1993
DOI: 10.1086/133267
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The Galactic bulge and halo

Abstract: The relationship between the galactic halo and bulge is discussed, with reference to early results from a survey for K giants in a field 2 kpc from the galactic center, and Zinn's ( 1992) data on globular-cluster kinematics. The data are currently too meager to decide whether the inner halo shades gradually into the bulge, although there are some interesting kinematical similarities between bulge stars and Zinn's Old Halo clusters in the inner Galaxy. Useful observations that would help decide this matter are … Show more

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Cited by 16 publications
(14 citation statements)
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References 27 publications
(43 reference statements)
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“…Whereas latetype giants which lie up to large distances relative to the Sun or up to large z-heights from the galactic plane have multi-modal metallicity distribution. However, the weighted mean metal-abundances of late-type giants in our sample is < [Fe/H] >= −0.7 dex, rather close to the one claimed by Morrison & Harding (1993), i.e. −0.8 dex, who investigated only the K giants in two square degree field almost symmetric to ours relative to the galactic plane (l = 350…”
Section: Resultssupporting
confidence: 89%
“…Whereas latetype giants which lie up to large distances relative to the Sun or up to large z-heights from the galactic plane have multi-modal metallicity distribution. However, the weighted mean metal-abundances of late-type giants in our sample is < [Fe/H] >= −0.7 dex, rather close to the one claimed by Morrison & Harding (1993), i.e. −0.8 dex, who investigated only the K giants in two square degree field almost symmetric to ours relative to the galactic plane (l = 350…”
Section: Resultssupporting
confidence: 89%
“…The existence of different classes of globular clusters in connection with both spatial extent, metal content, systematic rotation, and velocity dispersion, gives additional support to the idea of a monolithic collapse process, followed by accretion via the disruption of satellite systems (see e.g., Da Costa and Armandroff 1995). The existence of different classes of bulge populations (Morrison and Harding 1993) may lead to the same conclusion.…”
Section: The Abundance Distribution Among G Dwarfs In Geneml Is Appromentioning
confidence: 68%
“…The Galactic bulge extends over a region of galactic longitude l ≃±15° and galactic latitude b ≃±10°; dimensions ∼2 kpc toward and ∼1.5 kpc perpendicular the Galactic plane, respectively (Weiland et al 1993). In total, the bulge contains about 10 11 stars of Population II as well as gas (∼10 6 M ⊙ ) and dust; mass ∼100 times less than the mass of the gas (Morison & Harding 1993). It is generally accepted that a large number of PNe exist in the Galactic bulge, but because of the excessive interstellar extinction, only a small number of them (less than 500) have been discovered (Köppen & Vergely 1998; Parker et al 2001b).…”
Section: Introductionmentioning
confidence: 99%