Difference in chemical composition between the bright and faint red clump stars in the milky way bulge

Dongwook Lim, Young Wook Lee, Andreas Koch, Seungsoo Hong, Christian I. Johnson, Jaeyeon Kim, Chul Chung, Mario Mateo, John I. Bailey

Research output: Contribution to journalArticlepeer-review

Abstract

The double red clump (RC) observed in color-magnitude diagrams of the Milky Way bulge is at the heart of the current debate on the structure and formation origin of the bulge. This feature can be explained by the difference between the two RCs either in distance (“X-shaped scenario”) or in chemical composition (“multiple-population scenario”). Here we report our high-resolution spectroscopy for the RC and red giant branch stars in a high-latitude field (b ∼ −8.5°) of the bulge. We find a difference in [Fe/H] between the stars in the bright and faint RC regimes, in the sense that the bright stars are enhanced in [Fe/H] with respect to the faint stars by 0.149 ± 0.036 dex. The stars on the bright RC are also enhanced in [Na/Fe] but appear to be depleted in [Al/Fe] and [O/Fe], although more observations are required to confirm the significance of these differences. Interestingly, these chemical patterns are similar to those observed among multiple stellar populations in the metal-rich bulge globular cluster Terzan 5. In addition, we find a number of Na-rich stars, which would corroborate the presence of multiple populations in the bulge. Our results support an origin of the double RC from dissolved globular clusters that harbor multiple stellar populations. Thus, our study suggests that a substantial fraction of the outer bulge stars would have originated from the assembly of such stellar systems in the early phase of the Milky Way formation.

Original languageEnglish
Article numberabd08d
JournalAstrophysical Journal
Volume907
Issue number1
DOIs
Publication statusPublished - 2021 Jan 20

Bibliographical note

Funding Information:
IRAF is distributed by the National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation.

Funding Information:
We thank the referee for a number of helpful suggestions. We also thank Narae Hwang, Edward Olszewski, Anthony Kremin, Matthew Walker, and the Las Campanas Observatory staff for observing support. Support for this work was provided by the National Research Foundation of Korea (grants

Funding Information:
2017R1A6A3A11031025, 2017R1A2B3002919, and 2017R1A5A1070354). D.L. and A.K. acknowledge support from the Deutsche Forschungsgemeinschaft (DFG; German Research Foundation)—Project-ID 138713538—SFB 881 (“The Milky Way System,” subprojects A03, A05, A11). D. L. thanks Sree Oh and Hyejeon Cho for comments and encouragements.

Publisher Copyright:
© 2021. The American Astronomical Society. All rights reserved.

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Fingerprint Dive into the research topics of 'Difference in chemical composition between the bright and faint red clump stars in the milky way bulge'. Together they form a unique fingerprint.

Cite this