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Orion OB1: B-type stars vs nebular (M42) abundances (Simón-Díaz & Stasinska 2011)<br />
Taking care of O depletion onto dust grains... (see also Esteban et al. 1998)<br />
Draine (2003)<br />
O<br />
CEL<br />
RL<br />
Elem.<br />
Mg<br />
O (dust) = 125 – 135 ppM (± 10 ppm)<br />
Stars<br />
8.74 ± 0.04<br />
Gas<br />
8.52 ± 0.01<br />
8.65 ± 0.03<br />
Dust correction (O) = 0.09 – 0.16 dex<br />
Si<br />
Fe<br />
Gas + dust<br />
8.65 – 8.68<br />
8.74 – 8.79<br />
Stars<br />
7.51 ± 0.03 †<br />
7.57 ± 0.06 †<br />
7.50 ± 0.04 †<br />
6.50 ± 0.25<br />
6.50 ::<br />
6.0 ± 0.3<br />
Gas phase (M42)<br />
Rubin et al. (1993)<br />
Baldwin et al. 1991<br />
Rodríguez & Rubin (2005)
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