GA-NIFS: High number of dual active galactic nuclei at z ∼ 3

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Volume 696 (April 2025)

A&A, 696 (2025) A59

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Table A.3.

MUSE fit results.

target	dv	σ	$\frac{CIII]}{HeII}$ $\frac{\mathrm{CIII]}}{\mathrm{HeII}}$	$\frac{CIV}{HeII}$ $\frac{\mathrm{CIV}}{\mathrm{HeII}}$	$\frac{CIV}{CIII]}$ $\frac{\mathrm{CIV}}{\mathrm{CIII]}}$	$\frac{CIII] + CIV}{HeII}$ $\frac{\mathrm{CIII] + CIV}}{\mathrm{HeII}}$	$\frac{NV}{HeII}$ $\frac{\mathrm{NV}}{\mathrm{HeII}}$	$\frac{CIV}{NV}$ $\frac{\mathrm{CIV}}{\mathrm{NV}}$	$\frac{OIII]}{HeII}$ $\frac{\mathrm{OIII]}}{\mathrm{HeII}}$	L(He II)
	(km s⁻¹)	(km s⁻¹)								(erg s⁻¹)
GS10578	$- 260_{- 40}^{+ 50}$ $-260_{-40}^{+50}$	445 ± 30	$0 . 15_{- 0.03}^{+ 0.04}$ $0.15_{-0.03}^{+0.04}$	$0 . 24_{- 0.02}^{+ 0.04}$ $0.24_{-0.02}^{+0.04}$	$0 . 11_{- 0.04}^{+ 0.05}$ $0.11_{-0.04}^{+0.05}$	$0 . 54_{- 0.02}^{+ 0.04}$ $0.54_{-0.02}^{+0.04}$	$0 . 19_{- 0.04}^{+ 0.09}$ $0.19_{-0.04}^{+0.09}$	$0 . 05_{- 0.04}^{+ 0.09}$ $0.05_{-0.04}^{+0.09}$	< − 1.22	41.2 ± 0.1
LAE2	$208_{- 4}^{+ 10}$ $208_{-4}^{+10}$	$120_{- 9}^{+ 24}$ $120_{-9}^{+24}$	−0.08 ± 0.06	$0 . 03_{- 0.05}^{+ 0.07}$ $0.03_{-0.05}^{+0.07}$	$0 . 05_{- 0.05}^{+ 0.09}$ $0.05_{-0.05}^{+0.09}$	$0 . 24_{- 0.05}^{+ 0.07}$ $0.24_{-0.05}^{+0.07}$	< − 0.74	> 0.33	< − 0.85	40.8 ± 0.2

GS551	$- 2_{- 30}^{+ 10}$ $-2_{-30}^{+10}$	540 ± 20	0.02 ± 0.09	$0 . 63_{- 0.04}^{+ 0.08}$ $0.63_{-0.04}^{+0.08}$	$0 . 63_{- 0.05}^{+ 0.09}$ $0.63_{-0.05}^{+0.09}$	$0 . 73_{- 0.05}^{+ 0.07}$ $0.73_{-0.05}^{+0.07}$	$0 . 78_{- 0.05}^{+ 0.06}$ $0.78_{-0.05}^{+0.06}$	$- 0 . 14_{- 0.02}^{+ 0.03}$ $-0.14_{-0.02}^{+0.03}$	< − 0.44	41.9 ± 0.1

Notes. Best-fit spectroscopic results for the most prominent emission lines detected with MUSE. dv is the velocity offset with respect to the optical (NIRSpec) zero-velocities in the primary AGN. Luminosities and flux ratios are in log-scale.

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