Metal-rich globular clusters with R less than or equal 3 kpc: Disk or bulge clusters

Details Metal-rich globular clusters with R less than or equal 3 kpc: Disk or bulge clusters Metal-rich globular clusters with R less than or equal 3 kpc: Disk or bulge clusters

Apr 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995aj....109.1663m&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 109, no. 4, p. 1663-1669

Astronomy and Astrophysics

Astronomy

130

Disk Galaxies, Galactic Bulge, Galactic Evolution, Galactic Halos, Globular Clusters, Metallicity, Milky Way Galaxy, Galactic Structure, Kinematics, Star Distribution

Scientific paper

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 glactic bulge formed after the halo. Different formation senarios of the galaxy are examined, and it is concluded that dissapation played a major role in the inner 3 kpc.

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