companions around solar-type , pre-main sequence stars in the Scorpius-Centaurus association ( Sco-Cen ) .

Methods : As part of our ongoing survey we carried out high-contrast imaging with VLT/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 Crux subgroup of Sco-Cen .
For the total intensity images , we remove the stellar halo via an approach based on reference star differential imaging in combination with principal component analysis .

Results : Both total intensity and polarimetric data resolve a disk around the young , solar-like Sco-Cen member Wray~15-788 .
Modeling of the stellar spectral energy distribution suggests that this is a protoplanetary disk at a transition stage .
We detect a bright outer ring at a projected separation of \sim 370 mas ( \approx 56 au ) , hints of inner substructures at \sim 170 mas ( \approx 28 au ) , and a gap in between .
Within a position angle range of only 60° ¡ \phi ¡ 240° , we are confident at the 5 \sigma level that we detect actual scattered light flux from the outer ring of the disk ; the remaining part is indistinguishable from background noise .
For the detected part of the outer ring we determine a disk inclination of i = 21° \pm 6°and a position angle of \varphi = 76° \pm 16° .
Furthermore , we find that Wray~15-788 is part of a binary system with the A2V star HD~98363 at a separation of \sim 50″ ( \approx 6900 au ) .

Conclusions : The detection of only half of the outer ring might be due to shadowing by a misaligned inner disk .
A potential substellar companion can cause the misalignment of the inner structures and can be responsible for clearing the detected gap from scattering material .
However , we can not rule out the possibility of a non-detection due to our limited signal-to-noise ratio , combined with brightness azimuthal asymmetry .
From our data we can exclude companions more massive than 10 M _ { \text } { jup } within the gap at a separation of \sim 230 mas ( \approx 35 au ) .
Additional data are required to characterize the disk ’ s peculiar morphology and to set tighter constraints on the potential perturber ’ s orbital parameters and mass .