Same as Fig. 4, but for hot core models cr16-r3-l7 (upper panel) and cr16-r3.5-l4 (lower panel). Note the alternative labeling of the density and temperature axes on the right side of the respective plots.

Same as Fig. 4, but for hot core models cr16-r4-l2 (upper panel) and cr16-r4.5-l4 (lower panel). Note the alternative labeling of the density and temperature axes on the right side of the respective plots.

Same as Fig. 4, but for hot core models cr17-r3-l2 (upper panel) and cr17-r3.5-l4 (lower panel). Note the alternative labeling of the density and temperature axes on the right side of the respective plots.

Same as Fig. 4, but for hot core models cr17-r4-l7 (upper panel) and cr17-r4.5-l4 (lower panel). Note the alternative labeling of the density and temperature axes on the right side of the respective plots.

Temporal variation of the radii with temperature above 100 K, 150 K, and 200 K. Radii of the spatial distribution of various molecules as derived from the myXCLASS analysis (see Table 7) are overplotted with different colors. The arrow indicates that the radii of CH₃OH and C₂H₅OH at 1 × 10⁵ year are only lower limits.

Simulated spectra for the hot core model cr16-r3-l7 at 9 × 10⁴ year, overplotted on the spectra at 1 × 10⁵ year. The intensity of various spectral lines at two different epochs cannot be matched using a scaling factor. Spectral changes originate from the variation of temperature and abundances at different timescales.

Scaled-up version (multiplied by a factor of 2) of simulated spectra for the hot core model cr16-r3-l7 at 9 × 10⁴ year, overplotted on the Herschel-HIFI spectra of NGC 6334I.

Fitted spectra obtained from the myXCLASS analysis (solid black line), overplotted on the simulated spectra (colored dashed lines) of different COMs.