The planet formation seen through high-resolution images of protoplanetary disks

The high occurrence of exoplanets around solar-type stars suggests that planets form very efficiently in protoplanetary disks. Yet, numerical simulations and laboratory experiments show that the planet formation is a complicated process. The onset of optical/NIR and (sub-)mm surveys of young stars has been a game changer for our understanding of protoplanetary disks and planet formation. Thanks to the contributed effort of VLT/SPHERE, GPI, and ALMA we could resolve with unprecedented resolution several sub-structures at the disk surface and midplane from few to hundreds of au from the star. I show the method and the recent improvement of this type of observations and discuss the implications to the recurrent existence of these disk features.