Evolution of the grain size distribution in Milky Way-like galaxies in post-processed IllustrisTNG simulations
We model dust evolution in Milky Way-like galaxies by post-processing the IllustrisTNG cosmological hydrodynamical simulations in order to predict dust-to-gas ratios and grain size distributions. We treat grain-size-dependent dust growth and destruction processes using a 64-bin discrete grain size e...
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| Hauptverfasser: | , , , , , |
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| Dokumenttyp: | Article (Journal) |
| Sprache: | Englisch |
| Veröffentlicht: |
2021
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| In: |
Monthly notices of the Royal Astronomical Society
Year: 2020, Jahrgang: 501, Heft: 1, Pages: 1336-1351 |
| ISSN: | 1365-2966 |
| DOI: | 10.1093/mnras/staa3695 |
| Online-Zugang: | Verlag, lizenzpflichtig, Volltext: https://doi.org/10.1093/mnras/staa3695
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| Verfasserangaben: | Yu-Hsiu Huang, Hiroyuki Hirashita, Yun-Hsin Hsu, Yen-Ting Lin, Dylan Nelson and Andrew P Cooper |
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| 245 | 1 | 0 | |a Evolution of the grain size distribution in Milky Way-like galaxies in post-processed IllustrisTNG simulations |c Yu-Hsiu Huang, Hiroyuki Hirashita, Yun-Hsin Hsu, Yen-Ting Lin, Dylan Nelson and Andrew P Cooper |
| 264 | 1 | |c 2021 | |
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| 500 | |a Gesehen am 02.03.2021 | ||
| 520 | |a We model dust evolution in Milky Way-like galaxies by post-processing the IllustrisTNG cosmological hydrodynamical simulations in order to predict dust-to-gas ratios and grain size distributions. We treat grain-size-dependent dust growth and destruction processes using a 64-bin discrete grain size evolution model without spatially resolving each galaxy. Our model broadly reproduces the observed dust-metallicity scaling relation in nearby galaxies. The grain size distribution is dominated by large grains at z ≳ 3 and the small-grain abundance rapidly increases by shattering and accretion (dust growth) at z ≲ 2. The grain size distribution approaches the so-called MRN distribution at z ∼ 1, but a suppression of large-grain abundances occurs at z < 1. Based on the computed grain size distributions and grain compositions, we also calculate the evolution of the extinction curve for each Milky Way analogue. Extinction curves are initially flat at z > 2, and become consistent with the Milky Way extinction curve at z ≲ 1 at $1/\lambda \lt 6~\rm{\mu m}^{-1}$. However, typical extinction curves predicted by our model have a steeper slope at short wavelengths than is observed in the Milky Way. This is due to the low-redshift decline of gas-phase metallicity and the dense gas fraction in our TNG Milky Way analogues that suppresses the formation of large grains through coagulation. | ||
| 534 | |c 2020 | ||
| 700 | 1 | |a Hirashita, Hiroyuki |e VerfasserIn |4 aut | |
| 700 | 1 | |a Hsu, Yun-Hsin |e VerfasserIn |4 aut | |
| 700 | 1 | |a Lin, Yen-Ting |e VerfasserIn |4 aut | |
| 700 | 1 | |a Nelson, Dylan |e VerfasserIn |0 (DE-588)115182805X |0 (DE-627)101233600X |0 (DE-576)42382581X |4 aut | |
| 700 | 1 | |a Cooper, Andrew P |e VerfasserIn |4 aut | |
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