Home > Research > Publications & Outputs > The highly unusual chemical composition of the ...

Associated organisational unit

Links

Text available via DOI:

View graph of relations

The highly unusual chemical composition of the Hercules dwarf spheroidal galaxy

Research output: Contribution to journalJournal articlepeer-review

Published
  • Andreas Koch
  • Andrew McWilliam
  • Eva K. Grebel
  • D. B. Zucker
  • V. Belokurov
Close
<mark>Journal publication date</mark>3/11/2008
<mark>Journal</mark>Astrophysical Journal Letters
Issue number1
Volume688
Number of pages4
Pages (from-to)L13-L16
Publication StatusPublished
<mark>Original language</mark>English

Abstract

We report on the abundance analysis of two red giants in the faint Hercules dwarf spheroidal (dSph) galaxy. These stars show a remarkable deficiency in the neutron-capture elements, while the hydrostatic α-elements (O, Mg) are strongly enhanced. Our data indicate [Ba/Fe] and [Mg/Fe] abundance ratios of lesssim–2 and ~+0.8 dex, respectively, with essentially no detection of other n-capture elements. In contrast to the only other dSph star with similar abundance patterns, Dra 119, which has a very low metallicity at [Fe/H] = –2.95 dex, our objects, at [Fe/H] ~ –2.0 dex, are only moderately metal-poor. The measured ratio of hydrostatic/explosive α-elements indicates that high-mass (~35 M☉) Type II supernovae progenitors are the main, if not only, contributors to the enrichment of this galaxy. This suggests that star formation and chemical enrichment in the ultrafaint dSphs proceeds stochastically and inhomogeneously on small scales, or that the IMF was strongly skewed to high-mass stars. The neutron capture deficiencies and the [Co/Fe] and [Cr/Fe] abundance ratios in our stars are similar to those in the extremely low metallicity Galactic halo. This suggests that either our stars are composed mainly of the ejecta from the first, massive, Population III stars (but at moderately high [Fe/H]), or that SN ejecta in the Hercules galaxy were diluted with ~30 times less hydrogen than typical for extreme metal-poor stars.