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Title: Blanco DECam Bulge Survey (BDBS) Ⅳ: Metallicity distributions and bulge structure from 2.6 million red clump stars

Journal Article · · Monthly Notices of the Royal Astronomical Society
 [1]; ORCiD logo [2];  [3];  [4];  [5];  [4];  [4]; ORCiD logo [6]; ORCiD logo [7];  [8];  [9];  [10]; ORCiD logo [1];  [11];  [12]
  1. Space Telescope Science Institute, Baltimore, MD (United States)
  2. University of California, Los Angeles, CA (United States)
  3. Shanghai Normal University (China)
  4. Indiana University, Bloomington, IN (United States)
  5. University of Michigan-Dearborn, MI (United States)
  6. European Southern Observatory, Munich (Germany)
  7. Universidad de Atacama, Copiapó (Chile)
  8. Saint Martin’s University, Lacey, WA (United States)
  9. Heidelberg University (Germany)
  10. National Optical-Infrared Astronomy Research Laboratory, La Serena (Chile)
  11. Shanghai Jiao Tong University (China); Key Laboratory for Particle Astrophysics and Cosmology (MOE) / Shanghai Key Laboratory for Particle Physics and Cosmology, Shanghai (China)
  12. University of Michigan-Dearborn, MI (United States); University of South Carolina, Columbia, SC (United States)

We present photometric metallicity measurements for a sample of 2.6 million bulge red clump stars extracted from the Blanco DECam Bulge Survey (BDBS). Similar to previous studies, we find that the bulge exhibits a strong vertical metallicity gradient, and that at least two peaks in the metallicity distribution functions appear at b < -5°. We can discern a metal-poor ([Fe/H] ~ -0.3) and metal-rich ([Fe/H] ~+0.2) abundance distribution that each show clear systematic trends with latitude, and may be best understood by changes in the bulge’s star formation/enrichment processes. Both groups exhibit asymmetric tails, and as a result we argue that the proximity of a star to either peak in [Fe/H] space is not necessarily an affirmation of group membership. The metal-poor peak shifts to lower [Fe/H] values at larger distances from the plane while the metal-rich tail truncates. Close to the plane, the metal-rich tail appears broader along the minor axis than in off-axis fields. We also posit that the bulge has two metal-poor populations – one that belongs to the metal-poor tail of the low latitude and predominantly metal-rich group, and another belonging to the metal-poor group that dominates in the outer bulge. We detect the X-shape structure in fields with |Z| >0.7 kpc and for stars with [Fe/H] < -0.5. Stars with [Fe/H] > -0.5 may form a spheroidal or ‘thick bar’ distribution while those with [Fe/H] ≳ -0.1 are strongly concentrated near the plane.

Research Organization:
Oak Ridge Institute for Science and Education (ORISE), Oak Ridge, TN (United States)
Sponsoring Organization:
German Research Foundation (DFG); National Science Foundation (NSF); USDOE Office of Science (SC)
Grant/Contract Number:
SC0014664
OSTI ID:
1982630
Journal Information:
Monthly Notices of the Royal Astronomical Society, Journal Name: Monthly Notices of the Royal Astronomical Society Journal Issue: 1 Vol. 515; ISSN 0035-8711
Publisher:
Oxford University PressCopyright Statement
Country of Publication:
United States
Language:
English

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