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Phase-space distributions of chemical abundances in Milky Way-type Galaxy halos.

Font, A. S. and Johnston, K. V. and Bullock, J. S. and Robertson, B. E. (2006) 'Phase-space distributions of chemical abundances in Milky Way-type Galaxy halos.', Astrophysical journal., 646 (2). pp. 886-898.


Motivated by upcoming data from astrometric and spectroscopic surveys of the Galaxy, we explore the chemical abundance properties and phase-space distributions in hierarchically formed stellar halo simulations set in a CDM universe. Our stellar halo metallicities increase with stellar halo mass. The slope of the [Fe/H]-M* trend mimics that of the satellite galaxies that were destroyed to build the halos, implying that the relation propagates hierarchically. All simulated halos contain a significant fraction of old stellar populations accreted more than 10 Gyr ago, and in a few cases some intermediate-age populations exist. In contrast with the Milky Way, many of our simulated stellar halos contain old stellar populations that are metal-rich, originating in the early accretion of massive satellites (M* 109 M). We suggest that the (metal-rich) stellar halo of M31 falls into this category, while the more metal-poor halo of the Milky Way is lacking in early massive accretion events. Interestingly, our hierarchically formed stellar halos often have nonnegligible metallicity gradients in both [Fe/H] and [/Fe]. These gradients extend a few tens of kiloparsecs, and can be as large as 0.5 dex in [Fe/H] and 0.2 dex in [/Fe], with the most metal-poor halo stars typically buried within the central 5 kpc of the galaxy. Finally, we find that chemical abundances can act as a rough substitute for time of accretion of satellite galaxies, and, based on this finding, we propose a criterion for identifying tidal streams spatially by selecting stars with [/Fe] ratios below solar.

Item Type:Article
Keywords:Cosmology, Theory-galaxies, Abundances, Evolution.
Full text:Full text not available from this repository.
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Record Created:10 Jan 2008
Last Modified:15 Mar 2011 12:41

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