Context : While planet formation is thought to occur early in the history of a protoplanetary disk , the presence of planets embedded in disks , or of other processes driving disk evolution , might be traced from their imprints on the disk structure .

Aims : We study the morphology of the disk around the T Tauri star HD 143006 , located in the \sim 5-11 Myr-old Upper Sco region , and we look for signatures of the mechanisms driving its evolution .

Methods : We observed HD 143006 in polarized scattered light with VLT/SPHERE at near-infrared ( J -band , 1.2 \mu m ) wavelengths , reaching an angular resolution of \sim 0.037″ ( \sim 6 au ) .
We obtained two datasets , one with a 145 mas diameter coronagraph , and the other without , enabling us to probe the disk structure down to an angular separation of \sim 0.06″ ( \sim 10 au ) .

Results : In our observations , the disk of HD 143006 is clearly resolved up to \sim 0.5″ and shows a clear large-scale asymmetry with the eastern side brighter than the western side .
We detect a number of additional features , including two gaps and a ring .
The ring shows an overbrightness at a position angle ( PA ) of \sim 140 ^ { \circ } , extending over a range in position angle of \sim 60 ^ { \circ } , and two narrow dark regions .
The two narrow dark lanes and the overall large-scale asymmetry are indicative of shadowing effects , likely due to a misaligned inner disk .
We demonstrate the remarkable resemblance between the scattered light image of HD 143006 and a model prediction of a warped disk due to an inclined binary companion .
The warped disk model , based on the hydrodynamic simulations combined with three-dimensional radiative transfer calculations , reproduces all major morphological features .
However , it does not account for the observed overbrightness at PA \sim 140 ^ { \circ } .

Conclusions : Shadows have been detected in several protoplanetary disks , suggesting that misalignment in disks is not uncommon .
However , the origin of the misalignment is not clear .
As-yet-undetected stellar or massive planetary companions could be responsible for them , and naturally account for the presence of depleted inner cavities .