Notes. All the observed line fluxes are disk-integrated, with the exception for those taken from the following references: Ruíz-Rodríguez et al. (2022); van't Hoff et al. (2018); Zagaria et al. (2025). ^(a)The observed CH₃OH and SO line fluxes have been rescaled to a common distance of 140 pc and to the same transition (the 6_(1,5)−6_(0,6) A one for CH₃OH and the J_N = 6₅ − 5₄ transition for SO). ^(b)In the column, the first entry points to the reference where the CH₃OH line flux values are presented, while the second entry does the same for SO. ^(c)The high rescaled CH₃OH and SO fluxes inside the V883 Ori disk suggest that the emission could be optically thick. To be consistent with the other sources, we still rescale the fluxes using Eq. E.1 under the assumption of optically thin emission.

References. (1) Evans et al. (2025); (2) Booth et al. (2024a); (3) Booth et al. (2023); (4) Law et al. (2023); (5) Booth et al. (2025); (6) Booth et al. (2026); (7) Temmink et al. (2025); (8) Booth et al. (2024b); (9) Booth et al. (2026); (10) Zagaria et al. (2025); (11) van't Hoff et al. (2018): (12) Ruíz-Rodríguez et al. (2022); (13) This work; (14) Garufi et al. (2022);