Subjects: Astronomy >> Astrophysical processes submitted time 2023-02-19
Abstract： We combine the kinematics of 159 globular clusters (GCs) provided by the Gaia
Early Data Release 3 (EDR3) with other observational data to classify the GCs,
and to estimate the mass of the Milky Way (MW). We use the age-metallicity
relation, integrals of motion, action space and the GC orbits to identify the
GCs as either formed in-situ (Bulge and Disk) or ex situ (via accretion). We
find that $45.3\%$ have formed in situ, $38.4\%$ may be related to known merger
events: Gaia-Sausage-Enceladus, the Sagittarius dwarf galaxy, the Helmi
streams, the Sequoia galaxy, and the Kraken galaxy. We also further identify
three new sub-structures associated with the Gaia-Sausage-Enceladus. The
remaining $16.3\%$ of GCs are unrelated to the known mergers and thought to be
from small accretion events. We select 46 GCs which have radii $8.0
Peer Review Status:
Awaiting Review
Subjects: Astronomy >> Astrophysical processes submitted time 2023-02-19
Abstract： We combine the kinematics of 159 globular clusters (GCs) provided by the Gaia
Early Data Release 3 (EDR3) with other observational data to classify the GCs,
and to estimate the mass of the Milky Way (MW). We use the age-metallicity
relation, integrals of motion, action space and the GC orbits to identify the
GCs as either formed in-situ (Bulge and Disk) or ex situ (via accretion). We
find that $45.3\%$ have formed in situ, $38.4\%$ may be related to known merger
events: Gaia-Sausage-Enceladus, the Sagittarius dwarf galaxy, the Helmi
streams, the Sequoia galaxy, and the Kraken galaxy. We also further identify
three new sub-structures associated with the Gaia-Sausage-Enceladus. The
remaining $16.3\%$ of GCs are unrelated to the known mergers and thought to be
from small accretion events. We select 46 GCs which have radii $8.0
Peer Review Status:Awaiting Review
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