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Table 2.

Gas properties of the two SBs and two MSs.

SB1 SB2 MS1 MS2
(a)αCO(Z) (M/(K km s−1 pc2)) 4.09 4.10 4.06 4.06
(b)Mgas, CO (1010M) 20.2 ± 1.7 13.3 ± 1.4 9.2 ± 0.9 7.4 ± 1.1
(c)fgas, CO 0.70 0.66 0.29 0.25
(d)tdep, CO (Gyr) 0.15 ± 0.02 0.18 ± 0.08 0.32 ± 0.14 0.25 ± 0.15
(e)δGDR 126 ± 16 123 ± 28 110 ± 65 171 ± 47
(f)Mgas, GDR (1010M) 17.9 ± 6.4 12.8 ± 5.1 7.6 ± 5.1 4.0 ± 1.7
fgas, GDR 0.68 0.65 0.25 0.15
tdep, GDR (Gyr) 0.14 ± 0.05 0.17 ± 0.10 0.26 ± 0.21 0.13 ± 0.10
(g)Mgas, 3.2mm (1010M) 22.7 ± 6.4 10.4 ± 3.9 17.1 ± 5.5 5.1 ± 1.6
fgas, 3.2mm 0.73 0.61 0.43 0.18
tdep, 3.2mm (Gyr) 0.17 ± 0.05 0.14 ± 0.08 0.59 ± 0.32 0.17 ± 0.11

Notes. The molecular gas masses are estimated based on the CO(1−0) emission line using metallicity-dependent conversion factors, gas-to-dust ratio, and 3.2mm dust continuum emission.

(a)

CO-to-H2 conversion factor (αCO(Z)) from W18, calculated based on the mass-metallicity relation.

(b)

Total molecular gas mass, computed as .

(c)

Gas fraction: fgas = Mgas/(Mstar + Mgas).

(d)

Gas depletion time: tdep = Mgas/SFR, which is the inverse of the star formation efficiency (SFE =1/tdep).

(e)

Gas-to-dust mass ratio, computed based on the δGDR − Z relation (Eq. (2)).

(f)

Mgas, GDR, computed based on the gas-to-dust ratio (Eq. (1)).

(g)

Mgas, 3.2mm, computed based on the Rayleigh-Jeans tail dust continuum (Eq. (4)).

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