The Lowest Metallicity Stars in the LMC: Clues from MaGICC Simulations
arXiv:1306.3559 · doi:10.1017/pasa.2013.20
Abstract
Using a cosmological hydrodynamical simulation of a galaxy of similar mass to the Large Magellanic Cloud (LMC), we examine the predicted characteristics of its lowest metallicity populations. In particular, we emphasise the spatial distributions of first (Pop III) and second (polluted by only immediate Pop III ancestors) generation stars. We find that primordial composition stars form not only in the central galaxy's progenitor, but also in locally collapsed sub-halos during the early phases of galaxy formation. The lowest metallicity stars in these sub-halos end up in a relatively extended distribution around the host, with these accreted stars possessing present-day galactocentric distances as great as ~40kpc. By contrast, the earliest stars formed within the central galaxy remain in the inner region, where the vast majority of star formation occurs, for the entirety of the simulation. Consequently, the fraction of stars that are from the earliest generation increases strongly with radius.
accepted for publication in PASA, as part of the "The Magellanic System: In Perspective" edition
References in corpus (7)
- Star Formation and Feedback in Smoothed Particle Hydrodynamic Simulations--I. Isolated Galaxies
- Concentration, Spin and Shape of Dark Matter Haloes as a Function of the Cosmological Model: WMAP1, WMAP3 and WMAP5 results
- Are the Magellanic Clouds on their First Passage about the Milky Way?
- The Dual Origin of Stellar Halos
- Exploring Halo Substructure with Giant Stars XI: The Tidal Tails of the Carina Dwarf Spheroidal and the Discovery of Magellanic Cloud Stars in the Carina Foreground
- Constraining Sub-Grid Physics with High-Redshift Spatially-Resolved Metallicity Distributions
- The Spatial Distribution of the Galactic First Stars I: High-Resolution N-body Approach