ALMA 360 parsec, high-frequency observations reveal warm dust in the center of a z = 6.9 quasar

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Volume 695 (March 2025)

A&A, 695 (2025) L18

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Table D.1.

Inferred average dust properties as a function of galactocentric radius in J2348–3054.

				Independent annuli fits^a			Joint resolved+unresolved SED fit ^b
r_min	r_max	S_ν(250 GHz)	S_ν(670 GHz)	M_d	T_d	L_TIR	M_d	T_d	L_TIR
[pc]	[pc]	[mJy]	[mJy]	[10⁸M_⊙]	[K]	[10¹² L_⊙]	[10⁸M_⊙]	[K]	[10¹² L_⊙]
0	216	1.086 ± 0.006	3.24 ± 0.25	1.17 ± 0.11	88.2 ± 2.3	$4 . 81_{+ 0.47}^{- 0.48}$ $4.81^{-0.48}_{+0.47}$	$5 . 9_{- 3.2}^{+ 1.4}$ $5.9^{+1.4}_{-3.2}$	$72 . 5_{- 0.4}^{+ 2.6}$ $72.5^{+2.6}_{-0.4}$	$2 . 23_{- 0.02}^{+ 0.34}$ $2.23_{-0.02}^{+0.34}$
216	253	0.596 ± 0.010	2.41 ± 0.42	0.48 ± 0.10	63.3 ± 5.7	$1 . 69_{+ 0.67}^{- 0.51}$ $1.69^{-0.51}_{+0.67}$	$0 . 72_{- 0.10}^{+ 0.10}$ $0.72_{-0.10}^{+0.10}$	$64 . 3_{- 4.4}^{+ 3.3}$ $64.3^{+3.3}_{-4.4}$	$2 . 73_{- 0.61}^{+ 0.60}$ $2.73_{-0.61}^{+0.60}$
253	380	0.504 ± 0.014	1.80 ± 0.58	0.17 ± 0.11	61.0 ± 17.9	$0 . 98_{+ 0.52}^{- 0.87}$ $0.98^{-0.87}_{+0.52}$	$0 . 34_{- 0.11}^{+ 0.11}$ $0.34_{-0.11}^{+0.11}$	$60 . 7_{- 7.2}^{+ 13.5}$ $60.7^{+13.5}_{-7.2}$	$1 . 94_{- 0.64}^{+ 2.23}$ $1.94_{-0.64}^{+2.23}$
380	506	0.147 ± 0.018	1.03 ± 0.74	0.06 ± 0.13	62.6 ± 60.2	0.52 ± 0.52	$0 . 09_{- 0.08}^{+ 0.18}$ $0.09_{-0.08}^{+0.18}$	$66_{- 20}^{+ 82}$ $66^{+82}_{-20}$	$1 . 87_{- 1.57}^{+ 15.75}$ $1.87_{-1.57}^{+15.75}$
Total				1.88 ± 0.2^a	–	7.5 ± 1.2 ^a	$5 . 7_{- 2.1}^{+ 3.3}$ $5.7^{+3.3}_{-2.1}$	–	8.78 ± 0.10

Notes. The dust slope β is fixed to β = 1.8. See Appendix D for details on the simultaneous fitting of the resolved and integrated FIR SED. ^a Independent fits to the Band 6+9 resolved data, without the total SED constraint. Note that the sum of the luminosity and mass of the independent fits to each annuli are likely biased, as the sum of their best-fit SED is not constrained - and does not reproduced well - the total FIR SED observations. These results are only given here for completeness. ^b Joint fit to the unresolved and resolved data detailed further in Appendix D. The best-fit annuli SEDs and their sum (including the AGN torus contribution) are shown in Fig. 3.

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