The cold interstellar medium of a normal sub-L⋆ galaxy at the end of reionization

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Volume 685 (May 2024)

A&A, 685 (2024) A138

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Table 3.

Physical properties.

	z6.3	arc
RA [h:m:s]	06:00:09.55	06:00:09.13
Dec [d:m:s]	−20:08:11.26	−20:08:26.49
z_spec	6.0719	6.0736
μ	$21_{- 7}^{+ 14}$ $21^{+14}_{-7}$	$163_{- 13}^{+ 27}$ $163^{+27}_{-13}$ ^(†)
log(μM_⋆) [M_⊙]	10.2 ± 0.2	10.6 ± 0.2
μL_{FIR, 42.5 − 122.5 μm} [L_⊙]	$7 . 1_{- 3.5}^{+ 6.1} \times 10^{11}$ $7.1^{+6.1}_{-3.5} \times 10^{11}$	$5 . 7_{- 2.1}^{+ 4.1} \times 10^{11}$ $5.7^{+4.1}_{-2.1} \times 10^{11}$
μL_{IR, 8 − 1000 μm} [μL_⊙]	$1 . 1_{- 0.6}^{+ 2.2} \times 10^{12}$ $1.1^{+2.2}_{-0.6} \times 10^{12}$	$0 . 7_{- 0.2}^{+ 0.6} \times 10^{12}$ $0.7^{+0.6}_{-0.2} \times 10^{12}$
μL_{IR, CO(7 − 6)} [L_⊙]	< 0.4 × 10¹²	< 1.3 × 10¹²
μM_dust [M_⊙]	$0 . 4_{- 0.2}^{+ 0.4} \times 10^{8}$ $0.4^{+0.4}_{-0.2} \times 10^{8}$	$1 . 6_{- 0.8}^{+ 1.7} \times 10^{8}$ $1.6^{+1.7}_{-0.8} \times 10^{8}$
T_dust [K]	$50_{- 13}^{+ 20}$ $50^{+20}_{-13}$	$37_{- 7}^{+ 11}$ $37^{+11}_{-7}$
β_IR	$1 . 8_{- 0.2}^{+ 0.2}$ $1.8^{+0.2}_{-0.2}$	$1 . 6_{- 0.2}^{+ 0.2}$ $1.6^{+0.2}_{-0.2}$
μSFR(IR) [M_⊙ yr⁻¹]	$164_{- 95}^{+ 334}$ $164^{+334}_{-95}$	$111_{- 37}^{+ 96}$ $111^{+96}_{-37}$
μSFR(IR, CO (7 − 6)) [M_⊙ yr⁻¹]	< 53	< 193
μSFR(FUV) [M_⊙ yr⁻¹]	$49_{- 6}^{+ 7}$ $49^{+7}_{-6}$	–
Total μSFR(FUV_corr) [M_⊙ yr⁻¹]	$135_{- 48}^{+ 171}$ $135^{+171}_{-48}$	–
Total μSFR(Hα_corr)/k_Z [M_⊙ yr⁻¹]	$141_{- 14}^{+ 42}$ $141^{+42}_{-14}$	–
μM_gas([C I]) [M_⊙]	< 0.1 − 1 × 10¹⁰	–
μM_gas([C II])_Z18 [M_⊙]	(6.9 ± 0.6)×10¹⁰	–
μM_gas([C II])_H21 [M_⊙]^(§)	$2 . 2_{- 0.9}^{+ 1.5} \times 10^{11}$ $2.2^{+1.5}_{-0.9}\times10^{11}$	–
M_dyn [M_⊙]^(‡)	$3_{- 1}^{+ 1} \times 10^{9}$ $3^{+1}_{-1} \times10^{9}$	–

Notes. All estimates are not corrected for lensing (excluding the dynamical mass). The estimates of physical properties from optical and FIR/submillimeter SED modeling are expressed as the median value and the 16–84% of their posterior distributions. Upper limits at 3σ. Total μSFR(FUV_corr), μSFR(Hα_corr) are derived from the luminosities at 1500 Å and of the Hα line corrected for the dust attenuation as in Hao et al. (2011) and Murphy et al. (2011) (Sect. 4.4). μSFR(Hα_corr) is decreased by a factor of k_Z = 2.5 with respect to the calibration in Murphy et al. (2011) to account for the low metallicity (12 + log(O/H) = (8.11 ± 0.20) or Z ∼ 0.25 Z_⊙, Kennicutt & Evans 2012; Theios et al. 2019; Shapley et al. 2023). ^(†) For the arc, this factor is defined as the observed luminosity of the image divided by the local luminosity of the strongly lensed sub region near the caustic line shown in Fig. 4 of F21. The global μ factor for the whole galaxy (i.e., the observed luminosity of the multiple image divided by the overall intrinsic luminosity of the galaxy) is $μ_{whole} = 29_{- 7}^{+ 4}$ $\mu_{\mathrm{whole}}=29^{+4}_{-7}$ (F21).

^(§) The calibration in Heintz et al. (2021) returns the H I gas mass. ^(‡) From [C II] observations in F21.

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