Notes. Column (1): target name; Column (2): coordinates; Column (3): redshift; Column (4): J_up refers to the upper level of the (J_up → J_up − 1) CO transition; Column (5): the excitation correction defined as r_{Jup, 1} = CO(J_up → J_up − 1)/CO(1 → 0); Column (6): CO(1-0) luminosity; Column (7): gas mass; Column (8): stellar mass; Column (9): 8–1000 μm IR luminosity; Column (10): reference for the paper from which we derived CO and far-IR measurements, as well as assumed excitation correction and α_CO conversion factors. All lensed galaxy properties are corrected for magnification. The three lensed galaxies from Fudamoto et al. (2017), SGP-261206, NGP- 190387, and G09-83808, are not included in our sample as their magnification factors are unknown. The S15 and Y17 infrared luminosities are derived from SFR, using the following prescription: L_IR= SFR ×10¹⁰L_⊙ (Kennicutt 1998, correcting for a Chabrier IMF). The luminosity-to-gas-mass conversion factors used to derive the gas mass in the different papers are indicated in the table as follows: ^□: α_CO = 1.0; ∘: α_CO = 0.8; ^•: α_CO = 1.1; ^†: the gas masses are derived from a CO-based dynamical mass estimate by subtracting stellar and dark matter components (Silverman et al. 2015). The inferred M_gas yielded the estimate of α_CO = 0.6 ± 0.3 (PACS819) and α_CO = 1.6 ± 0.6 (PACS830).

References. Bothwell et al. (2013, Bo13); Fudamoto et al. (2017, F17); Sharon et al. (2016, S16); Silverman et al. (2015, S15); Yan et al. (2010, Y10); Yang et al. (2017, Y17).