Chemical and dynamical properties of the stellar halo

Ch Brook, D. Kawata, H. Martel, B. Gibson, E. Scannapieco

Research output: Chapter in Book/Report/Conference proceedingConference contribution

2 Scopus citations


The difference in density profiles of the contributions from different density peaks to dark matter halos results in certain expectations about the Milky Way's stellar halo. We cut our simulated halo stars into two populations: those forming before/during the last major merger, and those accreted after the last major merger. The former population are more centrally located at z = 0, while stars forming in low mass late forming proto-galaxies are spread through the halo. A difference in observed binding energy distinguishes these two populations. We look at possible chemical abundance signatures of the two populations. We also show that galaxies forming in isolated low a peaks will form from primordial material. Thus, even though the oldest stars are centrally concentrated as they originated in the early collapsing, densest regions, primordial stars would be found distributed throughout the halo. Thus, the lack of observed metal free stars can be taken as directly constraining the Population III IMF, and the lowest metallicity observed stars can be interpreted as holding clues to the chemical yields of Pop III stars.

Original languageEnglish (US)
Title of host publicationCRAL-2006 Chemodynamics
Subtitle of host publicationFrom First Stars to Local Galaxies
EditorsE. Emsellem, H. Wozniak, G. Massacrier, J.-F. Gonzales, J. Devriendt, N. Champavert
Number of pages7
StatePublished - 2007
Externally publishedYes

Publication series

NameEAS Publications Series
ISSN (Print)1633-4760
ISSN (Electronic)1638-1963

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • General Engineering
  • Space and Planetary Science


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