Triangulum–Andromeda overdensity
E539432
The Triangulum–Andromeda overdensity is a large, diffuse stellar structure in the outer regions of the Milky Way, thought to be the remnant of a disrupted dwarf galaxy or tidal stream.
Statements (40)
| Predicate | Object |
|---|---|
| instanceOf |
Galactic halo substructure
ⓘ
stellar overdensity ⓘ stellar structure ⓘ tidal debris candidate ⓘ |
| belongsTo | outer Galactic halo substructures ⓘ |
| composedOf |
metal-poor stars
ⓘ
old stars ⓘ |
| discoveredUsing | Sloan Digital Sky Survey NERFINISHED ⓘ |
| extendsAcrossConstellation |
Andromeda
NERFINISHED
ⓘ
Pisces NERFINISHED ⓘ Triangulum NERFINISHED ⓘ |
| hasAlternativeName |
TriAnd
NERFINISHED
ⓘ
TriAnd overdensity NERFINISHED ⓘ |
| hasAngularExtent | tens of degrees on the sky ⓘ |
| hasApproximateDistanceFromSun | 20–30 kiloparsecs ⓘ |
| hasEstimatedAge | several billion years ⓘ |
| hasKinematics |
distinct from Galactic disk
ⓘ
halo-like velocities ⓘ |
| hasMetallicity | low metallicity ⓘ |
| hasMorphology | large diffuse structure ⓘ |
| hasObservationMethod |
photometric surveys
ⓘ
spectroscopic follow-up ⓘ |
| hasScientificInterest | traces past accretion events ⓘ |
| hasShape | irregular ⓘ |
| hasStellarPopulation |
main-sequence turnoff stars
ⓘ
red giant branch stars ⓘ |
| hasTypeOfStructure | low-surface-brightness feature ⓘ |
| hasUncertainOrigin | true ⓘ |
| identifiedBy | star count overdensities ⓘ |
| isCandidateRemnantOf |
disrupted dwarf galaxy
ⓘ
tidal stream ⓘ |
| isDifferentFrom |
Monoceros Ring
NERFINISHED
ⓘ
Sagittarius tidal stream NERFINISHED ⓘ |
| isEvidenceFor |
accretion of dwarf galaxies by the Milky Way
ⓘ
hierarchical formation of the Milky Way ⓘ |
| isPartOf | large-scale substructure in the Milky Way halo ⓘ |
| locatedIn |
Galactic halo
NERFINISHED
ⓘ
outer regions of the Milky Way ⓘ |
| partOf | Milky Way NERFINISHED ⓘ |
| studiedInWavelength | optical ⓘ |
Referenced by (1)
Full triples — surface form annotated when it differs from this entity's canonical label.