JADES: Detecting [OIII]λ4363 emitters and testing strong line calibrations in the high-z Universe with ultra-deep JWST/NIRSpec spectroscopy up to z ∼ 9.5

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Table 3.

Significance of deviation (in units of σ) for the expected line ratios from each strong-line calibration to our JADES sample presented in Figs. 4–7.

	Maiolino et al. (2008)				Curti et al. (2017, 2020)				Bian et al. (2018)
	R2	R3	R23	O3O2	R2	R3	R23	O3O2	R2	R3	R23	O3O2
σ_cal	0.10	0.10	0.06	0.20	0.11	0.09	0.06	0.15	−	0.15	0.15	0.15
Sample deviation	1.17	1.12	1.04	1.11	1.13	0.95	1.04	1.11	−	0.50	0.58	0.96

	Nakajima et al. (2022) All				Nakajima et al. (2022) Large EW				Nakajima et al. (2022) Small EW

	R2	R3	R23	O3O2	R2	R3	R23	O3O2	R2	R3	R23	O3O2
σ_cal	0.27	0.16	0.10	0.39	0.21	0.06	0.06	0.25	0.21	0.17	0.08	0.35
Sample deviation	1.05	1.05	1.04	1.13	1.09	0.66	0.74	0.96	1.32	1.67	1.28	1.60

Notes. The metallicity dependency varies across each strong-line diagnostic examined (e.g., the turnover points in R3 and R23), thus we include (12 + log(O/H)_{T_e})−(12 + log(O/H)_cal) in Figs. 4–7 to demonstrate offsets with the respect to 12 + log(O/H)_{T_e} for our individual galaxies.

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