The Origin of the Galaxy Mass-Metallicity Relation and Implications for Galactic Outflows

Details The Origin of the Galaxy Mass-Metallicity Relation and Implications for Galactic Outflows The Origin of the Galaxy Mass-Metallicity Relation and Implications for Galactic Outflows

2007-04-24

arxiv.org/abs/0704.3100v2

Astronomy and Astrophysics

Astrophysics

28 pages, 15 figures, accepted by MNRAS with minor revisions. The definitive version is available at www.blackell-synergy.com

Scientific paper

10.1111/j.1365-2966.2008.12991.x

(Abridged) Using cosmological hydrodynamic simulations in combination with analytic modeling, we show that the galaxy stellar mass-metallicity relation (MZR) provides strong constraints on galactic outflows across cosmic time. We compare three outflow models: No outflows, a "constant wind" (cw) model that emulates the popular Dekel & Silk (1986) scenario, and a ``momentum-driven wind" (vzw) model. We find that only the vzw scaling reproduces the observed z~2 MZR's slope, amplitude, and scatter. Comparing our fully three-dimensional simulations with a simple one-zone chemical evolution model, we find that the MZR can be understood in terms of three parameters: (1) The equilibrium metallicity Z_eq=y*SFR/ACC (where y=true yield), reflecting the enrichment balance between star formation rate SFR and gas accretion rate ACC; (2) the dilution time t_d=M_g/ACC, representing the timescale for a galaxy to return to Z_eq after a metallicity-perturbing interaction; and (3) the blowout mass M_blowout, which is the galaxy stellar mass above which winds can escape its halo. When outflows with mass loading factor MLF are present, galaxies below M_blowout obey Z_eq = y/(1+MLF), while above M_blowout, Z_eq->y. Our cw model has M_blowout ~ 10^10 M_sun, which yields a sharp upturn in the MZR above this scale and a flat MZR with large scatter below it, in strong disagreement with observations. Our vzw model reproduces the observed Z_g \propto M_*^0.3 because Z_eq \propto MLF^-1 \propto M_*^1/3 when MLF >> 1 (i.e. at low masses). The flattening of the MZR at M_* > 10^10.5 M_sun observed by Tremonti et al. (2004) reflects the mass scale where MLF~1, rather than a characteristic wind speed. The tight observed MZR scatter is ensured when t_d<1 dynamical time, which is only satisified at all masses and epochs in our momentum-driven wind model.

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