Mocking integral field unit observations and metallicity diagnostics from cosmological simulations

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Table 3.

Predicted metallicity calibrations.

Line ratio	Fit	Lower curve	Upper curve
N2	c₀=−21.243 c₁ = 4.007 c₂=−0.192	c₀=−21.492 c₁ = 4.028 c₂=−0.193	c₀=−20.994 c₁ = 3.986 c₂=−0.191
R23	c₀=−38.566 c₁ = 9.645 c₂=−0.589	c₀=−38.730 c₁ = 9.659 c₂=−0.590	c₀=−38.403 c₁ = 9.631 c₂=−0.588
$\hat{R}$ ${\hat {\mathrm {R}}}$	c₀=−39.436 c₁ = 9.810 c₂=−0.599	c₀=−39.574 c₁ = 9.821 c₂=−0.600	c₀=−39.298 c₁ = 9.798 c₂=−0.599
O3N2	c₀=−20.276 c₁ = 6.312 c₂=−0.438	c₀=−20.683 c₁ = 6.346 c₂=−0.440	c₀=−19.870 c₁ = 6.278 c₂=−0.436
N2O2	c₀ = 10.313 c₁=−3.532 c₂ = 0.264	c₀ = 10.199 c₁=−3.522 c₂ = 0.264	c₀ = 10.427 c₁=−3.541 c₂ = 0.265

Notes. As in Table 2, but considering the spectra attenuated by both dust within the H II regions and ISM dust within the LoS, assuming the Calzetti law (Calzetti et al. 2000). These curves are represented by the pink, dashed lines in Fig. 6.

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