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The chemical composition of planets is inherited by the distribution of thevarious molecular species in the protoplanetary disk at thetime of theirformation. As of today, only a handful of disks has been imaged in multiplespectral lines with high spatial resolution. As part of a small campaigndevoted to the chemical characterization of disk-outflow sources in Taurus, wereport on new ALMA Band 6 observations with 20 au resolution toward theembedded young star DG Tau B. Images of the continuum emission reveals a dustdisk with rings and, putatively, a leading spiral arm. The disk, as well as theprominent outflow cavities, are detected in CO, H2CO, CS, and CN while theyremain undetected in SO2, HDO, and CH3OH. From the absorption of the back-sideoutflow, we inferred that the disk emission is optically thick in the inner 50au. This morphology explains why no line emission is detected from this innerregion and poses some limitations toward the calculation of the dust mass andthe characterization of the inner gaseous disk. The H2CO and CS emission fromthe inner 200 au is mostly from the disk and their morphology is very similar.The CN emission significantly differs from the other two molecules as it isobserved only beyond 150 au. This ring-like morphology is consistent withprevious observations and the predictions of thermochemical disk models.Finally, we constrained the disk-integrated column density of all molecules. Inparticular, we found that the CH3OH/H2CO ratio must be smaller than 2, makingthe methanol non-detection still consistent with the only such a ratioavailable from the literature (1.27 in TW Hya).

ALMA chemical survey of disk-outflow sources in Taurus (ALMA-DOT): I. CO, CS, CN, and H2CO around DG Tau B