J/A+A/700/A154ivo://CDS.VizieR/J/A+A/700/A154doi:10.26093/cds/vizier/bc-nw/lbfeCDSDodd E.Matsuno T.Helmi A.Balbinot E.Callingham T.M.Starkenburg E.,Woudenberg H.C.Ruiz-Lara T.2026-08-03T06:56:12Z2025-08-14T09:02:04ZCDS support team

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

cds-question@unistra.frmilky-way-galaxyhalo-starschemical-abundancesline-intensitiesultraviolet-astronomyThe local stellar halo of the Milky Way is known to contain the debris from accreted dwarf galaxies and globular clusters, in the form of stellar streams and over-densities in the space of orbital properties (e.g. integrals of motion). While several over-densities have been uncovered and characterised dynamically using Gaia data, their nature is not always clear. Especially for a full understanding of the smaller halo substructures, the kinematic information from Gaia needs to be coupled with chemical information. In this work, we combine Gaia data with targeted high-resolution UVES spectroscopy of five small substructures that were recently discovered in the local halo, namely the ED-2, 3, 4, 5 and 6; the ED streams. We present the chemical abundances measured from our newly obtained UVES spectra (20 stars) and from archival UVES spectra (9 stars). We compare these with homogeneously derived abundances from archive spectra of 12 Gaia Enceladus (GE) stars. The chemical abundances of all 5 substructures suggest that they are of accreted origin, except for two stars that present a high [alpha/Fe] at high [Fe/H] more in line with an in-situ origin. All but ED-2 present a significant spread in [Fe/H], suggestive of a dwarf galaxy origin. ED-3 and ED-4 tend to exhibit lower [alpha/Fe] compared to GE stars. ED-5 and ED-6 are consistent with the GE chemical track and could be high-energy tails of GE that were lost earlier in the accretion process. We present new elemental abundances for 5 ED-2 stars, including more elements for the Gaia BH3 companion star. Our findings are in line with the picture that ED-2 is a disrupted ancient star cluster.2025A&A...700A.154Dhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/700/A154CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toI/355 : Gaia DR3 Part 1. Main source (Gaia Collaboration, 2022)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/700/A154https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/700/A154http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/700/A154https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/700/A154https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/700/A154http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/700/A154GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/700/A154/tablea2 (Stellar parameters for all stars)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/700/A154/tablea2?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/700/A154/tablea2?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/700/A154/tablea2?GETtext/xml+votable180.050000true220.82483335.82769440.0055555555555555566/8235 17315 17408 17788 18127 18483 18494 18855 20680 21518 21955 23209 27019 27162 27948 30166 30684 31447 31826 33067 33306 33957 35234 35619 36919 37969 38245 38297 38986 39917 42911 43740 43878 44515 45012 45351 45718 46591 46771 47125 47208 47934https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/700/A154?format=asciiUVdefaultJ/A+A/700/A154/tablea2Stellar parameters for all starsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintEWDisplay the equivalent widhts in table 1meta.ref.urlcharAbundDisplay the abundances in table 2meta.ref.urlcharGaiaDR3Gaia DR3 source_idmeta.id;meta.mainRAJ2000Simbad right ascension (J2000)pos.eq.ra;meta.mainDEJ2000Simbad declination (J2000)pos.eq.dec;meta.mainSimbadSimbad column added by the CDSmeta.ref.urlcharNameNamemeta.idcharNoteNotemeta.notecharTeff? Effective temperatureKphys.temperature.effectiveintnullablelogg? Surface gravitylog(cm.s**-2)phys.gravityfloatnullableksi? Microturbulent velocitykm/sphys.velocfloatnullable[Fe/H]? Metallicityphys.abund.ZfloatnullableJ/A+A/700/A154/table1Equivalent widthsEW? Equivalent width0.1pmspect.line.eqWidthfloatnullableab1DLTE1D LTE abundancephys.abundfloatab1DNLTE? 1D NLTE abundancephys.abundfloatnullablerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintGaiaDR3Gaia DR3 source_idmeta.id;meta.mainSpeciesName of of speciesphys.atmol.elementcharlambdaWavelength0.1nmem.wlfloatchi? Excitation potentialphys.atmol.excitationfloatnullableloggf? Oscillator strength valuephys.atmol.oscStrengthfloatnullableJ/A+A/700/A154/table2AbundancesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintGaiaDR3Gaia DR3 source_idmeta.id;meta.mainSpeciesName of of speciesphys.atmol.elementcharNlinesNumber of linesmeta.numberint[X/H]X abundance relative to Hphys.abund.X;arith.ratiofloate_[X/H]Uncertainty in X abundance relative to Hstat.error;phys.abundfloat[X/Fe]X abundance relative to Fephys.abund.Xfloate_[X/Fe]Uncertainty in X abundance relative to Festat.error;phys.abundfloat