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Evidence for a metal-poor population in the inner Galactic Bulge

Authors
  • Schultheis, M.
  • Cunha, K.
  • Zasowski, G.
  • Pérez, A. E. García
  • Sellgren, K.
  • Smith, V.
  • García-Hernández, D. A.
  • Zamora, O.
  • Fritz, T. K.
  • Anders, F.
  • Prieto, C. Allende
  • Bizyaev, D.
  • Kinemuchi, K.
  • Pan, K.
  • Malanushenko, E.
  • Malanushenko, V.
  • Shetrone, M. D.
Type
Published Article
Publication Date
Sep 23, 2015
Submission Date
Sep 23, 2015
Identifiers
DOI: 10.1051/0004-6361/201527027
Source
arXiv
License
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External links

Abstract

The inner Galactic Bulge has, until recently, been avoided in chemical evolution studies due to extreme extinction and stellar crowding. Large, near-IR spectroscopic surveys, such as APOGEE, allow for the first time the measurement of metallicities in the inner region of our Galaxy. We study metallicities of 33 K/M giants situated in the Galactic Center region from observations obtained with the APOGEE survey. We selected K/M giants with reliable stellar parameters from the APOGEE/ASPCAP pipeline. Distances, interstellar extinction values, and radial velocities were checked to confirm that these stars are indeed situated in the inner Galactic Bulge. We find a metal-rich population centered at [M/H] = +0.4 dex, in agreement with earlier studies of other bulge regions, but also a peak at low metallicity around $\rm [M/H] = -1.0\,dex$, suggesting the presence of a metal-poor population which has not previously been detected in the central region. Our results indicate a dominant metal-rich population with a metal-poor component that is enhanced in the $\alpha$-elements. This metal-poor population may be associated with the classical bulge and a fast formation scenario.

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