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We present data on the gas phase abundances for 9 different elements in theinterstellar medium of the Small Magellanic Cloud (SMC), based on the strengthsof ultraviolet absorption features over relevant velocities in the spectra of18 stars within the SMC. From this information and the total abundances definedby the element fractions in young stars in the SMC, we construct a generalinterpretation on how these elements condense into solid form onto dust grains.As a group, the elements Si, S, Cr, Fe, Ni, and Zn exhibit depletion sequencessimilar to those in the local part of our Galaxy defined by Jenkins (2009). Theelements Mg and Ti deplete less rapidly in the SMC than in the Milky Way, andMn depletes more rapidly. We speculate that these differences might beexplained by the different chemical affinities to different existing grainsubstrates. For instance, there is evidence that the mass fractions ofpolycyclic aromatic hydrocarbons (PAHs) in the SMC are significantly lower thanthose in the Milky Way. We propose that the depletion sequences that weobserved for the SMC may provide a better model for interpreting the elementabundances in low metallicity Damped Lyman Alpha (DLA) and sub-DLA absorptionsystems that are recorded in the spectra of distant quasars and gamma ray burstafterglows.

Interstellar Gas-phase Element Depletions in the Small Magellanic Cloud: A Guide to Correcting for Dust in QSO Absorption Line Systems