Exploring a primordial solution for early black holes detected with JWST

Open Access

Table 1.

Black holes confirmed by the JWST at z ≳ 4.

No.	ID	Redshift	Log $\frac{M_{BH}}{M_{⊙}}$ $\frac{M_{\mathrm{BH}}}{\mathrm{M}_{\odot}}$	Signature	Log $\frac{N_{LF}}{{cMpc}^{3}}$ $\frac{{N_{\mathrm{LF}}}}{\mathrm{cMpc^3}}$	Log $\frac{N_{i}}{{cMpc}^{3}}$ $\frac{{N_i}}{\mathrm{cMpc^3}}$	Reference	Log $\frac{M_{PBH}}{M_{⊙}}$ $\frac{M_{\mathrm{PBH}}}{\mathrm{M}_{\odot}}$
1	GHZ9	10.4	$7 . 9_{- 0.22}^{+ 0.16}$ $7.9^{+0.16}_{-0.22}$	X-rays	−5.27	−5.57	Kovács et al. (2024)	3.9
2	UHZ1	10.3	$7 . 5_{- 0.5}^{+ 0.5}$ $7.5^{+0.5}_{-0.5}$	X-rays	−5.27	−5.57	Bogdán et al. (2024)	3.4
3	Abell2744–QSO1	7.04	$7 . 47_{- 0.17}^{+ 0.22}$ $7.47^{+0.22}_{-0.17}$	Hβ	−4.13	−4.44	Furtak et al. (2024)	0.7
4	CEERS 1670	5.24	$7 . 11_{- 0.16}^{+ 0.12}$ $7.11^{+0.12}_{-0.16}$	Hα	−	−4.97	Kocevski et al. (2023)	−2.7
5	JADES1146115	6.68	$8 . 61_{- 0.24}^{+ 0.27}$ $8.61^{+0.27}_{-0.24}$	Hα	−	−5.36	Juodžbalis et al. (2024)	2.3
6	GN–z11	10.6	$6 . 2_{- 0.3}^{+ 0.3}$ $6.2^{+0.3}_{-0.3}$	N, Ne lines	−	−6.06	Maiolino et al. (2024b),	1.3
							Fujimoto et al. (2023)
7	4286	5.84	8.0 ± 0.3	Hα	−4.37	−4.97	Greene et al. (2024)	−0.6
8	13123	7.04	7.3 ± 0.2	Hα	−4.58	−4.88	Greene et al. (2024)	0.5
9	13821	6.34	8.1 ± 0.2	Hα	−4.37	−4.97	Greene et al. (2024)	0.4
10	20466	8.5	8.14 ± 0.42	Hα	−4.88	−5	Greene et al. (2024),	2.9
							Kokorev et al. (2023)
11	23608	5.8	7.5 ± 0.2	Hα	−5	−5	Greene et al. (2024)	−1.2
12	35488	6.26	7.4 ± 0.2	Hα	−4.37	−4.97	Greene et al. (2024)	−0.5
13	38108	4.96	8.4 ± 0.5	Hα	−4.37	−4.97	Greene et al. (2024)	−2.1
14	41255	6.76	7.7 ± 0.4	Hα	−4.58	−4.88	Greene et al. (2024)	0.6
15	45924	4.46	8.9 ± 0.1	Hα	−5	−5	Greene et al. (2024)	−3.1
16	CEERS01244	4.47	$7 . 5_{- 0.02}^{+ 0.04}$ $7.5^{+0.04}_{-0.02}$	Hα	−3.04	−3.64	Harikane et al. (2023)	−4.5
17	GLASS 160133	4.01	$6 . 36_{- 0.01}^{+ 0.02}$ $6.36^{+0.02}_{-0.01}$	Hα	−3.04	−3.64	Harikane et al. (2023)	−7.3
18	GLASS 150029	4.58	$6 . 56_{- 0.03}^{+ 0.03}$ $6.56^{+0.03}_{-0.03}$	Hα	−3.04	−3.64	Harikane et al. (2023)	−5.1
19	CEERS 00746	5.62	$7 . 76_{- 0.1}^{+ 0.1}$ $7.76^{+0.1}_{-0.1}$	Hα	−3.82	−4.12	Harikane et al. (2023)	−1.3
20	CEERS 01665	4.48	$7 . 27_{- 0.12}^{+ 0.16}$ $7.27^{+0.16}_{-0.12}$	Hα	−5.05	−5.05	Harikane et al. (2023)	−4.7
21	CEERS 00672	5.66	$7 . 69_{- 0.12}^{+ 0.14}$ $7.69^{+0.14}_{-0.12}$	Hα	−3.82	−4.12	Harikane et al. (2023)	−1.2
22	CEERS 02782	5.24	$7 . 62_{- 0.11}^{+ 0.11}$ $7.62^{+0.11}_{-0.11}$	Hα	−3.85	−3.85	Harikane et al. (2023)	−2.2
23	CEERS 00397	6.0	$7 . 0_{- 0.3}^{+ 0.25}$ $7.0^{+0.25}_{-0.3}$	Hα	−5.45	−5.45	Harikane et al. (2023)	−1.3
24	CEERS 00717	6.93	$7 . 99_{- 0.17}^{+ 0.16}$ $7.99^{+0.16}_{-0.17}$	Hα	−5.79	−5.79	Harikane et al. (2023)	1.1
25	CEERS 01236	4.48	$7 . 25_{- 0.17}^{+ 0.2}$ $7.25^{+0.2}_{-0.17}$	Hα	−3.04	−3.64	Harikane et al. (2023)	−4.7
26	8083	4.64	$7 . 25_{- 0.0 . 31}^{+ 0.31}$ $7.25^{+0.31}_{-0.0.31}$	Hα	−3.06	−3.90	Maiolino et al. (2024a)	−4.2
27	1093	5.59	$7 . 36_{- 0.31}^{+ 0.31}$ $7.36^{+0.31}_{-0.31}$	Hα	−3.06	−3.90	Maiolino et al. (2024a)	−1.7
28	3608	5.26	$6 . 82_{- 0.33}^{+ 0.38}$ $6.82^{+0.38}_{-0.33}$	Hα	−3.83	−4.52	Maiolino et al. (2024a)	−2.9
29	11836	4.40	$7 . 13_{- 0.31}^{+ 0.31}$ $7.13^{+0.31}_{-0.31}$	Hα	−3.83	−4.52	Maiolino et al. (2024a)	−5.1
30	20621	4.68	$7 . 3_{- 0.31}^{+ 0.31}$ $7.3^{+0.31}_{-0.31}$	Hα	−3.06	−3.90	Maiolino et al. (2024a)	−4.0
31	77652	5.23	$6 . 86_{- 0.34}^{+ 0.34}$ $6.86^{+0.34}_{-0.34}$	Hα	−3.06	−3.90	Maiolino et al. (2024a)	−3.0
32	61888	5.87	$7 . 22_{- 0.31}^{+ 0.31}$ $7.22^{+0.31}_{-0.31}$	Hα	−3.83	−4.52	Maiolino et al. (2024a)	−1.3
33	62309	5.17	$6 . 56_{- 0.31}^{+ 0.31}$ $6.56^{+0.31}_{-0.31}$	Hα	−3.06	−3.90	Maiolino et al. (2024a)	−3.4
34	954	6.76	$7 . 9_{- 0.3}^{+ 0.3}$ $7.9^{+0.3}_{-0.3}$	Hα	−3.83	−4.52	Maiolino et al. (2024a)	0.8

Notes. For each object, we list the ID (column 2), the redshift (column 3), the inferred black hole mass (column 4), the signature (column 5), and the number density from the luminosity function (column 6) as quoted by the cited work (column 8). We assign the same weight to each object in a given luminosity bin for a given work to infer the individual number density calculated in column 7. Finally, we quote the primordial black hole seed mass for each object assuming continuous Eddington accretion onto this seed mass from a redshift of z = 3400.

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