Notes. Source IDs in boldface are classified as starbursts based on the main-sequence offset. The stellar mass (M_star), the instantaneous star-formation rate (SFR_inst) and the SFR averaged over the past 100 Myr (SFR₁₀₀) were obtained from the CIGALE SED best-fit model (see Sect. 4). The CIGALE parameters are not available for IDs 4, 4b, and 24b because they are not detected in the NIR and MIR images. SFR_IR was derived from the total IR luminosity (L_IR) assuming the relation in Kennicutt & Evans (2012) corrected for a Chabrier IMF (i.e., SFR  =  1.40 × 10⁻¹⁰ × L_IR) and L_IR was obtained from fitting the sub-mm/mm data with a modified blackbody using the cmcirsed package (Casey 2012). SFR_IR was not derived for IDs 4b, 18, 19, and 24b because of lack of submm/mm detections. The molecular gas mass, $M_{\mathrm{gas}}^{\mathrm{CO}}$, was derived from L′_{CO(1 − 0)} assuming α_CO = 4.36 M_⊙ pc⁻² (K km s⁻¹)⁻¹ (Bolatto et al. 2013; Genzel et al. 2015), and $M_{\mathrm{gas}}^{\mathrm{CI}}$ as 5.2${\alpha }_{\mathrm{CO}}L{\prime }_{\mathrm{C}\mathrm{I}(1-0)}$ (Birkin et al. 2021). The gas-to-stellar mass ratio is given by μ_gas = M_gas/M_star, and the gas depletion time by τ_depl = M_gas/SFR_IR (here we use CO-derived gas masses when both CO and CI are available). The main sequence offset (SFR/SFR^MS) is derived using SFR_IR, or SFR_inst when the former is not available (i.e., for IDs 18 and 19), and the SFR predicted by the relation in Popesso et al. (2023) assuming the redshift and the stellar mass of each source. The relative quantities ${\tau }_{\mathrm{depl}}/{\tau }_{\mathrm{depl}}^{\mathrm{MS}}$ and ${\mu }_{\mathrm{gas}}/{\mu }_{\mathrm{gas}}^{\mathrm{MS}}$ are derived by assuming the scaling relations for ${\mu }_{\mathrm{gas}}^{\mathrm{MS}}$ and ${\tau }_{\mathrm{depl}}^{\mathrm{MS}}$ as a function of stellar mass and redshift from Liu et al. (2019).