JADES - The diverse population of infant black holes at 4 < z < 11: Merging, tiny, poor, but mighty

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Volume 691 (November 2024)

A&A, 691 (2024) A145

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Table 3.

Parameters inferred for the broad-line AGNs presented in this JADES sub-sample.

ID	Comp.	lg(M_BH)	lg(L_bol)	L/L_Edd	lg(M_star)	lg(σ) ^(a)	R_∗	Sérsic index	lg(M_dyn)	M_UV	A_V ^(b)
		[M_⊙]	[erg s⁻¹]		[M_⊙]	km s⁻¹	[kpc]		[M_⊙]	[mag]	[mag]
10013704	BLR1	$5 . 65_{- 0.31}^{+ 0.31}$ $\rm 5.65^{+0.31}_{-0.31}$	43.8	1.06	$8 . 88_{- 0.66}^{+ 0.66}$ $\rm 8.88^{+0.66}_{-0.66}$	$1 . 93_{- 0.06}^{+ 0.05}$ $\rm 1.93^{+0.05}_{-0.06}$	0.15	0.8	$9 . 23_{- 0.13}^{+ 0.1}$ $\rm 9.23^{+0.1}_{-0.13}$	−18.89	0.27
10013704	BLR2	$7 . 5_{- 0.31}^{+ 0.31}$ $\rm 7.5^{+0.31}_{-0.31}$	44.3	0.06	$8 . 88_{- 0.66}^{+ 0.66}$ $\rm 8.88^{+0.66}_{-0.66}$	$1 . 93_{- 0.06}^{+ 0.05}$ $\rm 1.93^{+0.05}_{-0.06}$	0.15	0.8	$9 . 23_{- 0.13}^{+ 0.1}$ $\rm 9.23^{+0.1}_{-0.13}$	−18.89	0.27
8083		$7 . 25_{- 0.31}^{+ 0.31}$ $\rm 7.25^{+0.31}_{-0.31}$	44.6	0.16	$8 . 45_{- 0.03}^{+ 0.03}$ $\rm 8.45^{+0.03}_{-0.03}$	$1 . 9_{- 0.07}^{+ 0.06}$ $\rm 1.9^{+0.06}_{-0.07}$	0.11	5.7	$8 . 84_{- 0.15}^{+ 0.11}$ $\rm 8.84^{+0.11}_{-0.15}$	−18.67	0.64
1093		$7 . 36_{- 0.31}^{+ 0.32}$ $\rm 7.36^{+0.32}_{-0.31}$	44.8	0.2	$8 . 34_{- 0.2}^{+ 0.2}$ $\rm 8.34^{+0.2}_{-0.2}$	$1 . 95_{- 0.06}^{+ 0.05}$ $\rm 1.95^{+0.05}_{-0.06}$	–	–	–	−17.48	0.99
3608		$6 . 82_{- 0.33}^{+ 0.38}$ $\rm 6.82^{+0.38}_{-0.33}$	44.0	0.11	$8 . 38_{- 0.15}^{+ 0.11}$ $\rm 8.38^{+0.11}_{-0.15}$	$1 . 92_{- 0.07}^{+ 0.06}$ $\rm 1.92^{+0.06}_{-0.07}$	–	–	–	−19.5	0.48
11836		$7 . 13_{- 0.31}^{+ 0.31}$ $\rm 7.13^{+0.31}_{-0.31}$	44.5	0.2	$7 . 79_{- 0.3}^{+ 0.3}$ $\rm 7.79^{+0.3}_{-0.3}$	$1 . 96_{- 0.06}^{+ 0.05}$ $\rm 1.96^{+0.05}_{-0.06}$	0.48	0.8	$9 . 81_{- 0.14}^{+ 0.1}$ $\rm 9.81^{+0.1}_{-0.14}$	−18.75	0.68
20621		$7 . 3_{- 0.31}^{+ 0.31}$ $\rm 7.3^{+0.31}_{-0.31}$	44.7	0.18	$8 . 06_{- 0.7}^{+ 0.7}$ $\rm 8.06^{+0.7}_{-0.7}$	$1 . 93_{- 0.07}^{+ 0.06}$ $\rm 1.93^{+0.06}_{-0.07}$	–	–	–	−18.27	0.67
73488	BLR1	$6 . 18_{- 0.3}^{+ 0.3}$ $\rm 6.18^{+0.3}_{-0.3}$	44.7	2.48	$9 . 78_{- 0.2}^{+ 0.2}$ $\rm 9.78^{+0.2}_{-0.2}$	$1 . 64_{- 0.15}^{+ 0.11}$ $\rm 1.64^{+0.11}_{-0.15}$	0.59	0.8	$9 . 28_{- 0.41}^{+ 0.21}$ $\rm 9.28^{+0.21}_{-0.41}$	−18.73	0.45
73488	BLR2	$7 . 71_{- 0.3}^{+ 0.3}$ $\rm 7.71^{+0.3}_{-0.3}$	45.0	0.16	$9 . 78_{- 0.2}^{+ 0.2}$ $\rm 9.78^{+0.2}_{-0.2}$	$1 . 64_{- 0.15}^{+ 0.11}$ $\rm 1.64^{+0.11}_{-0.15}$	0.59	0.8	$9 . 28_{- 0.41}^{+ 0.21}$ $\rm 9.28^{+0.21}_{-0.41}$	−18.73	0.45
77652		$6 . 86_{- 0.34}^{+ 0.35}$ $\rm 6.86^{+0.35}_{-0.34}$	44.5	0.38	$7 . 87_{- 0.28}^{+ 0.16}$ $\rm 7.87^{+0.16}_{-0.28}$	$1 . 95_{- 0.07}^{+ 0.06}$ $\rm 1.95^{+0.06}_{-0.07}$	–	–	–	−18.28	0.39
61888		$7 . 22_{- 0.31}^{+ 0.31}$ $\rm 7.22^{+0.31}_{-0.31}$	44.8	0.32	$8 . 11_{- 0.92}^{+ 0.92}$ $\rm 8.11^{+0.92}_{-0.92}$	$1 . 85_{- 0.09}^{+ 0.07}$ $\rm 1.85^{+0.07}_{-0.09}$	0.09	0.9	$8 . 92_{- 0.46}^{+ 0.22}$ $\rm 8.92^{+0.22}_{-0.46}$	−19.0	0.69
62309		$6 . 56_{- 0.31}^{+ 0.32}$ $\rm 6.56^{+0.32}_{-0.31}$	44.2	0.39	$8 . 12_{- 0.13}^{+ 0.12}$ $\rm 8.12^{+0.12}_{-0.13}$	$1 . 87_{- 0.08}^{+ 0.07}$ $\rm 1.87^{+0.07}_{-0.08}$	0.21	1.3	$9 . 27_{- 0.2}^{+ 0.14}$ $\rm 9.27^{+0.14}_{-0.2}$	−18.67	0.74
53757	BLR1	$6 . 29_{- 0.32}^{+ 0.33}$ $\rm 6.29^{+0.33}_{-0.32}$	44.1	0.56	$10 . 18_{- 0.12}^{+ 0.13}$ $\rm 10.18^{+0.13}_{-0.12}$	$1 . 77_{- 0.11}^{+ 0.09}$ $\rm 1.77^{+0.09}_{-0.11}$	–	–	–	−18.9	0.36
53757	BLR2	$7 . 69_{- 0.31}^{+ 0.32}$ $\rm 7.69^{+0.32}_{-0.31}$	44.4	0.05	$10 . 18_{- 0.12}^{+ 0.13}$ $\rm 10.18^{+0.13}_{-0.12}$	$1 . 77_{- 0.11}^{+ 0.09}$ $\rm 1.77^{+0.09}_{-0.11}$	–	–	–	−18.9	0.36
954 ^(c)		$7 . 9_{- 0.3}^{+ 0.3}$ $\rm 7.9^{+0.3}_{-0.3}$	45.6	0.42	$10 . 66_{- 0.1}^{+ 0.09}$ $\rm 10.66^{+0.09}_{-0.1}$	$1 . 91_{- 0.06}^{+ 0.06}$ $\rm 1.91^{+0.06}_{-0.06}$	0.35	0.8	$9 . 56_{- 0.18}^{+ 0.13}$ $\rm 9.56^{+0.13}_{-0.18}$	−19.78	0.64
GN-z11 ^(d)		$6 . 2_{- 0.3}^{+ 0.3}$ $\rm 6.2^{+0.3}_{-0.3}$	45.0	5.5	$8 . 9_{- 0.3}^{+ 0.2}$ $\rm 8.9^{+0.2}_{-0.3}$	–	0.20	0.9		−21.79	0.0

Notes. ^(a)Central velocity dispersion of the host galaxy inferred from the narrow component of either Hα or, if not available, [OIII], from the high-resolution spectrum; the velocity dispersion is corrected for instrumental resolution and we have also applied a correction factor of 0.175 dex to take into account for the offset between gaseous and stellar velocity dispersion inferred by Bezanson et al. (2018). ^(b)Dust extinction toward the AGN from the low-resolution spectral fitting. ^(c)This is the most luminous AGN in the sample and the stellar and AGN light decomposition has been more challenging, and therefore the stellar mass might be significantly overestimated. ^(d)GN-z11 at z = 10.6, is still part of the JADES survey but the derivation of the parameters is reported in Maiolino et al. (2024a) and Tacchella et al. (2023).

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