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Planet-forming disks are not isolated systems. Their interaction with thesurrounding medium affects their mass budget and chemical content. In thecontext of the ALMA-DOT program, we obtained high-resolution maps of assortedlines from six disks that are still partly embedded in their natal envelope. Inthis work, we examine the SO and SO$_2$ emission that is detected from foursources: DG Tau, HL Tau, IRAS 04302+2247, and T Tau. The comparison with CO,HCO$^+$, and CS maps reveals that the SO and SO$_2$ emission originates at theintersection between extended streamers and the planet-forming disk. Twotargets, DG Tau and HL Tau, offers clear cases of inflowing material inducingan accretion shock on the disk material. The measured rotational temperaturesand radial velocities are consistent with this view. In contrast to youngerClass 0 sources, these shocks are confined to the specific disk region impactedby the streamer. In HL Tau, the known accreting streamer induces a shock in thedisk outskirt, and the released SO and SO$_2$ molecules spiral toward the starin a few hundreds years. These results suggest that shocks induced by lateaccreting material may be common in the disks of young star-forming regionswith possible consequences on the chemical composition and mass content of thedisk. They also highlight the importance of SO and SO$_2$ line observations toprobe accretion shocks from a larger sample.

ALMA chemical survey of disk-outflow sources in Taurus (ALMA-DOT) VI: Accretion shocks in the disk of DG Tau and HL Tau