Unveiling dust, molecular gas, and high star-formation efficiency in extremely UV bright star-forming galaxies at z ∼ 2.1–3.6

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Volume 693 (January 2025)

A&A, 693 (2025) A17

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Table 4.

Dust and molecular gas properties of the galaxy sample.

Target	z_nebular^(a)	SFR_IR^(b)	M_molgas^(c)	M_dust^(d)	t_depl^(e,^f)	f_molgas^(f)	ϵ_SF^(f)
		(M_⊙ yr⁻¹)	(10¹⁰ M_⊙)	(10⁷ M_⊙)	(Myr)		(%)
J1322+0423	2.0800	< 26	< 0.76	< 1.09	< 42	< 0.69	> 31
J0146–0220	2.1595	81 ± 29	1.28 ± 0.09	3.32 ± 1.78	61 ± 23	0.79 ± 0.11	21 ± 3
J1415+2036	2.2435	< 34	< 1.11 ± 0.23	< 1.38	< 50 ± 11	< 0.86 ± 0.20	> 14 ± 3
J1249+1550	2.2928	85 ± 30.	0.73 ± 0.05	3.42 ± 1.79	36 ± 13	0.63 ± 0.09	37 ± 5
J0006+2452	2.3796	283 ± 98	3.67 ± 0.21	11.1 ± 5.7	71 ± 25	0.92 ± 0.11	8 ± 0.9
J0850+1549	2.4235	59 ± 20	< 0.75	2.30 ± 1.18	< 30	< 0.80	> 20
J1220–0051	2.4269	96 ± 33	1.01 ± 0.10	3.73 ± 1.90	42 ± 15	0.87 ± 0.13	13 ± 2
J0950+0523	2.4548	185 ± 63	2.01 ± 0.12	7.15 ± 3.63	55 ± 19	0.91 ± 0.15	9 ± 1
J1220+0842	2.4698	< 57	< 1.12	< 2.20	< 31	< 0.76	> 24
J1157+0113	2.5450	141 ± 48	1.08 ± 0.10	8.97 ± 2.68	44 ± 16	0.85 ± 0.31	15 ± 6
J0121+0025	3.2445	71 ± 22	< 1.11 ± 0.32	3.75 ± 1.08	< 32 ± 14	< 0.71 ± 0.25	> 29 ± 10
J1316+2614	3.6122	74 ± 21	< 0.63	3.53 ± 1.01	< 13	< 0.60	> 40

Notes.

^(a)

Redshifts derived from optical nebular emission lines.

^(b)

Obscured SFRs derived from the IR luminosities (Table 3) following the calibration of Kennicutt (1998) for the Chabrier (2003) IMF, SFR_IR = L_IR/10¹⁰. For SFR_IR non-detections, we considered the L_IR 4σ upper limits.

^(c)

Molecular gas masses computed from the CO(3–2) or CO(4–3) luminosities (Table 2) following Eq. (1) and assuming here the CO-to-H₂ conversion factor derived for nearby starbursts, $α_{CO}^{SB} = 1 M_{⊙} {(K km s^{- 1} {pc}^{2})}^{- 1}$ $\alpha_{\mathrm{CO}}^{\mathrm{SB}} = 1\,M_{\odot}\,\rm (K\,km\,s^{-1}\,pc^2)^{-1}$ (Sect. 3.2).

^(d)

Dust masses derived from the FIR fluxes (Table 3) following Eq. (2) (Sect. 3.3).

^(e)

Molecular gas depletion timescales derived using the total SFR_UV+IR.

^(f)

Molecular gas depletion timescales, molecular gas mass fractions, and star-formation efficiencies defined in Sects. 4.2 and 4.3, and all computed here with $α_{CO}^{SB}$ $\alpha_{\mathrm{CO}}^{\mathrm{SB}}$ .

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