Table 2
Differences among the mean abundances in the different stellar populations, as predicted by the different models (see text); they can be interpreted as gradients.
| Model | Δ ⟨[Fe/H]⟩ | Δ ⟨[Mg/H]⟩ | Δ ⟨[O/H]⟩ | Δ ⟨[S/H]⟩ | Δ ⟨[Si/H]⟩ | Δ ⟨[Ba/H]⟩ |
|
|
||||||
| MP–MR | –0.521 dex | –0.232 dex | –0.214 dex | –0.350 dex | –0.325 dex | –0.270 dex |
| EMP–IMP | –0.145 dex | –0.142 dex | –0.137 dex | –0.140 dex | –0.145 dex | –0.156 dex |
| bulge3 (0–1 kpc) | –0.36 dex kpc-1 | –0.29 dex kpc-1 | ||||
| bulge3 (0–0.5 kpc) | –0.26 dex kpc-1 | –0.21 dex kpc-1 | ||||
Notes. Only for model bulge3 do we show the real gradient as Δ ⟨ [X/H] ⟩ /ΔR and do we compute it for two distance ranges from the Galactic center (0–1 kpc and 0–0.5 kpc).
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