The signature of galaxy formation models in the power spectrum of the hydrogen 21 cm line during reionization
Observations of the 21 cm line of hydrogen are poised to revolutionize our knowledge of reionization and the first galaxies. However, harnessing such information requires robust and comprehensive theoretical modelling. We study the non-linear effects of hydrodynamics and astrophysical feedback proce...
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| Hauptverfasser: | , , , , |
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| Dokumenttyp: | Article (Journal) |
| Sprache: | Englisch |
| Veröffentlicht: |
February 2024
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| In: |
Monthly notices of the Royal Astronomical Society
Year: 2024, Jahrgang: 528, Heft: 2, Pages: 3592-3612 |
| ISSN: | 1365-2966 |
| DOI: | 10.1093/mnras/stad3903 |
| Online-Zugang: | Verlag, kostenfrei, Volltext: https://doi.org/10.1093/mnras/stad3903
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| Verfasserangaben: | Joseph S.W. Lewis, Annalisa Pillepich, Dylan Nelson, Ralf S. Klessen and Simon C.O. Glover |
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| 100 | 1 | |a Lewis, Joseph |e VerfasserIn |0 (DE-588)1268840114 |0 (DE-627)1817370995 |4 aut | |
| 245 | 1 | 4 | |a The signature of galaxy formation models in the power spectrum of the hydrogen 21 cm line during reionization |c Joseph S.W. Lewis, Annalisa Pillepich, Dylan Nelson, Ralf S. Klessen and Simon C.O. Glover |
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| 520 | |a Observations of the 21 cm line of hydrogen are poised to revolutionize our knowledge of reionization and the first galaxies. However, harnessing such information requires robust and comprehensive theoretical modelling. We study the non-linear effects of hydrodynamics and astrophysical feedback processes, including stellar and AGN feedback, on the 21 cm signal by post-processing three existing cosmological hydrodynamical simulations of galaxy formation: Illustris, IllustrisTNG, and Eagle. Despite their different underlying galaxy-formation models, the simulations return similar predictions for the global 21 cm brightness temperature and its power spectrum. At fixed redshift, most differences are attributable to alternative reionization histories, in turn driven by differences in the buildup of stellar sources of radiation. However, several astrophysical processes imprint signatures in the 21 cm power spectrum at two key scales. First, we find significant small-scale |k \ge 10\, \rm {Mpc}^{-1}$) differences between Illustris and IllustrisTNG, where higher velocity winds generated by supernova feedback soften density peaks, leading to lower 21 cm power in TNG. Thus, constraints at these scales could rule out extreme feedback models. Secondly, we find more 21 cm power at intermediate scales |k \approx 0.8\, \rm {Mpc}^{-1}$) in Eagle due to ionization differences driven by highly effective stellar feedback, resulting in lower star formation, older and redder stellar populations, and lower ionizing luminosities for $M_h \gt 10^9 \, \rm M_\odot$. Different source models can manifest similarly in the 21 cm power spectrum, leading to often ignored degeneracies. These subtle features could allow future observations of the 21 cm signal, in conjunction with other observables, to constrain theoretical models for galactic feedback at high redshift. | ||
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| 700 | 1 | |a Nelson, Dylan |e VerfasserIn |0 (DE-588)115182805X |0 (DE-627)101233600X |0 (DE-576)42382581X |4 aut | |
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