Fig. 3
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Mean molecular mass fractions per bin of metallicity. Top panels correspond to APOGEE-DR17; middle panels correspond to GALAH-DR3; bottom panels correspond to GALAH-DR2. Left panels correspond to the inner proto-planetary disc (T > 150 K); right panels correspond to the outer proto-planetary disc (T < 150 K, which includes H2O ice). For the inner proto-planetary disc, the MgSiO3 mass fraction is higher than the Mg2SiO4 mass fraction in APOGEE-DR17 and GALAH-DR3; albeit the trend with the metallicity is different. The MgSiO3 and the Mg2SiO4 mass fractions are reversed between the GALAH-DR2 and GALAH-DR3 but only at [Fe/H] > 0. For [Fe/H] < 0, the trend is similar. For the outer proto-planetary disc, the water ice mass fraction decreases with the metallicity in the three samples.
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