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Why do high-redshift galaxies show diverse gas-phase metallicity gradients?

Ma, Xiangcheng and Hopkins, Philip F. and Feldmann, Robert and Torrey, Paul and Faucher-Giguère, Claude-André and Kereš, Dušan (2017) Why do high-redshift galaxies show diverse gas-phase metallicity gradients? Monthly Notices of the Royal Astronomical Society, 466 (4). pp. 4780-4794. ISSN 0035-8711. http://resolver.caltech.edu/CaltechAUTHORS:20170623-110357171

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Abstract

Recent spatially resolved observations of galaxies at z ∼ 0.6–3 reveal that high-redshift galaxies show complex kinematics and a broad distribution of gas-phase metallicity gradients. To understand these results, we use a suite of high-resolution cosmological zoom-in simulations from the Feedback in Realistic Environments project, which include physically motivated models of the multiphase interstellar medium, star formation and stellar feedback. Our simulations reproduce the observed diversity of kinematic properties and metallicity gradients, broadly consistent with observations at z ∼ 0–3. Strong negative metallicity gradients only appear in galaxies with a rotating disc, but not all rotationally supported galaxies have significant gradients. Strongly perturbed galaxies with little rotation always have flat gradients. The kinematic properties and metallicity gradient of a high-redshift galaxy can vary significantly on short time-scales, associated with starburst episodes. Feedback from a starburst can destroy the gas disc, drive strong outflows and flatten a pre-existing negative metallicity gradient. The time variability of a single galaxy is statistically similar to the entire simulated sample, indicating that the observed metallicity gradients in high-redshift galaxies reflect the instantaneous state of the galaxy rather than the accretion and growth history on cosmological time-scales. We find weak dependence of metallicity gradient on stellar mass and specific star formation rate (sSFR). Low-mass galaxies and galaxies with high sSFR tend to have flat gradients, likely due to the fact that feedback is more efficient in these galaxies. We argue that it is important to resolve feedback on small scales in order to produce the diverse metallicity gradients observed.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1093/mnras/stx034DOIArticle
https://academic.oup.com/mnras/article-lookup/doi/10.1093/mnras/stx034PublisherArticle
https://arxiv.org/abs/1610.03498arXivDiscussion Paper
ORCID:
AuthorORCID
Hopkins, Philip F.0000-0003-3729-1684
Feldmann, Robert0000-0002-1109-1919
Torrey, Paul0000-0002-5653-0786
Kereš, Dušan0000-0002-1666-7067
Additional Information:© 2017 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2017 January 5. Received 2016 December 30; in original form 2016 October 10. Published: 11 January 2017. We thank Nicha Leethochawalit, Tucker Jones, Richard Ellis, Xin Wang and Tommaso Treu for insightful discussions and Nicha Leethochawalit for providing a compilation of observational data. We also acknowledge the anonymous referee for helpful suggestions on clarifying the manuscript. The simulations used in this paper were run on XSEDE computational resources (allocations TG-AST120025, TG-AST130039, TG-AST140023 and TG-AST150045) and computational resources provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center (proposal SMD-14-5492 and SMD-15-5950). The analysis was performed on the Caltech compute cluster ‘Zwicky’ (NSF MRI award #PHY-0960291). Support for PFH was provided by an Alfred P. Sloan Research Fellowship, NASA ATP Grant NNX14AH35G, and NSF Collaborative Research Grant #1411920 and CAREER grant #1455342. RF was supported in part by NASA through Hubble Fellowship grant HF2-51304.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555, in part by the Theoretical Astrophysics Center at UC Berkeley, and by NASA ATP grant 12-ATP-120183. CAFG was supported by NSF through grants AST-1412836 and AST-1517491, by NASA through grant NNX15AB22G and by STScI through grant HST-AR-14293.001-A. DK was supported by NSF grant AST-1412153 and Cottrell Scholar Award from the Research Corporation for Science Advancement.
Group:TAPIR
Funders:
Funding AgencyGrant Number
NSFTG-AST120025
NSFTG-AST130039
NSFTG-AST140023
NSFTG-AST150045
NSFPHY-0960291
Alfred P. Sloan FoundationUNSPECIFIED
NASANNX14AH35G
NSFAST-1411920
NSFAST-1455342
NASA Hubble FellowshipHF2-51304.001-A
NASANAS 5-26555
University of California, BerkeleyUNSPECIFIED
NASA12-ATP-120183
NSFAST-1412836
NSFAST-1517491
NASANNX15AB22G
NASAHST-AR-14293.001-A
NSFAST-1412153
Cottrell Scholar of Research CorporationUNSPECIFIED
Subject Keywords:galaxies: evolution – galaxies: formation – cosmology: theory
Record Number:CaltechAUTHORS:20170623-110357171
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20170623-110357171
Official Citation:Xiangcheng Ma, Philip F. Hopkins, Robert Feldmann, Paul Torrey, Claude-André Faucher-Giguère, Dušan Kereš; Why do high-redshift galaxies show diverse gas-phase metallicity gradients?. Mon Not R Astron Soc 2017; 466 (4): 4780-4794. doi: 10.1093/mnras/stx034
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:78517
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:24 Jun 2017 02:52
Last Modified:01 Nov 2017 16:48

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