The chemical composition of the Orion star forming region - II. Stars, gas, and dust: the abundance discrepancy conundrum

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Table 5

Summary of gas-phase abundances in the Orion nebula.

A	ϵ(A)	Data	Source	Method	Major uncertainties

C	8.40 ± 0.25	CEL: C iii]1907,09	Rubin et al. (1993)	model	dereddening, CII not fitted
	8.37 ± 0.03	RL: C ii	C⁺⁺: E04	icf (own model)
N	7.92 ± 0.09	CEL: [N ii]6584	data: E04, N⁺: this paper	icf (own model)	icf
O	8.52 ± 0.01	CEL: [O iii]5007, [O ii]3727	data: E04, O⁺ & O⁺⁺: this paper	no icf needed
	8.65 ± 0.03	RL: O iii	O⁺⁺: E04	icf (own model)
Ne	8.05 ± 0.03	CEL: [Ne iii]3869	data: E04, Ne⁺⁺: this paper	icf (own model)
	7.84 ± 0.03	CEL: [Ne iii]3869	data: E04, Ne⁺⁺: this paper	icf (classical)
	8.25 ± 0.35	RL: Ne ii	Ne⁺⁺: E04^a	icf (own model)
	8.03 ± 0.26	RL: Ne ii	Ne⁺⁺: E04^a	icf (classical)
S	6.87 ± 0.06	CEL: [S iii]9069	data: E04, S⁺⁺: this paper	icf (own model)
Ar	6.39 ± 0.03	CEL: [Ar iii]7135	data: E04, S⁺⁺: this paper	icf (own model)
Mg	6.50 ::	CEL: Mg ii 2798	Baldwin et al. (1991)	model	intensity, interstellar absorption
Si	6.50 ± 0.25	CEL: Si iii]1883,92	Rubin et al. (1993)	model	Si/C more accurate than Si/H
Fe	6.0 ± 0.3	CEL: [Fe ii], [Fe iii], [Fe iv]	Rodríguez & Rubin (2005)	model	sum of observed ions gives
					different result

Notes.

^(a)

The uncertainty for Ne⁺⁺ was erroneaously given as 0.09 dex in E04, instead of 0.2 dex (García-Rojas, private communication).

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