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• W3100361350 endingPage "A97" @default.
• W3100361350 startingPage "A97" @default.
• W3100361350 abstract "We study metal depletion due to dust in the interstellar medium (ISM) to infer the properties of dust grains and characterize the metal and dust content of galaxies down to low metallicity and intermediate redshift z. We provide metal column densities and abundances of a sample of 70 damped Lyman-α absorbers (DLAs) towards quasars, observed at high spectral resolution with the Very Large Telescope (VLT) Ultraviolet and Visual Echelle Spectrograph (UVES). This is the largest sample of phosphorus abundances measured in DLAs so far. We use literature measurements for Galactic clouds to cover the high-metallicity end. We discover tight (scatter ≲ 0.2 dex) correlations between [Zn/Fe] and the observed relative abundances from dust depletion. This implies that grain growth in the ISM is an important process of dust production. These sequences are continuous in [Zn/Fe] from dust-free to dusty DLAs, and to Galactic clouds, suggesting that the availability of refractory metals in the ISM is crucial for dust production, regardless of the star formation history. We observe [S/Zn] up to ~0.25 dex in DLAs, which is broadly consistent with Galactic stellar abundances. Furthermore, we find a good agreement between the nucleosynthetic pattern of Galactic halo stars and our observations of the least dusty DLAs. This supports recent star formation in low-metallicity DLAs. The derived depletions of Zn, O, P, S, Si, Mg, Mn, Cr, and Fe correlate with [Zn/Fe], with steeper slopes for more refractory elements. P is mostly not affected by dust depletion. We present canonical depletion patterns to be used as reference in future studies of relative abundances and depletion. We derive the total (dust-corrected) metallicity, typically −2 ≲ [M/H] tot ≲ 0 for DLAs, and scattered around solar metallicity for the Galactic ISM. The dust-to-metal ratio () increases with metallicity, again supporting the importance of grain growth for dust production. The dust extinction AV derived from the depletion is typically <0.2 mag in DLAs. Finally, we derive elemental abundances in dust, which is key to understanding the dust composition and its evolution. We observe similar abundances of Mg, Si, and Fe in dust; this suggests that grain species such as pyroxenes and iron oxides are more important than olivine, but this needs to be confirmed by more detailed analysis. Overall, we characterize dust depletion, nucleosynthesis, and dust-corrected metallicity in DLAs, providing a unified picture from low-metallicity systems to the Galactic ISM." @default.
• W3100361350 created "2020-11-23" @default.
• W3100361350 creator A5007052267 @default.
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• W3100361350 creator A5076292184 @default.
• W3100361350 creator A5079300560 @default.
• W3100361350 creator A5084059584 @default.
• W3100361350 creator A5088192303 @default.
• W3100361350 date "2016-12-01" @default.
• W3100361350 modified "2023-10-12" @default.
• W3100361350 title "Dust-depletion sequences in damped Lyman-<i>α</i>absorbers" @default.
• W3100361350 cites W1501582143 @default.
• W3100361350 cites W1523639169 @default.
• W3100361350 cites W1524502439 @default.
• W3100361350 cites W1573299053 @default.
• W3100361350 cites W1634574618 @default.
• W3100361350 cites W1658763637 @default.
• W3100361350 cites W1787117759 @default.
• W3100361350 cites W1814975636 @default.
• W3100361350 cites W1868862929 @default.
• W3100361350 cites W1973412110 @default.
• W3100361350 cites W1973815499 @default.
• W3100361350 cites W1974418581 @default.
• W3100361350 cites W1976679348 @default.
• W3100361350 cites W1978009383 @default.
• W3100361350 cites W1978084091 @default.
• W3100361350 cites W1983716874 @default.
• W3100361350 cites W1984879627 @default.
• W3100361350 cites W2000481895 @default.
• W3100361350 cites W2001490443 @default.
• W3100361350 cites W2008710846 @default.
• W3100361350 cites W2008724305 @default.
• W3100361350 cites W2008991502 @default.
• W3100361350 cites W2011646311 @default.
• W3100361350 cites W2013839573 @default.
• W3100361350 cites W2015798867 @default.
• W3100361350 cites W2016280819 @default.
• W3100361350 cites W2034457553 @default.
• W3100361350 cites W2037309326 @default.
• W3100361350 cites W2040615387 @default.
• W3100361350 cites W2042583444 @default.
• W3100361350 cites W2043258333 @default.
• W3100361350 cites W2057439642 @default.
• W3100361350 cites W2064888972 @default.
• W3100361350 cites W2074040676 @default.
• W3100361350 cites W2077504681 @default.
• W3100361350 cites W2084775107 @default.
• W3100361350 cites W2089167229 @default.
• W3100361350 cites W2092929107 @default.
• W3100361350 cites W2096471541 @default.
• W3100361350 cites W2097292025 @default.
• W3100361350 cites W2100461368 @default.
• W3100361350 cites W2103896241 @default.
• W3100361350 cites W2110941132 @default.
• W3100361350 cites W2112879294 @default.
• W3100361350 cites W2114317630 @default.
• W3100361350 cites W2116610103 @default.
• W3100361350 cites W2117105462 @default.
• W3100361350 cites W2119746764 @default.
• W3100361350 cites W2123197592 @default.
• W3100361350 cites W2123367369 @default.
• W3100361350 cites W2123829915 @default.
• W3100361350 cites W2123924478 @default.
• W3100361350 cites W2125426812 @default.
• W3100361350 cites W2139594802 @default.
• W3100361350 cites W2140341131 @default.
• W3100361350 cites W2147018772 @default.
• W3100361350 cites W2157126200 @default.
• W3100361350 cites W2157577462 @default.
• W3100361350 cites W2157594202 @default.
• W3100361350 cites W2158091684 @default.
• W3100361350 cites W2158536470 @default.
• W3100361350 cites W2159264410 @default.
• W3100361350 cites W2165031544 @default.
• W3100361350 cites W2166710450 @default.
• W3100361350 cites W2169224160 @default.
• W3100361350 cites W2192976736 @default.
• W3100361350 cites W2227040008 @default.
• W3100361350 cites W2264263942 @default.
• W3100361350 cites W2267934497 @default.
• W3100361350 cites W2277438896 @default.
• W3100361350 cites W2474884382 @default.
• W3100361350 cites W2899497983 @default.
• W3100361350 cites W2951559137 @default.
• W3100361350 cites W2987869637 @default.
• W3100361350 cites W3098072422 @default.
• W3100361350 cites W3098796376 @default.
• W3100361350 cites W3099137176 @default.
• W3100361350 cites W3099140520 @default.
• W3100361350 cites W3099862774 @default.
• W3100361350 cites W3100163303 @default.
• W3100361350 cites W3101273319 @default.
• W3100361350 cites W3103037995 @default.
• W3100361350 cites W3104418698 @default.
• W3100361350 cites W3104707606 @default.
• W3100361350 cites W3105230740 @default.
• W3100361350 cites W3105299221 @default.

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