Abstract Despite observational progress in planet formation, the stage in which planetesimals grow into planets remains poorly understood. During this phase, protoplanets may develop gaseous envelopes that are warmer than the surrounding disk gas, potentially providing observable signatures through molecules otherwise depleted in cold regions. In this Letter, we report the detection of the silicon sulfide isotopologues 28 SiS J = 16−15 and 30 SiS J = 18−17 in the protoplanetary disk around PDS 66 (MP Mus) at a significance of ∼5 σ −6 σ , using the Atacama Large Millimeter/submillimeter Array. These constitute the second and first detections of 28 SiS and 30 SiS in a protoplanetary disk, respectively. The emission appears as a compact source at r = 60 au in the southwestern region of the disk, unresolved with a ∼ 0 . ″ 5 beam, and shows a velocity consistent with Keplerian rotation, suggesting a protoplanetary origin. By modeling the line fluxes, we constrain the emitting radius to ∼0.5−4 au and estimate a SiS mass of 10 22 –10 23 g, corresponding to at least ∼10% of the silicon contained in local dust grains. Because complete sublimation of a substantial fraction of dust grains by local processes is difficult to achieve, this result instead implies an accumulation of silicon from a larger region. We propose that a circumplanetary envelope surrounding a low-mass protoplanet, where pebble accretion and subsequent sublimation of grains may enhance gaseous silicon abundance with respect to observable dust grains around it, can account for the observed characteristics.
Yoshida et al. (2026) studied this question.