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Using current solar abundances (Asplund et al. 2009), we convert the gas-phase abundances into dust-phase abundances for 196 sightlines. We deduce a sharp difference in abundances for sightlines located at low ($|b|<30\\degr$) and high ($|b|>30\\degr$) galactic latitudes. For high-latitude stars the ratios Mg/Si and Fe/Si in dust are close to 1.5. For disk stars they are reduced to ${\\rm Mg/Si} \\sim 1.2$ and ${\\rm Fe/Si} \\sim 1.05$. 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