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[abridged] We present new scattered light and millimeter observations of theprotoplanetary disk around LkH$\alpha\,330$, using SPHERE/VLT and ALMA,respectively. The scattered-light SPHERE observations reveal an asymmetric ringat around 45au from the star in addition to two spiral arms with similar radiallaunching points at around 90au. The millimeter observations from ALMA(resolution of 0.06''$\times$0.04'') mainly show an asymmetric ring located at110au from the star. In addition to this asymmetry, there are two faintsymmetric rings at 60au and 200au. The $^{12}$CO, $^{13}$CO, and C$^{18}$Olines seem to be less abundant in the inner disk (these observations have aresolution of 0.16''$\times$0.11''). The $^{13}$CO peaks at a location similarto the inner ring observed with SPHERE, suggesting that this line is opticallythick and traces variations of disk temperature instead of gas surface-densityvariations, while the C$^{18}$O peaks slightly further away at around 60au. Wecompare our observations with hydrodynamical simulations that include gas anddust evolution, and conclude that a 10$M_{\rm{Jup}}$ mass planet at 60au and inan eccentric orbit ($e=0.1$) can qualitatively explain most of the observedstructures. A planet in a circular orbit leads to a much narrower concentrationin the millimeter emission, while a planet in a more eccentric orbit leads to avery eccentric cavity as well. In addition, the outer spiral arm launched bythe planet changes its pitch angle along the spiral due to the eccentricity andwhen it interacts with the vortex, potentially appearing in observations as twodistinct spirals. Our observations and models show that LkH$\alpha\,330$ is aninteresting target to search for (eccentric-) planets while they are stillembedded in their parental disk, making it an excellent candidate for studieson planet-disk interaction.

Distributions of gas and small and large grains in the LkH$\alpha\,330$ disk trace a young planetary system