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arXiv:astro-ph/9610181 (astro-ph)
[Submitted on 23 Oct 1996]

Title:Substructure in the Globular Cluster System of the Milky Way

Authors:A. Burkert (MPIA), G. Smith (UCSC)
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Abstract: The kinematical and spatial properties of the metal-rich globular clusters in the Galaxy ([Fe/H] > -0.8) indicates that these objects do not comprise a homogeneous population. Three subsystems are identified. The highest-mass clusters exhibit a very slow net rotation with a speed of v_rot = 24 km/s and v_rot/sigma = 0.3, indicative of a centrally condensed, spheroidal subsystem. Roughly half of the lower-mass clusters appear to be located in an elongated bar-like structure which passes through the Galactic Center, and has similar properties to the central stellar bar of the Milky Way. The remaining lower-mass clusters exhibit very rapid net rotation, with a rotation speed of v_rot = 164 km/s and v_rot/sigma = 6. These clusters are located in the Galactic plane, within a ring of 4 to 6 kpc radial distance from the Galactic Center. The highest-mass clusters may have formed during relatively advanced stages of the dissipative evolution of the inner Galactic halo. The lower-mass bar clusters may be associated with the formation of the Galactic stellar bar or bulge. The lower-mass ring clusters appear to be real disk objects. They may represent a stage in cluster formation that was intermediate between that of the halo globular clusters and the oldest extant open clusters.
Comments: 15 pages LaTeX, 2 postscript figures. To appear in ApJ (Letters). See also this http URL
Subjects: Astrophysics (astro-ph)
Cite as: arXiv:astro-ph/9610181
  (or arXiv:astro-ph/9610181v1 for this version)
  https://doi.org/10.48550/arXiv.astro-ph/9610181

Submission history

From: Andreas Burkert [view email]
[v1] Wed, 23 Oct 1996 11:51:16 UTC (39 KB)
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