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The Metallicity Distribution of the Milky Way Bulge
Ness, M.; Freeman, K.
AA(Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany), AB(Research School of Astronomy and Astrophysics, Australian National University, Cotter Rd., Weston, ACT 2611, Australia)
Publications of the Astronomical Society of Australia, Volume 33, id.e022 8 pp. (PASA Homepage)
Publication Date:
Astronomy Keywords:
galaxy: bulge, galaxy: evolution, galaxy: formation, galaxy: fundamental parameters, galaxy: center
Abstract Copyright:
2016: Astronomical Society of Australia
Bibliographic Code:


The Galactic bulge of the Milky Way is made up of stars with a broad range of metallicity, -3.0 < [Fe/H] < 1 dex. The mean of the metallicity distribution function decreases as a function of height z from the plane and, more weakly, with galactic radius R GC. The most metal-rich stars in the inner Galaxy are concentrated to the plane and the more metal-poor stars are found predominantly further from the plane, with an overall vertical gradient in the mean of the metallicity distribution function of about - 0.45 dex kpc-1. This vertical gradient is believed to reflect the changing contribution with height of different populations in the innermost region of the Galaxy. The more metal-rich stars of the bulge are part of the boxy/peanut structure and comprise stars in orbits which trace out the underlying X-shape. There is still a lack of consensus on the origin of the metal-poor stars ([Fe/H] < -0.5) in the region of the bulge. Some studies attribute the more metal-poor stars of the bulge to the thick disk and stellar halo that are present in the inner region, and other studies propose that the metal-poor stars are a distinct `old spheroid' bulge population. Understanding the origin of the populations that make up the metallicity distribution function of the bulge, and identifying if there is a unique bulge population which has formed separately from the disk and halo, has important consequences for identifying the relevant processes in the formation and evolution of the Milky Way.
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