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    Kinematics and stellar populations of the galactic bulge.

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    Author
    Minniti, Dante.
    Issue Date
    1993
    Keywords
    Dissertations, Academic.
    Astrophysics.
    Committee Chair
    Olszewski, Edward W.
    Liebert, James W.
    
    Metadata
    Show full item record
    Publisher
    The University of Arizona.
    Rights
    Copyright © is held by the author. Digital access to this material is made possible by the University Libraries, University of Arizona. Further transmission, reproduction or presentation (such as public display or performance) of protected items is prohibited except with permission of the author.
    Abstract
    In order to measure radial and/or rotation velocities and obtain metallicities for the stellar population of the Galactic bulge, several hundred spectra of giants have been obtained. These include three bulge fields at projected distances from the Galactic center of 1.5, 1.7 and 1.7 kpc, and 33 globular and open clusters. We measure metallicities based on a calibration from stars belonging to the field and to clusters of known abundances. There is a clear dependence of the kinematics on metallicity in all the fields studied, in the sense that the more metal poor stars have lower rotation and higher velocity dispersion than the more metal rich stars. In particular, we identify the giants having [Fe/H] ≤ 1.0 with an extension of the halo population to the innermost regions of the Galaxy rather than with the bulge itself. Near-IR photometry of 21 globulars clusters and bulge fields within 3 kpc of the Galactic center has also been obtained. We find a metallicity gradient with radial distance from the center, consistent with previous results obtained from optical photometry. We argue that the majority of the metal rich globulars within 3 kpc of the center are associated with the bulge population. We also argue that the RR Lyraes previously studied in bulge fields are associated with the inner halo, and that the bulge is younger than the halo. Other kinematic tracers are examined (M giants, RR Lyraes, Miras, OH/IR stars, planetary nebulae) to associate them with different Galactic components. We conclude that all the existing evidence shows that dissipation played an important role in the formation of the bulge.
    Type
    text
    Dissertation-Reproduction (electronic)
    Degree Name
    Ph.D.
    Degree Level
    doctoral
    Degree Program
    Astronomy
    Graduate College
    Degree Grantor
    University of Arizona
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