J/A+A/710/A381ivo://CDS.VizieR/J/A+A/710/A381CDSDonada J.Casamiquela L.Anders F.Balaguer-Nunez L.Blanco-Cuaresma S.,Luri X.Slumstrup D.Jordi C.Castro-Ginard A.Carrera R.Carrasco J.M.2026-06-29T15:07:29Z2026-06-29T16:05:46ZCDS support team

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

cds-question@unistra.fropen-star-clustersspectroscopyradial-velocitychemical-abundancesOf the thousands of newly discovered open clusters (OCs) thanks to the exquisite precision of the Gaia mission data, only a small fraction has been observed with high-resolution spectroscopy. Particularly, the population of OCs in the inner disc at relatively high altitudes (Z) from the Galactic plane remains poorly studied. Few such high-|Z| inner-disc OCs have been detected, and most are sparse groupings of stars that still await confirmation as real OCs. We performed a detailed spectroscopic analysis of the high-|Z| inner-disc OC UBC 1052, an old cluster located at a cylindrical Galactocentric radius Rgc=6.1kpc, where it is one of a few OCs situated at a considerable altitude (Z=340pc). We used FLAMES/VLT to acquire high signal-to-noise ratio (S/N) UVES spectra of four red clump (RC) members (G~14 mag), from which we derived high-precision radial velocities and local thermodynamic equilibrium chemical abundances for 23 elements. A strict line-by-line differential analysis was carried out using a reference RC star and a solar analogue in the OC M 67, allowing us to derive very precise abundances for each star (a median precision in [X/H] of ~0.06dex). We also acquired GIRAFFE spectra for other candidate member stars and derived their radial velocities. We determine that UBC 1052 has an age of 2.25+/-0.25Gyr, a distance of 3.11+/-0.07kpc, an extinction of A_V_=1.23mag, and a mean radial velocity of 34.0+/-0.6km/s. We find that the four RC stars have fully compatible chemical abundances, thus confirming UBC 1052 as a real OC. It has [Fe/H]=+0.05+/-0.01dex, and with [X/H] dispersions among the four stars <0.03dex for 20 elements, we give conservative limits for chemical inhomogeneities at ~0.05dex for these species. UBC 1052 stands out as the oldest and highest-|Z| inner-disc OC studied at high resolution to date, being located in the poorly sampled inner Galactic region where old OCs and OCs with large maximum excursions from the plane are scarce. Its relatively low [Fe/H] at its Rgc suggests it is a rare candidate for an inward-migrated OC in the inner disc. Its detailed abundance pattern (e.g. [Ba/Zr] and [Nd/Y]) shows some interesting features that appear to be unique in the current census of OCs studied at high resolution, making it an interesting object for potential strong chemical-tagging searches for already dispersed member stars.2026A&A...710A.381Dhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/710/A381CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/661/A118 : 628 new open clusters found with OCfinderJ/A+A/673/A114 : Improving the open cluster census. II. (Hunt+, 2023)J/A+A/645/A106 : Atomic data for the Gaia-ESO Survey (Heiter+, 2021)J/A+A/652/A25 : Abundance-age relations with open clustersJ/A+A/566/A98 : The Gaia Benchmark Stars Library (Blanco-Cuaresma+, 2014)J/A+A/687/A239 : Open clusters abundances (Carbajo-Hijarrubia+, 2024)J/A+A/640/A1 : Portrait Galactic disc (Cantat-Gaudin+, 2020)J/AJ/167/12 : Open cluster parameters with ANN (Cavallo+, 2024)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/710/A381https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/710/A381http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/710/A381https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/710/A381https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/710/A381http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/710/A381GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/710/A381/tablea2 (Radial velocities, atmospheric parameters and mean elemental abundances for the stars observed with UVES)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/710/A381/tablea2?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/710/A381/tablea2?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/710/A381/tablea2?GETtext/xml+votable180.050000true280.09630947.6526850.005555555555555556Cone search capability for table J/A+A/710/A381/tablef1 (Radial velocities for the stars observed with GIRAFFE)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/710/A381/tablef1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/710/A381/tablef1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/710/A381/tablef1?GETtext/xml+votable180.050000true280.16613147.75069720.0055555555555555566/4298 304591.9867573869263685e-19 3.916500758235022e-19https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/710/A381?format=asciidefaultJ/A+A/710/A381/tablea1Selected absorption lines and their absolute abundances for the stars observed with UVESrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintElementElement symbol (e.g. Fe)phys.atmol.elementcharIon[1/2] Ionisation stage (1)phys.atmol.ionStageintWavePeak[480.06/675.28] Central wavelength of the absorption linenmem.wl.central;spect.linedoubleloggfTransition probability in the form of log(gf) from Heiter et al. (2021A&A...645A.106H, Cat. J/A+A/645/A106) (2)phys.atmol.transProbfloatAX-1? Absolute abundance for UBC 1052 star Gaia DR3 4286764462544613120phys.abundfloatnullableAX-2? Absolute abundance for UBC 1052 star Gaia DR3 4286764703062797952phys.abundfloatnullableAX-3? Absolute abundance for UBC 1052 star Gaia DR3 4286766932128889472phys.abundfloatnullableAX-4? Absolute abundance for UBC 1052 star Gaia DR3 4286776522812820224phys.abundfloatnullableAX-5? Absolute abundance for UBC 1052 star Gaia DR3 4286778137720526080phys.abundfloatnullableAX-6? Absolute abundance for the auxiliary M67 star Gaia DR3 604914949295282816phys.abundfloatnullableJ/A+A/710/A381/tablea2Radial velocities, atmospheric parameters and mean elemental abundances for the stars observed with UVESe_[Zr1/H]Uncertainty in [Zr1/H]log(Sun)stat.error;phys.abundfloatSimbadSimbad column added by the CDSmeta.ref.urlcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintGaiaDR3Gaia DR3 source IDmeta.id;meta.mainRVRadial velocitykm/sphys.veloc;pos.heliocentricfloate_RVUncertainty in radial velocitykm/sstat.errorfloatTeffEffective temperatureKphys.temperature.effectivefloate_TeffUncertainty in effective temperatureKstat.error;phys.temperature.effectivefloatloggLogarithm of surface gravitylog(cm.s**-2)phys.gravityfloate_loggUncertainty in logarithm of surface gravitylog(cm.s**-2)stat.errorfloatvmicMicroturbulent velocitykm/sphys.velocfloate_vmicUncertainty in microturbulent velocitykm/sstat.errorfloato_Na1[4]? Number of Na1 lines used to determine its abundancemeta.numberintnullable[Na1/H]? Abundance [Na1/H] relative to the Sunlog(Sun)phys.abundfloatnullablee_[Na1/H]? Uncertainty in [Na1/H]log(Sun)stat.error;phys.abundfloatnullable[Na1/Fe]? Abundance [Na1/Fe] relative to the Sunlog(Sun)phys.abundfloatnullablee_[Na1/Fe]? Uncertainty in [Na1/Fe]log(Sun)stat.error;phys.abundfloatnullableo_Mg1[4/6] Number of Mg1 lines used to determine its abundancemeta.numberint[Mg1/H]Abundance [Mg1/H] relative to the Sunlog(Sun)phys.abundfloate_[Mg1/H]Uncertainty in [Mg1/H]log(Sun)stat.error;phys.abundfloat[Mg1/Fe]Abundance [Mg1/Fe] relative to the Sunlog(Sun)phys.abundfloate_[Mg1/Fe]Uncertainty in [Mg1/Fe]log(Sun)stat.error;phys.abundfloato_Al1[3] Number of Al1 lines used to determine its abundancemeta.numberint[Al1/H]Abundance [Al1/H] relative to the Sunlog(Sun)phys.abundfloate_[Al1/H]Uncertainty in [Al1/H]log(Sun)stat.error;phys.abundfloat[Al1/Fe]Abundance [Al1/Fe] relative to the Sunlog(Sun)phys.abundfloate_[Al1/Fe]Uncertainty in [Al1/Fe]log(Sun)stat.error;phys.abundfloato_Si1[3/7] Number of Si1 lines used to determine its abundancemeta.numberint[Si1/H]Abundance [Si1/H] relative to the Sunlog(Sun)phys.abundfloate_[Si1/H]Uncertainty in [Si1/H]log(Sun)stat.error;phys.abundfloat[Si1/Fe]Abundance [Si1/Fe] relative to the Sunlog(Sun)phys.abundfloate_[Si1/Fe]Uncertainty in [Si1/Fe]log(Sun)stat.error;phys.abundfloato_Ca1[16/20] Number of Ca1 lines used to determine its abundancemeta.numberint[Ca1/H]Abundance [Ca1/H] relative to the Sunlog(Sun)phys.abundfloate_[Ca1/H]Uncertainty in [Ca1/H]log(Sun)stat.error;phys.abundfloat[Ca1/Fe]Abundance [Ca1/Fe] relative to the Sunlog(Sun)phys.abundfloate_[Ca1/Fe]Uncertainty in [Ca1/Fe]log(Sun)stat.error;phys.abundfloato_Sc2[10] Number of Sc2 lines used to determine its abundancemeta.numberint[Sc2/H]Abundance [Sc2/H] relative to the Sunlog(Sun)phys.abundfloate_[Sc2/H]Uncertainty in [Sc2/H]log(Sun)stat.error;phys.abundfloat[Sc2/Fe]Abundance [Sc2/Fe] relative to the Sunlog(Sun)phys.abundfloate_[Sc2/Fe]Uncertainty in [Sc2/Fe]log(Sun)stat.error;phys.abundfloato_Ti1[6/9] Number of Ti1 lines used to determine its abundancemeta.numberint[Ti1/H]Abundance [Ti1/H] relative to the Sunlog(Sun)phys.abundfloate_[Ti1/H]Uncertainty in [Ti1/H]log(Sun)stat.error;phys.abundfloat[Ti1/Fe]Abundance [Ti1/Fe] relative to the Sunlog(Sun)phys.abundfloate_[Ti1/Fe]Uncertainty in [Ti1/Fe]log(Sun)stat.error;phys.abundfloato_V1[7/17] Number of V1 lines used to determine its abundancemeta.numberint[V1/H]Abundance [V1/H] relative to the Sunlog(Sun)phys.abundfloate_[V1/H]Uncertainty in [V1/H]log(Sun)stat.error;phys.abundfloat[V1/Fe]Abundance [V1/Fe] relative to the Sunlog(Sun)phys.abundfloate_[V1/Fe]Uncertainty in [V1/Fe]log(Sun)stat.error;phys.abundfloato_Cr1[7/12] Number of Cr1 lines used to determine its abundancemeta.numberint[Cr1/H]Abundance [Cr1/H] relative to the Sunlog(Sun)phys.abundfloate_[Cr1/H]Uncertainty in [Cr1/H]log(Sun)stat.error;phys.abundfloat[Cr1/Fe]Abundance [Cr1/Fe] relative to the Sunlog(Sun)phys.abundfloate_[Cr1/Fe]Uncertainty in [Cr1/Fe]log(Sun)stat.error;phys.abundfloato_Mn1[3/6] Number of Mn1 lines used to determine its abundancemeta.numberint[Mn1/H]Abundance [Mn1/H] relative to the Sunlog(Sun)phys.abundfloate_[Mn1/H]Uncertainty in [Mn1/H]log(Sun)stat.error;phys.abundfloat[Mn1/Fe]Abundance [Mn1/Fe] relative to the Sunlog(Sun)phys.abundfloate_[Mn1/Fe]Uncertainty in [Mn1/Fe]log(Sun)stat.error;phys.abundfloato_Fe1[56/106] Number of Fe1 lines used to determine its abundancemeta.numberint[Fe1/H]Abundance [Fe1/H] relative to the Sunlog(Sun)phys.abundfloate_[Fe1/H]Uncertainty in [Fe1/H]log(Sun)stat.error;phys.abundfloato_Co1[8/11] Number of Co1 lines used to determine its abundancemeta.numberint[Co1/H]Abundance [Co1/H] relative to the Sunlog(Sun)phys.abundfloate_[Co1/H]Uncertainty in [Co1/H]log(Sun)stat.error;phys.abundfloat[Co1/Fe]Abundance [Co1/Fe] relative to the Sunlog(Sun)phys.abundfloate_[Co1/Fe]Uncertainty in [Co1/Fe]log(Sun)stat.error;phys.abundfloato_Ni1[10/25] Number of Ni1 lines used to determine its abundancemeta.numberint[Ni1/H]Abundance [Ni1/H] relative to the Sunlog(Sun)phys.abundfloate_[Ni1/H]Uncertainty in [Ni1/H]log(Sun)stat.error;phys.abundfloat[Ni1/Fe]Abundance [Ni1/Fe] relative to the Sunlog(Sun)phys.abundfloate_[Ni1/Fe]Uncertainty in [Ni1/Fe]log(Sun)stat.error;phys.abundfloato_Cu1[1/2] Number of Cu1 lines used to determine its abundancemeta.numberint[Cu1/H]Abundance [Cu1/H] relative to the Sunlog(Sun)phys.abundfloate_[Cu1/H]Uncertainty in [Cu1/H]log(Sun)stat.error;phys.abundfloat[Cu1/Fe]Abundance [Cu1/Fe] relative to the Sunlog(Sun)phys.abundfloate_[Cu1/Fe]Uncertainty in [Cu1/Fe]log(Sun)stat.error;phys.abundfloato_Zn1[1] Number of Zn1 lines used to determine its abundancemeta.numberint[Zn1/H]Abundance [Zn1/H] relative to the Sunlog(Sun)phys.abundfloate_[Zn1/H]Uncertainty in [Zn1/H]log(Sun)stat.error;phys.abundfloat[Zn1/Fe]Abundance [Zn1/Fe] relative to the Sunlog(Sun)phys.abundfloate_[Zn1/Fe]Uncertainty in [Zn1/Fe]log(Sun)stat.error;phys.abundfloato_Sr1[1] Number of Sr1 lines used to determine its abundancemeta.numberint[Sr1/H]Abundance [Sr1/H] relative to the Sunlog(Sun)phys.abundfloate_[Sr1/H]Uncertainty in [Sr1/H]log(Sun)stat.error;phys.abundfloat[Sr1/Fe]Abundance [Sr1/Fe] relative to the Sunlog(Sun)phys.abundfloate_[Sr1/Fe]Uncertainty in [Sr1/Fe]log(Sun)stat.error;phys.abundfloato_Y2[1/3]? Number of Y2 lines used to determine its abundancemeta.numberintnullable[Y2/H]? Abundance [Y2/H] relative to the Sunlog(Sun)phys.abundfloatnullablee_[Y2/H]? Uncertainty in [Y2/H]log(Sun)stat.error;phys.abundfloatnullable[Y2/Fe]? Abundance [Y2/Fe] relative to the Sunlog(Sun)phys.abundfloatnullablee_[Y2/Fe]? Uncertainty in [Y2/Fe]log(Sun)stat.error;phys.abundfloatnullableo_Zr1[1/2] Number of Zr1 lines used to determine its abundancemeta.numberint[Zr1/H]Abundance [Zr1/H] relative to the Sunlog(Sun)phys.abundfloat[Zr1/Fe]Abundance [Zr1/Fe] relative to the Sunlog(Sun)phys.abundfloate_[Zr1/Fe]Uncertainty in [Zr1/Fe]log(Sun)stat.error;phys.abundfloato_Ba2[1/2] Number of Ba2 lines used to determine its abundancemeta.numberint[Ba2/H]Abundance [Ba2/H] relative to the Sunlog(Sun)phys.abundfloate_[Ba2/H]Uncertainty in [Ba2/H]log(Sun)stat.error;phys.abundfloat[Ba2/Fe]Abundance [Ba2/Fe] relative to the Sunlog(Sun)phys.abundfloate_[Ba2/Fe]Uncertainty in [Ba2/Fe]log(Sun)stat.error;phys.abundfloato_Ce2[1]? Number of Ce2 lines used to determine its abundancemeta.numberintnullable[Ce2/H]? Abundance [Ce2/H] relative to the Sunlog(Sun)phys.abundfloatnullablee_[Ce2/H]? Uncertainty in [Ce2/H]log(Sun)stat.error;phys.abundfloatnullable[Ce2/Fe]? Abundance [Ce2/Fe] relative to the Sunlog(Sun)phys.abundfloatnullablee_[Ce2/Fe]? Uncertainty in [Ce2/Fe]log(Sun)stat.error;phys.abundfloatnullableo_Pr2[1]? Number of Pr2 lines used to determine its abundancemeta.numberintnullable[Pr2/H]? Abundance [Pr2/H] relative to the Sunlog(Sun)phys.abundfloatnullablee_[Pr2/H]? Uncertainty in [Pr2/H]log(Sun)stat.error;phys.abundfloatnullable[Pr2/Fe]? Abundance [Pr2/Fe] relative to the Sunlog(Sun)phys.abundfloatnullablee_[Pr2/Fe]? Uncertainty in [Pr2/Fe]log(Sun)stat.error;phys.abundfloatnullableo_Nd2[1/2]? Number of Nd2 lines used to determine its abundancemeta.numberintnullable[Nd2/H]? Abundance [Nd2/H] relative to the Sunlog(Sun)phys.abundfloatnullablee_[Nd2/H]? Uncertainty in [Nd2/H]log(Sun)stat.error;phys.abundfloatnullable[Nd2/Fe]? Abundance [Nd2/Fe] relative to the Sunlog(Sun)phys.abundfloatnullablee_[Nd2/Fe]? Uncertainty in [Nd2/Fe]log(Sun)stat.error;phys.abundfloatnullableo_Eu2[1] Number of Eu2 lines used to determine its abundancemeta.numberint[Eu2/H]Abundance [Eu2/H] relative to the Sunlog(Sun)phys.abundfloate_[Eu2/H]Uncertainty in [Eu2/H]log(Sun)stat.error;phys.abundfloat[Eu2/Fe]Abundance [Eu2/Fe] relative to the Sunlog(Sun)phys.abundfloate_[Eu2/Fe]Uncertainty in [Eu2/Fe]log(Sun)stat.error;phys.abundfloat_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/710/A381/tablea3UBC 1052 mean cluster abundances from UVES spectraElementElement symbol (e.g. Fe)phys.atmol.elementcharIon[1/2] Ionisation stage (1)phys.atmol.ionStageint[X/H]UBC 1052 mean cluster [X/H] abundance relative to the Sunlog(Sun)phys.abund;stat.meanfloate_[X/H]Uncertainty in [X/H]log(Sun)stat.error;phys.abundfloat[X/Fe]? UBC 1052 mean cluster [X/Fe] abundance relative to the Sunlog(Sun)phys.abundfloatnullablerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordinte_[X/Fe]? Uncertainty in [X/Fe]log(Sun)stat.error;phys.abundfloatnullableNlinestotal[1/78] Total number of different lines used for this element (2)meta.numberintJ/A+A/710/A381/tablef1Radial velocities for the stars observed with GIRAFFErecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintGaiaDR3Gaia DR3 source IDmeta.id;meta.maininCG22Is star a member of UBC 1052 in Castro-Ginard et al. 2022 (2022A&A...661A.118C, Cat. J/A+A/661/A118)meta.codecharinHR23Is star a member of UBC 1052 in Hunt & Reffert (2023A&A...673A.114H, Cat. J/A+A/673/A114)meta.codecharGmagMean G-band magnitude from Gaia DR3magphot.mag;em.optfloatBP-RPBP-RP colour from Gaia DR3magphot.color;em.opt.B;em.opt.RfloatS/NSignal-to-noise ratio of the merged spectrum (three gratings joined)stat.snrintRV? Radial velocitykm/sphys.veloc;pos.heliocentricfloatnullablee_RV? Uncertainty in radial velocitykm/sstat.errorfloatnullabledispOCmRV? RV discrepancy with respect to UBC 1052's mean RV (1)phys.veloc;arith.difffloatnullable_RAPositions from Gaia DR3 (right ascension part)degpos.eq.ra;meta.main_DEPositions from Gaia DR3 (declination part)degpos.eq.dec;meta.main