HYPERION - Coevolution of supermassive black holes and galaxies at z > 6 and the build-up of massive galaxies

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Volume 689 (September 2024)

A&A, 689 (2024) A220

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Table C.3.

Results of the SED fitting

		J036+03	J0224-4711	J231-20	J2054-0005	J183+05	J1342+0928	J1319+0950	J1148+5251	J0100+2802	J2310+1855
HYP		Y	Y	Y	N	N	Y	N	Y	Y	N
z		6.540	6.522	6.587	6.390	6.439	7.540	6.133	6.419	6.327	6.003
M_dust	[10⁷ M_⊙]	6.1 ± 2.5	9.3 ± 2.7	53 ± 5	10.6 ± 2.4	45 ± 9	2.6 ± 1.4	63 ± 29	32 ± 8	2.3 ± 0.8	44 ± 7
T_dust	[K]	59 ± 2	$85_{- 8}^{+ 12}$ $85^{+12}_{-8}$	51 ± 3	64 ± 2	54 ± 5	55 ± 20	66 $_{- 12}^{+ 15}$ $^{+15}_{-12}$	75 ± 8	48 ± 2	71 ± 4
β		2.4 ± 0.2	1.7 ± 0.2	1.6 ± 0.1	2.1 ± 0.1	1.7 ± 0.2	1.8 ± 0.4	1.5 ± 0.3	1.5 ± 0.2	2.6 ± 0.2	1.86 ± 0.12
L_TIR	[10¹² L_⊙]	6.2 ± 1.0	33.2 $_{- 10}^{+ 22}$ $^{+22}_{-10}$	6.6 ± 1.6	9.8 ± 1.0	11.9 ± 4.0	2.4 $_{- 2.3}^{+ 3.7}$ $^{+3.7}_{-2.3}$	16 $_{- 6}^{+ 13}$ $^{+13}_{-6}$	21 ± 7	5.3 ± 0.6	2.48 $_{- 0.52}^{+ 0.62}$ $^{+0.62}_{-0.52}$
SFR	[M_⊙ yr⁻¹]	466 ± 75	2485 $_{- 768}^{+ 1682}$ $^{+1682}_{-768}$	496 ± 118	730 ± 75	894 ± 299	180 $_{- 170}^{+ 280}$ $^{+280}_{-170}$	1197 $_{- 449}^{+ 972}$ $^{+972}_{-449}$	1570 ± 524	396 ± 48	$1855_{- 389}^{+ 464}$ $1855^{+464}_{-389}$
Refs-D		This work	This work	This work	This work	TW,[1]	TW,[2]	[3]	[3]	[4]	[5]

M_gas	[10¹⁰ M_⊙]	0.7 ± 0.1	1.0 ± 0.1	1.4 ± 0.1	0.6 ± 0.1	4.5	< 0.35	1.5 ± 0.2	2.6	0.5 ± 0.2	4.4 ± 0.2
GDR		123	110	26	60	100	< 130	24	81	236	101
τ1_dep	[Gyr]	0.01	0.004	0.03	0.008	0.05	< 0.02	0.01	0.02	0.01	0.02
Refs-G		This work	This work	TW,[6]	This work	[1]	[2]	This work	[7]	[1]	[5]

Notes. The results for the QSOs on the left side of the first vertical line are entirely obtained from this work, that is, all observations were analyzed by the author. Between the two vertical lines, the results for J183+05 and J1342+0928 were obtained fitting their observed SEDs presented in Decarli et al. (2023) and Novak et al. (2019), respectively; the results for J1319+0950 and J1148+5251 are taken from Carniani et al. (2019). On the right side of the second vertical line, the results for J0100+2802 and J2310+1855 are taken from (Tripodi et al. 2023b, 2022), respectively. The SFRs are computed from L_TIR assuming a Kroupa IMF, and they are corrected by a factor of 50% in order to take the contribution of the AGN to the dust heating into account. The first raw shows whether the QSO belongs to the HYPERION sample. The gas mass for J231-20 is computed from the CO(7-6) luminosity in [6] using the r₇₆ derived in Sect. 5.2 for J1007+2115, and it agrees with that derived from [CI] in [2]. Refs-D: References for the dust properties and SFR. Refs-G: References for the gas mass. Refs: This work (TW); [1] Decarli et al. (2023); [2] Novak et al. (2019); [3] (Carniani et al. 2019); [4] (Tripodi et al. 2023b); [5] Tripodi et al. (2022); [6] Pensabene et al. (2021); [7] Stefan et al. (2015).

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