The Chemical Evolution of Milky Way Satellite Galaxies

Details The Chemical Evolution of Milky Way Satellite Galaxies The Chemical Evolution of Milky Way Satellite Galaxies

Aug 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011rrls.conf..263k&link_type=abstract

RR Lyrae Stars, Metal-Poor Stars, and the Galaxy, Carnegie Observatories %Astrophysics Series, Vol. 5. Edited by Andrew McWillia

Astronomy and Astrophysics

Astrophysics

Scientific paper

A Keck/DEIMOS spectroscopic campaign of eight Milky Way (MW) dwarf spheroidal (dSph) satellite galaxies has generated spectral synthesis-based abundance measurements for nearly 3000 stars. The elements measured are Fe and the α elements Mg, Si, Ca, and Ti. The dSph metallicity distributions show that the histories of the less luminous dSphs were marked by massive amounts of gas loss. The [α4/Fe] distributions indicate that the early star formation histories of most dSphs ere very similar and that Type Ia supernova ejecta contributed to the abundances of all but the most metal-poor ([Fe/H]<-2.5) stars. Finally, a numerical chemical evolution model reveals that the star formation history of a dSph is a strong function of its present-day luminosity, but not vvelocity dispersion, half-light radius, or Galacocentric distance.

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