J/AJ/162/42ivo://CDS.VizieR/J/AJ/162/42doi:10.26093/cds/vizier.51620042CDSWoody T.Schlaufman K.C.2022-03-21T12:01:52Z2021-11-29T09:10:49ZCDS support team

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

cds-question@unistra.frglobular-star-clustersmilky-way-galaxyvisible-astronomytrigonometric-parallaxproper-motionsradial-velocitymetallicityGlobular clusters can form inside their host galaxies at high redshift when gas densities are higher and gas-rich mergers are common. They can also form inside lower-mass galaxies that have since been accreted and tidally disrupted, leaving their globular cluster complement bound to higher-mass halos. We argue that the age-metallicity-specific orbital energy relation in a galaxy's globular cluster system can be used to identify its origin. Gas-rich mergers should produce tightly bound systems in which metal-rich clusters are younger than metal-poor clusters. Globular clusters formed in massive disks and then scattered into a halo should have no relationship between age and specific orbital energy. Accreted globular clusters should produce weakly bound systems in which age and metallicity are correlated with eachother but inversely correlated with specific orbital energy. We use precise relative ages, self-consistent metallicities, and space-based proper motion-informed orbits to show that the Milky Way's metal-poor globular cluster system lies in a plane in age-metallicity-specific orbital energy space. We find that relatively young or metal-poor globular clusters are weakly bound to the Milky Way, while relatively old or metal-rich globular clusters are tightly bound to the Galaxy. While metal-rich globular clusters may be formed either in situ or ex situ, our results suggest that metal-poor clusters are formed outside of the Milky Way in now-disrupted dwarf galaxies. We predict that this relationship between age, metallicity, and specific orbital energy in a L* galaxy's globular cluster system is a natural outcome of galaxy formation in a {Lambda}CDM universe.2021AJ....162...42Whttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/AJ/162/42CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toVII/195 : Globular Clusters in the Milky Way (Harris, 1996)VII/202 : Globular Clusters in the Milky Way (Harris, 1997)I/337 : Gaia DR1 (Gaia Collaboration, 2016)I/345 : Gaia DR2 (Gaia Collaboration, 2018)J/A+AS/121/95 : Giant stars abundances in 24 clusters (Carretta+ 1997)J/PASP/109/883 : Globular metallicity scale. I. (Rutledge+ 1997)J/AJ/118/1671 : Fornax cluster 4 VI photometry (Buonanno+, 1999)J/A+AS/141/371 : Low-mass stars evoluti. tracks & isochrones (Girardi+, 2000)J/AJ/127/1545 : Abundance ratios of 4 stars in Pal 12 (Cohen+, 2004)J/A+A/465/815 : Abundances of Sgr dSph stars (Sbordone+, 2007)J/AJ/136/614 : Arp 2 and Ter 8 red giants equivalent widths (Mottini+, 2008)J/A+A/520/A95 : Abundances of red giants in M54 and Sgr dSph (Carretta+, 2010)J/ApJ/670/346 : Mgiant stars in the Sagittarius dwarf galaxy. V. (Chou+, 2007)J/ApJ/779/102 : Metallicities of RGB stars in dwarf galaxies (Kirby+, 2013)J/A+A/561/A87 : FLAMES observations of Terzan 8 (Carretta+, 2014)J/A+A/616/A12 : Gaia DR2 sources in GC and dSph (Gaia Collaboration+, 2018)J/MNRAS/482/5138 : Galactic GC mean pm & velocities (Baumgardt+, 2019)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/AJ/162/42https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/AJ/162/42http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/AJ/162/42https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/AJ/162/42https://vizier.iucaa.in/viz-bin/votable?-source=J/AJ/162/42http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/AJ/162/42GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/AJ/162/42/table1 (Input astrometric, distance, and radial velocity data)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/AJ/162/42/table1?https://vizier.iucaa.in/viz-bin/conesearch/J/AJ/162/42/table1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/AJ/162/42/table1?GETtext/xml+votable180.050000true6.0194-72.08210.0055555555555555566/9436 9666 10321 10336 12405 12425 12943 14489 16647 19091 24843 27981 27986 28067 28705 28741 28973 29184 30378 30769 30998 31019 31115 31417 33321 33330 33635 34242 37294 38465 39642 41257 41304 41522 41852 42076 42278 42314 42320 42700 42955 42958 42990 43125 43227 47125 47620 47777 47825 47868 47903 47916 47935 47971 48434 48444 48952https://cdsarc.cds.unistra.fr/viz-bin/moc/J/AJ/162/42?format=asciiOpticaldefaultJ/AJ/162/42/table1Input astrometric, distance, and radial velocity dataplx[0.006/0.51]? Parallax (1)maspos.parallax.trigfloatnullableNGCNGC identifiermeta.id;meta.maincharprimaryrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameCommon namemeta.idcharRAJ2000[6/327] Right Ascension (J2000) (1)degpos.eq.ra;meta.mainDEJ2000[-73/44] Declination (J2000) (1)degpos.eq.dec;meta.mainpmRA[-13/10] Proper motion along RA (1)mas/yrpos.pm;pos.eq.radoublee_pmRA[0.001/0.08] Uncertainty in pmRA (1)mas/yrstat.error;pos.pm;pos.eq.rafloatpmDE[-19/2] Proper motion along DE (1)mas/yrpos.pm;pos.eq.decdoublee_pmDE[0.001/0.06] Uncertainty in pmDE (1)mas/yrstat.error;pos.pm;pos.eq.decfloate_plx[0.0002/0.007]? Uncertainty in plx (1)masstat.error;pos.parallaxfloatnullablesigma1[-0.32/0.3]? Covariance between pmRA & pmDEstat.covariancefloatnullablesigma2[-0.38/0.15]? Covariance between pmRA & plxstat.covariancefloatnullablesigma3[-0.27/0.18]? Covariance between pmDE & plxstat.covariancefloatnullableDist[2.2/27.6] Distance (2)kpcpos.distance;src.orbitalfloatE_Dist[0.1/0.6] Upper uncertainty in D (2)kpcstat.error;stat.maxfloate_Dist[0.1/0.6] Lower uncertainty in D (2)kpcstat.errorfloatRVel[-412/494] Radial velocity (2)km/sphys.veloc;pos.heliocentricfloate_RVel[0.1/15] Uncertainty in RVel (2)km/sstat.error;spect.dopplerVelocfloatt2Display data from table2meta.ref.urlcharSimbadSimbad column added by the CDSmeta.ref.urlcharJ/AJ/162/42/table2Age, metallicity, and specific orbital energy inferencesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNGCNGC identifiermeta.id;meta.maincharNameCommon namemeta.idcharAge[0.57/1.09] Normalized age (1)time.age;arith.ratiofloate_Age[0.02/0.2] Uncertainty in taustat.error;time.agefloat[M/H][-1.98/-0.42] Metallicity (2)log(Sun)phys.abund.Zfloate_[M/H][0.05] Uncertainty in [M/H]log(Sun)stat.error;phys.abundfloatSOE[-11.4/-3.1] MWPotential2014 specific orbital energylog(10000km**2.s**-2)src.orbitalfloatE_SOE[0.02/0.9] Upper uncertainty in SOElog(10000km**2.s**-2)stat.error;stat.maxfloate_SOE[0.01/0.8] Lower uncertainty in SOElog(10000km**2.s**-2)stat.errorfloatSOEscl[-16.2/-7.21] Scaled MWPotential2014 specific orbital energy (3)log(10000km**2.s**-2)src.orbitalfloatE_SOEscl[0.02/0.97] Upper uncertainty in SOEscllog(10000km**2.s**-2)stat.error;stat.maxfloate_SOEscl[0.01/0.73] Lower uncertainty in SOEscllog(10000km**2.s**-2)stat.errorfloatSOEMc17[-24.6/-8.3] Mc17 specific orbital energy (4)log(10000km**2.s**-2)src.orbitalfloatE_SOEMc17[0.04/0.92] Upper uncertainty in SOMc17log(10000km**2.s**-2)stat.error;stat.maxfloate_SOEMc17[0.04/0.91] Lower uncertainty in SOMc17log(10000km**2.s**-2)stat.errorfloat