Progenitor-mass-dependent yields amplify intrinsic scatter in dwarf-galaxy elemental abundance ratios
Abstract
We explore the effect of including progenitor mass- and metallicity-dependent yields, supernova rates and energetics on variations in elemental abundance ratios (particularly [α/Fe]) in dwarf galaxies. To understand how the scatter and overall trends in [α/Fe] are affected by including variable metal yields from a discretely sampled initial mass function, we run FIRE simulations of a dwarf galaxy (M⋆(z = 0)∼10⁶M⊙) using nucleosynthetic yields from the NuGrid data base that depend on the stellar progenitor mass and metallicity. While NuGrid exhibits lower aggregate α-element production than default FIRE yields, we find that its explicit mass dependence, even when including turbulent metal diffusion, substantially widens the intrinsic scatter in the simulated [Fe/H]-[α/Fe] – a phenomenon visible in some observations of dwarf galaxies.
Additional Information
© 2021 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). Accepted 2021 September 8. Received 2021 September 7; in original form 2020 August 12. Published: 11 September 2021. We thank Benoit Côté, Andrew Graus, Alexander Ji, Evan Kirby, Mariska Kriek, Shea Garrison-Kimmel, Michael Grudić, Andrew Graus, Xiangcheng Ma, and Kung-Yi Su for useful discussions. Support for DM and coauthors was provided by NSF Collaborative Research Grants 1715847and 1911233, NSF CAREER grant 1455342, and NASA grants 80NSSC18K0562 and JPL 1589742. Numerical calculations were run on the Caltech compute cluster 'Wheeler,' allocations FTA-Hopkins supported by the NSF and TACC, and NASA HEC SMD-16-7592. The data used in this work were, in part, hosted on facilities supported by the Scientific Computing Core at the Flatiron Institute, a division of the Simons Foundation. CRW acknowledges support from NASA through the NASA Hubble Fellowship grant #HST-HF2-51449.001-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 NAS5-26555. AW received support from NASA through ATP grant 80NSSC18K1097 and HST grants GO-14734, AR-15057, AR-15809, and GO-15902 from STScI; a Scialog Award from the Heising-Simons Foundation; and a Hellman Foundation Fellowship. DK was supported by NSF Grant AST-1715101 and by a Cottrell Scholar Award from the Research Corporation for Science Advancement. Data Availability: The data underlying this work will be shared at reasonable request to the corresponding author.Attached Files
Published - stab2572.pdf
Accepted Version - 2008.04901.pdf
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2008.04901.pdf
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Additional details
Identifiers
- Eprint ID
- 111643
- Resolver ID
- CaltechAUTHORS:20211026-152808911
Related works
- Describes
- https://arxiv.org/abs/2008.04901 (URL)
Funding
- NSF
- AST-1715847
- NSF
- AST-1911233
- NSF
- AST-1455342
- NASA
- 80NSSC18K0562
- JPL
- 1589742
- NASA
- SMD-16-7592
- NASA Hubble Fellowship
- HST-HF2-51449.001-A
- NASA
- NAS5-26555
- NASA
- 80NSSC18K1097
- NASA Hubble Fellowship
- GO-14734
- NASA Hubble Fellowship
- AR-15057
- NASA Hubble Fellowship
- AR-15809
- NASA Hubble Fellowship
- GO-15902
- Heising-Simons Foundation
- Hellman Fellowship
- NSF
- AST-1715101
- Cottrell Scholar of Research Corporation
Dates
- Created
-
2021-10-26Created from EPrint's datestamp field
- Updated
-
2021-10-26Created from EPrint's last_modified field