Unlocking the mystery of strontium synthesis in the early Galaxy through analysis of barium isotopes in very metal-poor stars

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Table 2

NLTE abundance corrections and EWs in mÅ for Ti II lines as a function of T_eff, log g, and [Fe/H].

λ, Å species E_exc, eV log gf
T_eff1, K	log g₁	log g₂	log g₃	log g₄	log g₅	log g₆
[Fe/H]₁	EW₁	EW₂	EW₃	EW₄	EW₅	EW₆
[Fe/H]₁	Δ₁	Δ₂	Δ₃	Δ₄	Δ₅	Δ₆

4417.710, Ti II, E_exc = 1.16, log gf = −1.19
T_eff = 5000	1.0	1.5	2.0	2.5	3.0	3.5
−2.0	−1	124	106	92	79	−1
−2.0	−1	−0.094	−0.085	−0.065	−0.049	−1

Notes. The table is accessible in a machine-readable format at the CDS. A portion is shown to illustrate its format and content. If EW = −1 and Δ_NLTE = −1, this means that EW is either <3 mÅ or not computed in a model atmosphere with given parameters.

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