Fast supermassive black hole growth in the SPT2349–56 protocluster at z = 4.3

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Volume 689 (September 2024)

A&A, 689 (2024) A130

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Table 2.

Positions and X-ray photometric properties of the two members of the protocluster detected with Chandra (see Sect. 2.2).

ID	RA	Dec	C_sb	C_hb	C_fb	HR	Γ_eff	N_H	F_{0.5 − 7 keV}	L_{2 − 10 keV}
	J2000	J2000						[10²⁴ cm⁻²]	[10⁻¹⁵ erg cm⁻² s⁻¹]	[10⁴⁵ erg s⁻¹]
(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)	(9)	(10)	(11)
C1	23:49:42.65	−56:38:19.4	< 4.8	$19 . 1_{- 4.1}^{+ 4.8}$ $19.1^{+ 4.8}_{-4.1}$	$20 . 5_{- 4.4}^{+ 5.0}$ $20.5^{+ 5.0}_{-4.4}$	> 0.58	< 0.13	$2 . 4_{- 1.2}^{+ 2.3}$ $2.4_{-1.2}^{+2.3}$	$2 . 4_{- 1.5}^{+ 4.9}$ $2.4_{-1.5}^{+4.9}$	$2 . 2_{- 1.4}^{+ 4.5}$ $2.2_{-1.4}^{+4.5}$
C6	23:49:42.84	−56:38:25.1	< 2.3	$3 . 6_{- 1.7}^{+ 2.4}$ $3.6^{+ 2.4}_{-1.7}$	$3 . 3_{- 1.7}^{+ 2.4}$ $3.3^{+ 2.4}_{-1.7}$	> 0.18	< 1.22	> 0.4	$0 . 3_{- 0.1}^{+ 0.2}$ $0.3_{-0.1}^{+0.2}$	> 0.02

Notes. (1) ID, (2) RA, and (3) Dec from Hill et al. (2020) of the detected X-ray sources; (4) soft-band, (5) hard-band, and (6) full-band net counts; (7) hardness ratio and (8) corresponding effective photon index; (9) column density; (10) full-band flux; (11) intrinsic luminosity. The column density, flux, and luminosity of C1 are derived via a spectral analysis (Sect. 3.1), whereas these quantities are based on the hardness ratio for C6 (Sect. 3.3).

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