Low-Eddington ratio, changing-look active galactic nuclei: The case of NGC 4614

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Table 1.

Integrated luminosities and EWs resulting from the fit for the main emission lines.

Year	$L_{H α}^{B}$ $L^{\mathrm{B}}_{\mathrm{H\alpha}}$	EW $_{H α}^{B}$ $^{\mathrm{B}}_{\mathrm{H\alpha}}$	$L_{H β}^{N}$ $L^{\mathrm{N}}_{\mathrm{H\beta}}$	EW $_{H β}^{N}$ $^{\mathrm{N}}_{\mathrm{H\beta}}$	$L_{H α}^{N}$ $L^{\mathrm{N}}_{\mathrm{H\alpha}}$	EW $_{H α}^{N}$ $^{\mathrm{N}}_{\mathrm{H\alpha}}$	$L_{[OIII]}^{N}$ $L^{\mathrm{N}}_{\mathrm{[OIII]}}$	EW $_{[OIII]}^{N}$ $^{\mathrm{N}}_{\mathrm{[OIII]}}$
2005/SDSS	5.74 ± 0.06	50.7 ± 0.5	0.3 ± 0.1^*	2.4 ± 0.1^*	1.30 ± 0.02	11.4 ± 0.2	0.51 ± 0.02	4.8 ± 0.1
2024/LR-B	–	–	0.34 ± 0.03	3.0 ± 0.2	2.0 ± 0.1	18.6 ± 0.6	0.85 ± 0.03	8.1 ± 0.3
2024/VHR-R	1.13 ± 0.02	9.8 ± 0.2	–	–	1.40 ± 0.02	12.0 ± 0.1	–	–

Notes. For each line measurement, both the broad (B) and narrow (N) components are provided if constrained by the fit. Gaussian profiles are considered. Luminosities and EWs are in units of 10⁴⁰ erg s⁻¹ and Å, respectively. Measurements marked with ^* are not well constrained (i.e. have a warning flag in the fit).

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