Gas excitation of post-SB galaxies at 0.6 < z < 1.3

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Table 3.

Physical properties of our sample galaxies.

ID	log(M_★/M_⊙)	SFR	log(M_H2/M_⊙)	sSFR	R_ij
		(M_⊙ yr⁻¹)		(Gyr⁻¹)
(1)	(2)	(3)	(4)	(5)	(6)
J1448^a	$11 . 6_{- 0.07}^{+ 0.04}$ $Mathematical equation: $ 11.6^{+0.04}_{-0.07} $$	$1 . 06_{- 0.94}^{+ 0.99}$ $Mathematical equation: $ 1.06^{+0.99}_{-0.94} $$	10.4 ± 0.06	0.003	0.76 ± 0.19
J2258^a	$11 . 8_{- 0.05}^{+ 0.03}$ $Mathematical equation: $ 11.8^{+0.03}_{-0.05} $$	$0 . 94_{- 1.71}^{+ 1.85}$ $Mathematical equation: $ 0.94^{+1.85}_{-1.71} $$	10.9 ± 0.05	0.001	0.27 ± 0.09
ID83492^b	$10 . 8_{- 0.20}^{+ 0.20}$ $Mathematical equation: $ 10.8^{+0.20}_{-0.20} $$	$0 . 52_{- 0.32}^{+ 0.79}$ $Mathematical equation: $ 0.52^{+0.79}_{-0.32} $$	10.4 ± 0.16	0.008	0.24 ± 0.12^c
J1109^a	$11 . 3_{- 0.03}^{+ 0.09}$ $Mathematical equation: $ 11.3^{+0.09}_{-0.03} $$	$2 . 33_{- 1.62}^{+ 1.12}$ $Mathematical equation: $ 2.33^{+1.12}_{-1.62} $$	10.4 ± 0.04	0.012	< 0.08
J1302^a	$11 . 6_{- 0.06}^{+ 0.04}$ $Mathematical equation: $ 11.6^{+0.04}_{-0.06} $$	$0 . 26_{- 0.26}^{+ 0.93}$ $Mathematical equation: $ 0.26^{+0.93}_{-0.26} $$	10.4 ± 0.06	0.001	< 0.16
J0912^a	$11 . 2_{- 0.02}^{+ 0.03}$ $Mathematical equation: $ 11.2^{+0.03}_{-0.02} $$	$0 . 81_{- 0.76}^{+ 1.33}$ $Mathematical equation: $ 0.81^{+1.33}_{-0.76} $$	10.8 ± 0.03	0.003	< 0.05
J2202^a	$11 . 2_{- 0.02}^{+ 0.03}$ $Mathematical equation: $ 11.2^{+0.03}_{-0.02} $$	$1 . 99_{- 1.70}^{+ 1.91}$ $Mathematical equation: $ 1.99^{+1.91}_{-1.70} $$	10.1 ± 0.14	0.004	< 1.50
ID97148^b	$10 . 7_{- 0.10}^{+ 0.10}$ $Mathematical equation: $ 10.7^{+0.10}_{-0.10} $$	< 0.72	10.1 ± 0.23	< 0.016	< 0.11^c

C1-83492^b	10.6 ± 0.1	$295 . 12_{- 225.94}^{+ 217.74}$ $Mathematical equation: $ 295.12^{+217.74}_{-225.94} $$	9.9 ± 0.06	7.9	0.19 ± 0.04^c
C2-83492^b	10.8 ± 0.20	$851 . 14_{- 651.61}^{+ 19.83}$ $Mathematical equation: $ 851.14^{+19.83}_{-651.61} $$	9.9 ± 0.06	13.5	0.12 ± 0.04^c

Notes. Columns: (1) ID; (2) Stellar mass from optical SED fit. We report the formal uncertainties from the SED modeling, although more realistic uncertainties accounting for systematics are ∼0.2 dex (Pacifici et al. 2023); (3) Star formation rate from optical SED; (4) Molecular gas mass. We used α_CO = 4.4 M_⊙ pc⁻² (K km s⁻¹)⁻¹ for the post-SBs and α_CO = 0.8 M_⊙ pc⁻² (K km s⁻¹)⁻¹ for the starbursting companions; (5) Specific star formation rate; (6) Ratio of the CO(5–4) and lower-J brightness temperature. In this table we report R₅₃ = L′_{CO(5 − 4)}/L′_{CO(3 − 2)} for ID83492 and ID97148, while we report R₅₂ = L′_{CO(5 − 4)}/L′_{CO(2 − 1)} for the rest of the sample. ^aStellar mass and SFR from Bezanson et al. (2022). ^bStellar mass and SFR from Zanella et al. (2023). ^cWe report the R₅₃ ratio, while in the plots we adopt a pseudo-R₅₂ ratio estimated adopting R₃₂ = 0.62 (average of local post-SBs value, French et al. 2023).

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