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The chemical composition of planets is inherited from that of theprotoplanetary disk at the time of planet formation. Increasing observationalevidence suggests that planet formation occurs in less than 1 Myr. Thismotivates the need for spatially resolved spectral observations of Class Idisks, as carried out by the ALMA chemical survey of Disk-Outflow sources inTaurus (ALMA-DOT). In the context of ALMA-DOT, we observe the edge-on diskaround the Class I source IRAS 04302+2247 (the butterfly star) in the 1.3mmcontinuum and five molecular lines. We report the first tentative detection ofmethanol (CH$_3$OH) in a Class I disk and resolve, for the first time, thevertical structure of a disk with multiple molecular tracers. The bulk of theemission in the CO 2-1, CS 5-4, and o-H$_2$CO 3(1,2)-2(1,1) lines originatesfrom the warm molecular layer, with the line intensity peaking at increasingdisk heights, $z$, for increasing radial distances, $r$. Molecular emission isvertically stratified, with CO observed at larger disk heights (aperture$z/r\sim0.41-0.45$) compared to both CS and H$_2$CO, which are nearly cospatial($z/r\sim0.21-0.28$). In the outer midplane, the line emission decreases due tomolecular freeze-out onto dust grains (freeze-out layer) by a factor of >100(CO) and 15 (CS). The H$_2$CO emission decreases by a factor of only about 2,which is possibly due to H$_2$CO formation on icy grains, followed by anonthermal release into the gas phase. The inferred [CH$_3$OH]/[H$_2$CO]abundance ratio is 0.5-0.6, which is 1-2 orders of magnitude lower than forClass 0 hot corinos, and a factor ~2.5 lower than the only other value inferredfor a protoplanetary disk (in TW Hya, 1.3-1.7). Additionally, it is at thelower edge but still consistent with the values in comets. This may indicatethat some chemical reprocessing occurs in disks before the formation of planetsand comets.

ALMA chemical survey of disk-outflow sources in Taurus (ALMA-DOT) II: Vertical stratification of CO, CS, CN, H$_2$CO, and CH$_3$OH in a Class I disk