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tokens: identified toward these positions. Column densities of this species are presented in Table 3 . Figure 5. Detected transitions of CH 3 NHCHO in the spectrum toward position MM1-nmf. The observed spectrum is plotted in black, with the synthetic spectrum overplotted in blue and the rest-frequency center of the transition is indicated by the red dotted line. The upper state energy of each transition is given in the top-left corner. At a number of positions a handful of spectral features are identified that can be assigned to NH 2 C(O)NH 2 . The most and clearest lines are identified toward position MM1-v, see Figure 6 , with at least three unblended lines. While these lines are not enough for a secure detection, a tentative identification can be claimed. The tentative and upper-limit column densities of NH 2 C(O)NH 2 are presented in Table 3 . Figure 6. Overview of NH 2 C(O)NH 2 spectral features toward position MM1-v. The observed spectrum is plotted in black, with the synthetic spectrum overplotted in blue and the rest-frequency center of the transition is indicated by the red dotted line. The upper state energy of each transition is given in the top-left corner. 4. Discussion 4.1. Chemical Comparisons To get a better understanding of the chemical processes leading to amides, it is useful to compare molecular ratios of the positions within NGC 6334I, but also with other inter- and circumstellar sources. In the following subsections molecular ratios with respect to NH 2 CHO are discussed. Comparisons are made with the following works: IRAM 30 m and Green Bank Telescope (GBT) single-dish observations of G + 0.693-0.027 (hereafter G + 0.693), a quiescent giant molecular cloud (Zeng et al. 2018 ; Jiménez-Serra et al. 2020 ); ALMA observations of the incipient hot corino Barnard B1b-S (Marcelino et al. 2018 ); Northern Extended Millimeter Array observations of the low-mass protostars SVS13A, NGC 1333-IRAS4A2, NGC 1333-IRAS2A(1) (Coutens et al. 2018 ; Belloche et al. 2020 ); ALMA Protostellar Interferometric Line Survey (Jørgensen et al. 2016 ) observations of the low-mass protostar IRAS 16293B (Coutens et al. 2016 , 2018 ; Ligterink et al. 2018a ); GBT and IRAM 30 m single-dish observations of the Galactic center source Sgr B2 (Hollis et al. 2006 ; Belloche et al. 2013 ); ALMA observations of the HMSFR Orion KL (Cernicharo et al. 2016 ); the high-mass star AFGL 4176 (Bøgelund et al. 2019a ); and of Sgr B2 (Belloche et al. 2017 , 2019 ). One has to be aware that precise knowledge of the source size or emitting area of a certain molecule is essential for ratio comparisons. In particular, single-dish telescopes do not have the spatial resolution to determine the source size and these are often assumed or estimated, potentially resulting in large column density errors. Finally, mass spectrometric measurements of the Rosetta mission to comet 67P/C-G are used to compare with a solar system object (Goesmann et al. 2015 ; Altwegg et al. 2017 ). The