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Young planets are expected to cause perturbations in protostellar disks thatmay be used to infer their presence. Clear detection of still-forming planetsembedded within gas-rich disks is rare. HD 169142 is a very young Herbig Ae-Bestar surrounded by a pre-transitional disk, composed of at least three rings.While claims of sub-stellar objects around this star have been made previously,follow-up studies remain inconclusive. We used SPHERE at ESO VLT to obtain asequence of high-contrast images of the immediate surroundings of this starover about three years. This enables a photometric and astrometric analysis ofthe structures in the disk. While we were unable to definitively confirm theprevious claims of a massive sub-stellar object at 0.1-0.15 arcsec from thestar, we found both spirals and blobs within the disk. The spiral pattern maybe explained as due to the presence of a primary, a secondary, and a tertiaryarm excited by a planet of a few Jupiter masses lying along the primary arm,likely in the cavities between the rings. The blobs orbit the star consistentlywith Keplerian motion, allowing a dynamical determination of the mass of thestar. While most of these blobs are located within the rings, we found that oneof them lies in the cavity between the rings, along the primary arm of thespiral design. This blob might be due to a planet that might also beresponsible for the spiral pattern observed within the rings and for the cavitybetween the two rings. The planet itself is not detected at short wavelengths,where we only see a dust cloud illuminated by stellar light, but the planetaryphotosphere might be responsible for the emission observed in the K band. Themass of this putative planet may be constrained using photometric and dynamicalarguments; it should be between 1 and 4 Jupiter masses. The brightest blobs arefound at the 1:2 resonance with this putative planet

Blobs, spiral arms, and a possible planet around HD 169142