A3COSMOS: Measuring the cosmic dust-attenuated star formation rate density at 4 < z < 5

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Volume 688 (August 2024)

A&A, 688 (2024) A55

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Table 1.

Measured dust-attenuated luminosities and derived properties of our six uv-domain stacks.

Stellar mass	N	log₁₀⟨M_*⟩	⟨z⟩	log $_{10} ⟨ L_{150}^{rest} ⟩$ $_{10}\langle L_{\mathrm{150}}^{\mathrm{rest}} \rangle$	S/N	log $_{10} ⟨ {SFR}_{IR} ⟩$ $_{10}\langle \rm{SFR}_{\mathrm{IR}} \rangle$	log $_{10} ⟨ {SFR}_{UV} ⟩$ $_{10}\langle \rm{SFR}_{\mathrm{UV}} \rangle$	⟨β_UV⟩	log₁₀⟨IRX⟩
log₁₀(M_⊙)		log₁₀(M_⊙)		log₁₀(erg s⁻¹ Hz⁻¹)		log₁₀(M_⊙ yr⁻¹)	log₁₀(M_⊙ yr⁻¹)
Including all SFGs with a A³COSMOS coverage

9.5 − 10	302	$9 . 7_{- 0.1}^{+ 0.1}$ $9.7^{+0.1}_{-0.1}$	$4 . 4_{- 0.1}^{+ 0.1}$ $4.4^{+0.1}_{-0.1}$	$31 . 60_{- 0.16}^{+ 0.12}$ $31.60^{+0.12}_{-0.16}$	6	$1 . 19_{- 0.17}^{+ 0.14}$ $1.19^{+0.14}_{-0.17}$	$0 . 91_{- 0.05}^{+ 0.04}$ $0.91^{+0.04}_{-0.05}$	$- 1 . 53_{- 0.10}^{+ 0.10}$ $-1.53^{+0.10}_{-0.10}$	$0 . 45_{- 0.22}^{+ 0.14}$ $0.45^{+0.14}_{-0.22}$
10 − 10.5	96	$10 . 3_{- 0.1}^{+ 0.1}$ $10.3^{+0.1}_{-0.1}$	$4 . 5_{- 0.1}^{+ 0.1}$ $4.5^{+0.1}_{-0.1}$	$31 . 98_{- 0.09}^{+ 0.07}$ $31.98^{+0.07}_{-0.09}$	8	$1 . 56_{- 0.11}^{+ 0.09}$ $1.56^{+0.09}_{-0.11}$	$0 . 75_{- 0.20}^{+ 0.13}$ $0.75^{+0.13}_{-0.20}$	$- 1 . 03_{- 0.21}^{+ 0.21}$ $-1.03^{+0.21}_{-0.21}$	$1 . 00_{- 0.23}^{+ 0.15}$ $1.00^{+0.15}_{-0.23}$
10.5 − 11.5	42	$10 . 8_{- 0.1}^{+ 0.1}$ $10.8^{+0.1}_{-0.1}$	$4 . 5_{- 0.1}^{+ 0.1}$ $4.5^{+0.1}_{-0.1}$	$33 . 16_{- 0.68}^{+ 0.25}$ $33.16^{+0.25}_{-0.68}$	37	$2 . 74_{- 0.68}^{+ 0.26}$ $2.74^{+0.26}_{-0.68}$	$0 . 91_{- 0.17}^{+ 0.12}$ $0.91^{+0.12}_{-0.17}$	$- 0 . 31_{- 0.62}^{+ 0.62}$ $-0.31^{+0.62}_{-0.62}$	$2 . 01_{- 0.85}^{+ 0.27}$ $2.01^{+0.27}_{-0.85}$

Excluding the ALMA primary targets

9.5 − 10	271	$9 . 7_{- 0.1}^{+ 0.1}$ $9.7^{+0.1}_{-0.1}$	$4 . 4_{- 0.1}^{+ 0.1}$ $4.4^{+0.1}_{-0.1}$	$31 . 28_{- \infty}^{+ 0.33}$ $31.28^{+0.33}_{-\infty}$	3	$0 . 87_{- \infty}^{+ 0.34}$ $0.87^{+0.34}_{-\infty}$	$0 . 70_{- 0.07}^{+ 0.06}$ $0.70^{+0.06}_{-0.07}$	$- 1 . 43_{- 0.15}^{+ 0.15}$ $-1.43^{+0.15}_{-0.15}$	$0 . 34_{- \infty}^{+ 0.35}$ $0.34^{+0.35}_{-\infty}$
10 − 10.5	79	$10 . 3_{- 0.1}^{+ 0.1}$ $10.3^{+0.1}_{-0.1}$	$4 . 5_{- 0.1}^{+ 0.1}$ $4.5^{+0.1}_{-0.1}$	$31 . 86_{- 0.16}^{+ 0.12}$ $31.86^{+0.12}_{-0.16}$	5	$1 . 44_{- 0.17}^{+ 0.14}$ $1.44^{+0.14}_{-0.17}$	$0 . 44_{- 0.19}^{+ 0.13}$ $0.44^{+0.13}_{-0.19}$	$- 0 . 79_{- 0.23}^{+ 0.23}$ $-0.79^{+0.23}_{-0.23}$	$1 . 17_{- 0.28}^{+ 0.17}$ $1.17^{+0.17}_{-0.28}$
10.5 − 11.5	26	$10 . 8_{- 0.1}^{+ 0.1}$ $10.8^{+0.1}_{-0.1}$	$4 . 7_{- 0.1}^{+ 0.1}$ $4.7^{+0.1}_{-0.1}$	$32 . 66_{- 0.41}^{+ 0.21}$ $32.66^{+0.21}_{-0.41}$	15	$2 . 25_{- 0.41}^{+ 0.22}$ $2.25^{+0.22}_{-0.41}$	$0 . 50_{- 0.58}^{+ 0.24}$ $0.50^{+0.24}_{-0.58}$	$0 . 51_{- 0.50}^{+ 0.50}$ $0.51^{+0.50}_{-0.50}$	$1 . 92_{- 1.43}^{+ 0.29}$ $1.92^{+0.29}_{-1.43}$

Notes. Errors on each quantity were obtained from a bootstrap analysis. We used the 50th percentile as the best estimate and the 16th and 84th percentiles of this bootstrap analysis as errors. For $⟨ L_{150}^{rest} ⟩$ $\langle L_{\mathrm{150}}^{\mathrm{rest}} \rangle$ , we also provide the signal-to-noise ratio (S/N) in the stacks. Errors on $⟨ L_{150}^{rest} ⟩$ $\langle L_{\mathrm{150}}^{\mathrm{rest}} \rangle$ from the bootstrap analysis are much larger than these, as they take into account not only the photometric noise in the stacks but also the intrinsic dispersion in the luminosities of the stacked population.

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