J/A+A/666/A12ivo://CDS.VizieR/J/A+A/666/A12doi:10.26093/cds/vizier.36660012CDSKonstantopoulou C.De Cia A.Krogager J.-K.Ledoux C.Noterdaeme P.,Fynbo J.P.U.Heintz K.E.Watson D.Andersen A.C.Ramburuth-hurt T.,Jermann I.2024-01-18T12:34:33Z2023-02-22T12:50:47ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frquasarschemical-abundancesvisible-astronomyultraviolet-astronomyLarge fractions of metals are missing from the observable gas-phase in the interstellar medium (ISM) because they are incorporated into dust grains. This phenomenon is called dust depletion. It is important to study the depletion of metals into dust grains in the ISM to investigate the origin and evolution of metals and cosmic dust. We characterize the dust depletion of several metals from the Milky Way to distant galaxies. We collected measurements of ISM metal column densities from absorption-line spectroscopy in the literature, and in addition, we determined Ti and Ni column densities from a sample of 70 damped Lyman-{alpha} absorbers (DLAs) toward quasars that were observed at high spectral resolution with the Very Large Telescope (VLT) Ultraviolet and Visual Echelle Spectrograph (UVES). We used relative ISM abundances to estimate the dust depletion of 18 metals (C, P, O, Cl, Kr, S, Ge, Mg, Si, Cu, Co, Mn, Cr, Ni, Al, Ti, Zn, and Fe) for different environments (the Milky Way, the Magellanic Clouds, and DLAs toward quasars and towards gamma-ray bursts). We observed overall linear relations between the depletion of each metal and the overall strength of the dust depletion, which we traced with the observed [Zn/Fe]. The slope of these dust depletion sequences correlates with the condensation temperature of the various elements, that is, the more refractory elements show steeper depletion sequences. In the neutral ISM of the Magellanic Clouds, small deviations from linearity are observed as an overabundance of the {alpha}-elements Ti, Mg, S, and an underabundance of Mn, including for metal-rich systems. The Ti, Mg, and Mn deviations completely disappear when we assume that all systems in our sample of OB stars observed toward the Magellanic Clouds have an {alpha}-element enhancement and Mn underabundance, regardless of their metallicity. This may imply that the Magellanic Clouds have recently been enriched in {alpha}-elements, potentially through recent bursts of star formation. We also observe an S overabundance in all local galaxies, which is an effect of ionization due to the contribution of their HII regions to the measured SII column densities. The observed strong correlations of the depletion sequences of the metals all the way from low-metallicity quasi-stellar object DLAs to the Milky Way suggest that cosmic dust has a common origin, regardless of the star formation history, which, in contrast, varies significantly between these different galaxies. This supports the importance of grain growth in the ISM as a significant process of dust production.2022A&A...666A..12Khttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/666/A12CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/ApJ/700/1299 : Gas-phase element depletions in the ISM (Jenkins, 2009)J/MNRAS/452/4326 : Metal-rich damped Ly{alpha} systems at z~2 (Berg+, 2015)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/666/A12https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/666/A12http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/666/A12https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/666/A12https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/666/A12http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/666/A12GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/666/A12/tabled1 (*QSO-DLA column densities)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/666/A12/tabled1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/666/A12/tabled1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/666/A12/tabled1?GETtext/xml+votable180.050000true0.8456383-26.05508440.005555555555555556Cone search capability for table J/A+A/666/A12/tabled2 (*Milky Way column densities)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/666/A12/tabled2?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/666/A12/tabled2?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/666/A12/tabled2?GETtext/xml+votable180.050000true43.4200208-26.15567440.005555555555555556Cone search capability for table J/A+A/666/A12/tabled3 (*Milky Way column densities for elements with limited coverage)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/666/A12/tabled3?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/666/A12/tabled3?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/666/A12/tabled3?GETtext/xml+votable180.050000true43.4200208-26.15567440.0055555555555555566/2 1060 1196 1539 1558 1633 2172 2348 4279 4481 4488 5439 5452 5739 5780 6403 7964 8343 8395 8939 9730 9806 9940 9968 10061 10103 10432 10571 10602 11113 11498 12563 14825 15369 15478 16589 16752 16798 17215 17257 17314 17317 17404 17510 17772 17917 17999 18029 18084 18086 18308 18366 18765 18790 18858 19206 19456 19490 19682 20107 20516 20613 21012 21180 21438-21439 22854 22862 22884 22917 22994 25245 25294 25307 25950 26165-26166 26362 26453 26586 26614 26981 27022 27037 27225-27226 27510 27650 27687 27728 27747 27780 27943 28039 28042 28539 28669 28915 29893 30722 30818 31547 31705 34107 34379 34503 35751 36043 36086 38853 39100 39281 39327 39334 39907 41103 41630 42366 42408 42470 42657 42672 42687 42981 43024 43062 44305 44312 44389 46208 46529 46651 46851 48149 48474 49100 49103https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/666/A12?format=asciiUVOpticaldefaultJ/A+A/666/A12/tabled1*QSO-DLA column densitiesQSOQSO namemeta.id;meta.maincharSimbadNameSimbad column added by the CDSmeta.idcharnullablerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintzabsAbsorption redshiftsrc.redshiftfloatlogN(HI)? HI column densitylog(cm**-2)phys.columnDensityfloatnullablel_logN(TiII)Limit flag on logN(TiII)meta.code.errorchare_logN(HI)? HI column density errorlog(cm**-2)stat.errorfloatnullablelogN(OI)? OI column densitylog(cm**-2)phys.columnDensityfloatnullablee_logN(OI)? OI column density errorlog(cm**-2)stat.errorfloatnullablelogN(MgII)? MgII column densitylog(cm**-2)phys.columnDensityfloatnullablee_logN(MgII)? MgII column density errorlog(cm**-2)stat.errorfloatnullablelogN(SiII)? SiII column densitylog(cm**-2)phys.columnDensityfloatnullablee_logN(SiII)? SiII column density errorlog(cm**-2)stat.errorfloatnullablelogN(SII)? SII column densitylog(cm**-2)phys.columnDensityfloatnullablee_logN(SII)? SII column density errorlog(cm**-2)stat.errorfloatnullablelogN(PII)? PII column densitylog(cm**-2)phys.columnDensityfloatnullablee_logN(PII)? PII column density errorlog(cm**-2)stat.errorfloatnullablelogN(TiII)? TiII column densitylog(cm**-2)phys.columnDensityfloatnullablee_logN(TiII)? TiII column density errorlog(cm**-2)stat.errorfloatnullablelogN(CrII)? CrII column densitylog(cm**-2)phys.columnDensityfloatnullablee_logN(CrII)? CrII column density errorlog(cm**-2)stat.errorfloatnullablelogN(MnII)? MnII column densitylog(cm**-2)phys.columnDensityfloatnullablee_logN(MnII)? MnII column density errorlog(cm**-2)stat.errorfloatnullablelogN(FeII)? FeII column densitylog(cm**-2)phys.columnDensityfloatnullablee_logN(FeII)? FeII column density errorlog(cm**-2)stat.errorfloatnullablelogN(CoII)? CoII column densitylog(cm**-2)phys.columnDensityfloatnullablee_logN(CoII)? CoII column density errorlog(cm**-2)stat.errorfloatnullablel_logN(NiII)Limit flag on logN(NiII)meta.code.errorcharlogN(NiII)? NiII column densitylog(cm**-2)phys.columnDensityfloatnullablee_logN(NiII)? NiII column density errorlog(cm**-2)stat.errorfloatnullablelogN(ZnII)? ZnII column densitylog(cm**-2)phys.columnDensityfloatnullablee_logN(ZnII)? ZnII column density errorlog(cm**-2)stat.errorfloatnullableRefsReferences (1)meta.ref;pos.framechar_RARight Ascension (J2000) from SIMBAD (not part of the original data)degpos.eq.ra;meta.main_DEDeclination (J2000) from SIMBAD (not part of the original data)degpos.eq.dec;meta.mainJ/A+A/666/A12/tabled2*Milky Way column densitiesSimbadNameSimbad column added by the CDSmeta.idcharnullablee_logN(SII)? SII column density errorlog(cm**-2)stat.errorfloatnullablerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintStarStar namemeta.id;meta.maincharlogN(PII)? PII column densitylog(cm**-2)phys.columnDensityfloatnullablee_logN(PII)? PII column density errorlog(cm**-2)stat.errorfloatnullablelogN(MgII)? MgII column densitylog(cm**-2)phys.columnDensityfloatnullablee_logN(MgII)? MgII column density errorlog(cm**-2)stat.errorfloatnullablelogN(SiII)? SiII column densitylog(cm**-2)phys.columnDensityfloatnullablee_logN(SiII)? SiII column density errorlog(cm**-2)stat.errorfloatnullablelogN(SII)? SII column densitylog(cm**-2)phys.columnDensityfloatnullablelogN(TiII)? TiII column densitylog(cm**-2)phys.columnDensityfloatnullablee_logN(TiII)? TiII column density errorlog(cm**-2)stat.errorfloatnullablelogN(CrII)? CrII column densitylog(cm**-2)phys.columnDensityfloatnullablee_logN(CrII)? CrII column density errorlog(cm**-2)stat.errorfloatnullablelogN(MnII)? MnII column densitylog(cm**-2)phys.columnDensityfloatnullablee_logN(MnII)? MnII column density errorlog(cm**-2)stat.errorfloatnullablelogN(FeII)? FeII column densitylog(cm**-2)phys.columnDensityfloatnullablee_logN(FeII)? FeII column density errorlog(cm**-2)stat.errorfloatnullablelogN(NiII)? NiII column densitylog(cm**-2)phys.columnDensityfloatnullablee_logN(NiII)? NiII column density errorlog(cm**-2)stat.errorfloatnullablelogN(ZnII)? ZnII column densitylog(cm**-2)phys.columnDensityfloatnullablee_logN(ZnII)? ZnII column density errorlog(cm**-2)stat.errorfloatnullableRefsReferences (1)meta.ref;pos.framechar_RARight Ascension (J2000) from SIMBAD (not part of the original data)degpos.eq.ra;meta.main_DEDeclination (J2000) from SIMBAD (not part of the original data)degpos.eq.dec;meta.mainJ/A+A/666/A12/tabled3*Milky Way column densities for elements with limited coveragelogN(FeII)? FeII column densitylog(cm**-2)phys.columnDensityfloatnullablee_logN(FeII)? FeII column density errorlog(cm**-2)stat.errorfloatnullablelogN(ZnII)? ZnII column densitylog(cm**-2)phys.columnDensityfloatnullablee_logN(ZnII)? ZnII column density errorlog(cm**-2)stat.errorfloatnullablelogN(CoII)? CoII column densitylog(cm**-2)phys.columnDensityfloatnullablee_logN(CoII)? CoII column density errorlog(cm**-2)stat.errorfloatnullablelogN(GeII)? GeII column densitylog(cm**-2)phys.columnDensityfloatnullablee_logN(GeII)? GeII column density errorlog(cm**-2)stat.errorfloatnullablelogN(KrI)? KrI column densitylog(cm**-2)phys.columnDensityfloatnullablee_logN(KrI)? KrI column density errorlog(cm**-2)stat.errorfloatnullablelogN(ClII)? ClII column densitylog(cm**-2)phys.columnDensityfloatnullablee_logN(ClII)? ClII column density errorlog(cm**-2)stat.errorfloatnullablelogN(CuII)? CuII column densitylog(cm**-2)phys.columnDensityfloatnullablee_logN(CuII)? CuII column density errorlog(cm**-2)stat.errorfloatnullablelogN(AlII)? AlII column densitylog(cm**-2)phys.columnDensityfloatnullablee_logN(AlII)? AlII column density errorlog(cm**-2)stat.errorfloatnullablelogN(CII)? CII column densitylog(cm**-2)phys.columnDensityfloatnullablee_logN(CII)? CII column density errorlog(cm**-2)stat.errorfloatnullableRefsReferences (1)meta.ref;pos.framechar_RARight Ascension (J2000) from SIMBAD (not part of the original data)degpos.eq.ra;meta.main_DEDeclination (J2000) from SIMBAD (not part of the original data)degpos.eq.dec;meta.mainSimbadSimbad column added by the CDSmeta.ref.urlcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintStarStar namemeta.id;meta.maincharlogN(OI)? OI column densitylog(cm**-2)phys.columnDensityfloatnullablee_logN(OI)? OI column density errorlog(cm**-2)stat.errorfloatnullable