Metal-rich globular clusters with R≤3 KPC: Disk or bulge clusters?

Resultado de la investigación: Article

127 Citas (Scopus)

Resumen

We compare the metal-rich globular clusters within 3 kpc of the galactic center with the underlying stellar population. On the basis of kinematics, spatial distribution, and metallicity, we argue that these clusters may be associated with the galactic bulge (as concluded by Frenk & White 1982) rather than with the thick disk. On the basis of the available ages for some of these clusters, it is argued that the galactic bulge formed after the halo. Different formation scenarios of the galaxy are examined, and it is concluded that dissipation played a major role in the inner 3 kpc.

Idioma originalEnglish
Páginas (desde-hasta)1663-1669
Número de páginas7
PublicaciónAstronomical Journal
Volumen109
N.º4
EstadoPublished - abr 1995

Huella dactilar

galactic bulge
globular clusters
dissipation
kinematics
spatial distribution
metal
metals
metallicity
halos
galaxies

ASJC Scopus subject areas

  • Space and Planetary Science
  • Astronomy and Astrophysics

Citar esto

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title = "Metal-rich globular clusters with R≤3 KPC: Disk or bulge clusters?",
abstract = "We compare the metal-rich globular clusters within 3 kpc of the galactic center with the underlying stellar population. On the basis of kinematics, spatial distribution, and metallicity, we argue that these clusters may be associated with the galactic bulge (as concluded by Frenk & White 1982) rather than with the thick disk. On the basis of the available ages for some of these clusters, it is argued that the galactic bulge formed after the halo. Different formation scenarios of the galaxy are examined, and it is concluded that dissipation played a major role in the inner 3 kpc.",
author = "Dante Minniti",
year = "1995",
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language = "English",
volume = "109",
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Metal-rich globular clusters with R≤3 KPC : Disk or bulge clusters? / Minniti, Dante.

En: Astronomical Journal, Vol. 109, N.º 4, 04.1995, p. 1663-1669.

Resultado de la investigación: Article

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N2 - We compare the metal-rich globular clusters within 3 kpc of the galactic center with the underlying stellar population. On the basis of kinematics, spatial distribution, and metallicity, we argue that these clusters may be associated with the galactic bulge (as concluded by Frenk & White 1982) rather than with the thick disk. On the basis of the available ages for some of these clusters, it is argued that the galactic bulge formed after the halo. Different formation scenarios of the galaxy are examined, and it is concluded that dissipation played a major role in the inner 3 kpc.

AB - We compare the metal-rich globular clusters within 3 kpc of the galactic center with the underlying stellar population. On the basis of kinematics, spatial distribution, and metallicity, we argue that these clusters may be associated with the galactic bulge (as concluded by Frenk & White 1982) rather than with the thick disk. On the basis of the available ages for some of these clusters, it is argued that the galactic bulge formed after the halo. Different formation scenarios of the galaxy are examined, and it is concluded that dissipation played a major role in the inner 3 kpc.

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