The Origin and Evolution of the Galaxy Mass-Metallicity Relation
Abstract
We use high-resolution cosmological zoom-in simulations from the Feedback in Realistic Environment (FIRE) project to study the galaxy mass–metallicity relations (MZR) from z=0–6. These simulations include explicit models of the multi-phase ISM, star formation, and stellar feedback. The simulations cover halo masses M_(halo) = 10^9–10^(13) M_☉ and stellar masses M_* = 10^4–10^(11) M_☉ at z = 0 and have been shown to produce many observed galaxy properties from z = 0–6. For the first time, our simulations agree reasonably well with the observed mass–metallicity relations at z = 0–3 for a broad range of galaxy masses. We predict the evolution of the MZR from z = 0–6, as log(Z_(gas)/Z_☉) = 12+log(O/H)-9.0 = 0.35 [log(M_*/M_☉) - 10] + 0.93exp(-0.43z) - 1.05 and log(Z_*/Z_☉) = [Fe=H] + 0.2 = 0.40 [log(M_*/M_☉)-10]+0.67exp(-0.50z)-1.04, for gas-phase and stellar metallicity, respectively. Our simulations suggest that the evolution of MZR is associated with the evolution of stellar/gas mass fractions at different redshifts, indicating the existence of a universal metallicity relation between stellar mass, gas mass, and metallicities. In our simulations, galaxies above M_* = 10^6 M_☉ are able to retain a large fraction of their metals inside the halo, because metal-rich winds fail to escape completely and are recycled into the galaxy. This resolves a long-standing discrepancy between "sub-grid" wind models (and semi-analytic models) and observations, where common sub-grid models cannot simultaneously reproduce the MZR and the stellar mass functions.
Additional Information
© 2015 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2015 November 10. Received 2015 October 17. In original form 2015 April 8. First published online December 30, 2015. We thank Daniel Anglés-Alcázar, Yu Lu, Evan Kirby, Paul Torrey, Andrew Wetzel, and many friends for helpful discussion and useful comments on this paper. The simulations used in this paper were run on XSEDE computational resources (allocations TGAST120025, TG-AST130039, and TG-AST140023). Support for PFH was provided by the Gordon and Betty Moore Foundation through Grant 776 to the Caltech Moore Center for Theoretical Cosmology and Physics, by the Alfred P. Sloan Foundation through Sloan Research Fellowship BR2014-022, and by NSF through grant AST-1411920. CAFG was supported by NSF through grant AST-1412836, by NASA through grant NNX15AB22G, and by Northwestern University funds. DK was supported by NSF grant AST-1412153 and UC San Diego funds. EQ was supported by NASA ATP grant 12-APT12-0183, a Simons Investigator award from the Simons Foundation, the David and Lucile Packard Foundation, and the Thomas Alison Schneider Chair in Physics at UC Berkeley.Attached Files
Published - MNRAS-2016-Ma-2140-56.pdf
Submitted - 1504.02097v1.pdf
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Additional details
- Eprint ID
- 56899
- Resolver ID
- CaltechAUTHORS:20150423-081343792
- Gordon and Betty Moore Foundation
- 776
- Alfred P. Sloan Foundation
- BR2014-022
- NSF
- AST-1411920
- NSF
- AST-1412836
- NASA
- NNX15AB22G
- Northwestern University
- NSF
- AST-1412153
- University of California, San Diego
- NASA
- 12-APT12-0183
- Simons Foundation
- David and Lucile Packard Foundation
- UC Berkeley
- Created
-
2015-04-23Created from EPrint's datestamp field
- Updated
-
2021-11-10Created from EPrint's last_modified field
- Caltech groups
- TAPIR, Moore Center for Theoretical Cosmology and Physics