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Planets form in dusty, gas-rich disks around young stars, while at the sametime, the planet formation process alters the physical and chemical structureof the disk itself. Embedded planets will locally heat the disk and sublimatevolatile-rich ices, or in extreme cases, result in shocks that sputter heavyatoms such as Si from dust grains. This should cause chemical asymmetriesdetectable in molecular gas observations. Using high-angular-resolution ALMAarchival data of the HD 169142 disk, we identify compact SO J=8$_8$-7$_7$ andSiS J=19-18 emission coincident with the position of a ${\sim}$2 M$_{\rm{Jup}}$planet seen as a localized, Keplerian NIR feature within a gas-depleted,annular dust gap at ${\approx}$38 au. The SiS emission is located along anazimuthal arc and has a similar morphology as a known $^{12}$CO kinematicexcess. This is the first tentative detection of SiS emission in aprotoplanetary disk and suggests that the planet is driving sufficiently strongshocks to produce gas-phase SiS. We also report the discovery of compact$^{12}$CO and $^{13}$CO J=3-2 emission coincident with the planet location.Taken together, a planet-driven outflow provides the best explanation for theproperties of the observed chemical asymmetries. We also resolve a bright,azimuthally-asymmetric SO ring at ${\approx}$24 au. While most of this SOemission originates from ice sublimation, its asymmetric distribution impliesazimuthal temperature variations driven by a misaligned inner disk orplanet-disk interactions. Overall, the HD 169142 disk shows several distinctchemical signatures related to giant planet formation and presents a powerfultemplate for future searches of planet-related chemical asymmetries inprotoplanetary disks.

SO and SiS Emission Tracing an Embedded Planet and Compact $^{12}$CO and $^{13}$CO Counterparts in the HD 169142 Disk