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We performed observations of the Sco-Cen F star HD 117214 aiming at a searchfor planetary companions and the characterization of the debris disk structure.HD 117214 was observed with the SPHERE subsystems IRDIS, IFS and ZIMPOL atoptical and near-IR wavelengths using angular and polarimetric differentialimaging techniques. This provided the first images of scattered light from thedebris disk with a spatial resolution reaching 25 mas and an inner workingangle $< 0.1''$. With the observations with IRDIS and IFS we derive detectionlimits for substellar companions. The geometrical parameters of the detecteddisk are constrained by fitting 3D models for the scattering of an opticallythin dust disk. Investigating the possible origin of the disk gap, weintroduced putative planets therein and modeled the planet-disk andplanet-planet dynamical interactions. The obtained planetary architectures arecompared with the detection limit curves. The debris disk has an axisymmetricring structure with a radius of $0.42(\pm 0.01)''$ or $\sim45$ au and aninclination of $71(\pm 2.5)^\circ$ and exhibits a $0.4''$ ($\sim40$ au) wideinner cavity. From the polarimetric data, we derive a polarized flux contrastfor the disk of $(F_{\rm pol})_{\rm disk}/F_{\rm \ast}> (3.1 \pm 1.2)\cdot10^{-4}$ in the RI band. The fractional scattered polarized flux of the disk iseight times smaller than the fractional infrared flux excess. This ratio issimilar to the one obtained for the debris disk HIP 79977 indicating that dustradiation properties are not very different between these two disks. Inside thedisk cavity we achieve the high sensitivity limits on planetary companions witha mass down to $\sim 4 M_{\rm J}$ at projected radial separations between$0.2''$ and $0.4''$. We can exclude the stellar companions at a radialseparation larger than 75 mas from the star.

HD 117214 debris disk: scattered-light images and constraints on the presence of planets