Ionizing photon production and escape fractions during cosmic reionization in the TNG50 simulation
In this work, we investigate the dependence of the escape fraction of ionizing photons, fesc, on various galaxy and host halo properties during the epoch of reionization. We post-process the TNG50 magnetohydrodynamical simulation from the IllustrisTNG project using the three-dimensional multifrequen...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Kostyuk, Ivan - 1994- [verfasserIn] Nelson, Dylan [verfasserIn] Ciardi, Benedetta [verfasserIn] Glatzle, Martin [verfasserIn] Pillepich, Annalisa [verfasserIn] |
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| Format: |
E-Artikel |
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| Sprache: |
Englisch |
| Erschienen: |
May 2023 |
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| Anmerkung: |
Veröffentlicht: 17. März 2023 Gesehen am 14.08.2024 |
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| Umfang: |
Illustrationen 21 |
| Übergeordnetes Werk: |
Enthalten in: Monthly notices of the Royal Astronomical Society - Royal Astronomical Society, Oxford : Oxford Univ. Press, 1827, 521(2023), 2 vom: Mai, Seite 3077-3097 |
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| Übergeordnetes Werk: |
volume:521 ; year:2023 ; number:2 ; month:05 ; pages:3077-3097 ; extent:21 |
| Links: |
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| DOI / URN: |
10.1093/mnras/stad677 |
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| Katalog-ID: |
1898660883 |
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| 245 | 1 | 0 | |a Ionizing photon production and escape fractions during cosmic reionization in the TNG50 simulation |c Ivan Kostyuk, Dylan Nelson, Benedetta Ciardi, Martin Glatzle and Annalisa Pillepich |
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| 520 | |a In this work, we investigate the dependence of the escape fraction of ionizing photons, fesc, on various galaxy and host halo properties during the epoch of reionization. We post-process the TNG50 magnetohydrodynamical simulation from the IllustrisTNG project using the three-dimensional multifrequency radiative transfer code CRASH. Our work covers the stellar mass range of 106 ≲ M⋆/M⊙ ≲ 108 at redshifts 6 < z < 10. Adopting an unresolved, cloud-scale escape fraction parameter of unity, the average halo escape fraction fesc increases with mass from ∼0.3 at M⋆ = 106 M⊙ to ∼0.6 at M⋆ = 107.5 M⊙, after which we find hints of a turnover and decreasing escape fractions for even more massive galaxies. However, we demonstrate a strong and non-linear dependence of fesc on the adopted subgrid escape fraction, resulting in uncertainties for the absolute value of the escape fraction. In addition, fesc has significant scatter at fixed mass, driven by diversity in the ionizing photon rate together with a complex relationship between (stellar) source positions and the underling density distribution. The global emissivity is consistent with observations for reasonable cloud-scale absorption values, and haloes with a stellar mass ≲107.5 M⊙ contribute the majority of escaping ionizing photons at all redshifts. Incorporating dust reduces fesc by a few per cent at M⋆ ≲ 106.5 M⊙, and up to 10 per cent for larger haloes. Our multifrequency approach shows that fesc depends on photon energy, and is reduced substantially at E > 54.4 eV versus lower energies. This suggests that the impact of high-energy photons from binary stars is reduced when accounting for an energy-dependent escape fraction. | ||
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10.1093/mnras/stad677 doi (DE-627)1898660883 (DE-599)KXP1898660883 DE-627 ger DE-627 rda eng Kostyuk, Ivan 1994- verfasserin (DE-588)1270733850 (DE-627)1819468925 aut Ionizing photon production and escape fractions during cosmic reionization in the TNG50 simulation Ivan Kostyuk, Dylan Nelson, Benedetta Ciardi, Martin Glatzle and Annalisa Pillepich fifty May 2023 Illustrationen 21 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Veröffentlicht: 17. März 2023 Gesehen am 14.08.2024 In this work, we investigate the dependence of the escape fraction of ionizing photons, fesc, on various galaxy and host halo properties during the epoch of reionization. We post-process the TNG50 magnetohydrodynamical simulation from the IllustrisTNG project using the three-dimensional multifrequency radiative transfer code CRASH. Our work covers the stellar mass range of 106 ≲ M⋆/M⊙ ≲ 108 at redshifts 6 < z < 10. Adopting an unresolved, cloud-scale escape fraction parameter of unity, the average halo escape fraction fesc increases with mass from ∼0.3 at M⋆ = 106 M⊙ to ∼0.6 at M⋆ = 107.5 M⊙, after which we find hints of a turnover and decreasing escape fractions for even more massive galaxies. However, we demonstrate a strong and non-linear dependence of fesc on the adopted subgrid escape fraction, resulting in uncertainties for the absolute value of the escape fraction. In addition, fesc has significant scatter at fixed mass, driven by diversity in the ionizing photon rate together with a complex relationship between (stellar) source positions and the underling density distribution. The global emissivity is consistent with observations for reasonable cloud-scale absorption values, and haloes with a stellar mass ≲107.5 M⊙ contribute the majority of escaping ionizing photons at all redshifts. Incorporating dust reduces fesc by a few per cent at M⋆ ≲ 106.5 M⊙, and up to 10 per cent for larger haloes. Our multifrequency approach shows that fesc depends on photon energy, and is reduced substantially at E > 54.4 eV versus lower energies. This suggests that the impact of high-energy photons from binary stars is reduced when accounting for an energy-dependent escape fraction. Nelson, Dylan verfasserin (DE-588)115182805X (DE-627)101233600X (DE-576)42382581X aut Ciardi, Benedetta verfasserin aut Glatzle, Martin verfasserin aut Pillepich, Annalisa verfasserin (DE-588)1151829854 (DE-627)1012339327 (DE-576)423800841 aut Enthalten in Royal Astronomical Society Monthly notices of the Royal Astronomical Society Oxford : Oxford Univ. Press, 1827 521(2023), 2 vom: Mai, Seite 3077-3097 Online-Ressource (DE-627)314059164 (DE-600)2016084-7 (DE-576)090955420 1365-2966 nnns volume:521 year:2023 number:2 month:05 pages:3077-3097 extent:21 https://doi.org/10.1093/mnras/stad677 Verlag Resolving-System kostenfrei Volltext GBV_USEFLAG_U GBV_ILN_2013 ISIL_DE-16-250 SYSFLAG_1 GBV_KXP GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2007 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2018 GBV_ILN_2026 GBV_ILN_2088 GBV_ILN_2112 GBV_ILN_2190 GBV_ILN_4012 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 GBV_ILN_2403 GBV_ILN_2403 ISIL_DE-LFER AR 521 2023 2 5 3077-3097 21 2013 01 DE-16-250 4566034410 00 --%%-- --%%-- --%%-- --%%-- l01 14-08-24 2403 01 DE-LFER 4574110503 00 --%%-- --%%-- n --%%-- l01 03-09-24 2403 01 DE-LFER https://doi.org/10.1093/mnras/stad677 2013 01 DE-16-250 00 s hd2023 2013 01 DE-16-250 01 s (DE-627)1410508463 wissenschaftlicher Artikel (Zeitschrift) 2013 01 DE-16-250 02 s per_5 2013 01 DE-16-250 03 s s_21 2013 01 DE-16-250 04 p (DE-627)1750174588 Nelson, Dylan 2013 01 DE-16-250 04 k (DE-627)1416733752 ZAH Institut für Theoretische Astrophysik 2013 01 DE-16-250 04 s (DE-627)1410501914 Verfasser 2013 01 DE-16-250 04 s pos_2 2013 01 DE-16-250 05 p (DE-627)1587407663 Pillepich, Annalisa 2013 01 DE-16-250 05 k (DE-627)1416535055 Fakultät für Physik und Astronomie 2013 01 DE-16-250 05 s (DE-627)1410501914 Verfasser 2013 01 DE-16-250 05 s pos_5 |
| spelling |
10.1093/mnras/stad677 doi (DE-627)1898660883 (DE-599)KXP1898660883 DE-627 ger DE-627 rda eng Kostyuk, Ivan 1994- verfasserin (DE-588)1270733850 (DE-627)1819468925 aut Ionizing photon production and escape fractions during cosmic reionization in the TNG50 simulation Ivan Kostyuk, Dylan Nelson, Benedetta Ciardi, Martin Glatzle and Annalisa Pillepich fifty May 2023 Illustrationen 21 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Veröffentlicht: 17. März 2023 Gesehen am 14.08.2024 In this work, we investigate the dependence of the escape fraction of ionizing photons, fesc, on various galaxy and host halo properties during the epoch of reionization. We post-process the TNG50 magnetohydrodynamical simulation from the IllustrisTNG project using the three-dimensional multifrequency radiative transfer code CRASH. Our work covers the stellar mass range of 106 ≲ M⋆/M⊙ ≲ 108 at redshifts 6 < z < 10. Adopting an unresolved, cloud-scale escape fraction parameter of unity, the average halo escape fraction fesc increases with mass from ∼0.3 at M⋆ = 106 M⊙ to ∼0.6 at M⋆ = 107.5 M⊙, after which we find hints of a turnover and decreasing escape fractions for even more massive galaxies. However, we demonstrate a strong and non-linear dependence of fesc on the adopted subgrid escape fraction, resulting in uncertainties for the absolute value of the escape fraction. In addition, fesc has significant scatter at fixed mass, driven by diversity in the ionizing photon rate together with a complex relationship between (stellar) source positions and the underling density distribution. The global emissivity is consistent with observations for reasonable cloud-scale absorption values, and haloes with a stellar mass ≲107.5 M⊙ contribute the majority of escaping ionizing photons at all redshifts. Incorporating dust reduces fesc by a few per cent at M⋆ ≲ 106.5 M⊙, and up to 10 per cent for larger haloes. Our multifrequency approach shows that fesc depends on photon energy, and is reduced substantially at E > 54.4 eV versus lower energies. This suggests that the impact of high-energy photons from binary stars is reduced when accounting for an energy-dependent escape fraction. Nelson, Dylan verfasserin (DE-588)115182805X (DE-627)101233600X (DE-576)42382581X aut Ciardi, Benedetta verfasserin aut Glatzle, Martin verfasserin aut Pillepich, Annalisa verfasserin (DE-588)1151829854 (DE-627)1012339327 (DE-576)423800841 aut Enthalten in Royal Astronomical Society Monthly notices of the Royal Astronomical Society Oxford : Oxford Univ. Press, 1827 521(2023), 2 vom: Mai, Seite 3077-3097 Online-Ressource (DE-627)314059164 (DE-600)2016084-7 (DE-576)090955420 1365-2966 nnns volume:521 year:2023 number:2 month:05 pages:3077-3097 extent:21 https://doi.org/10.1093/mnras/stad677 Verlag Resolving-System kostenfrei Volltext GBV_USEFLAG_U GBV_ILN_2013 ISIL_DE-16-250 SYSFLAG_1 GBV_KXP GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2007 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2018 GBV_ILN_2026 GBV_ILN_2088 GBV_ILN_2112 GBV_ILN_2190 GBV_ILN_4012 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 GBV_ILN_2403 GBV_ILN_2403 ISIL_DE-LFER AR 521 2023 2 5 3077-3097 21 2013 01 DE-16-250 4566034410 00 --%%-- --%%-- --%%-- --%%-- l01 14-08-24 2403 01 DE-LFER 4574110503 00 --%%-- --%%-- n --%%-- l01 03-09-24 2403 01 DE-LFER https://doi.org/10.1093/mnras/stad677 2013 01 DE-16-250 00 s hd2023 2013 01 DE-16-250 01 s (DE-627)1410508463 wissenschaftlicher Artikel (Zeitschrift) 2013 01 DE-16-250 02 s per_5 2013 01 DE-16-250 03 s s_21 2013 01 DE-16-250 04 p (DE-627)1750174588 Nelson, Dylan 2013 01 DE-16-250 04 k (DE-627)1416733752 ZAH Institut für Theoretische Astrophysik 2013 01 DE-16-250 04 s (DE-627)1410501914 Verfasser 2013 01 DE-16-250 04 s pos_2 2013 01 DE-16-250 05 p (DE-627)1587407663 Pillepich, Annalisa 2013 01 DE-16-250 05 k (DE-627)1416535055 Fakultät für Physik und Astronomie 2013 01 DE-16-250 05 s (DE-627)1410501914 Verfasser 2013 01 DE-16-250 05 s pos_5 |
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10.1093/mnras/stad677 doi (DE-627)1898660883 (DE-599)KXP1898660883 DE-627 ger DE-627 rda eng Kostyuk, Ivan 1994- verfasserin (DE-588)1270733850 (DE-627)1819468925 aut Ionizing photon production and escape fractions during cosmic reionization in the TNG50 simulation Ivan Kostyuk, Dylan Nelson, Benedetta Ciardi, Martin Glatzle and Annalisa Pillepich fifty May 2023 Illustrationen 21 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Veröffentlicht: 17. März 2023 Gesehen am 14.08.2024 In this work, we investigate the dependence of the escape fraction of ionizing photons, fesc, on various galaxy and host halo properties during the epoch of reionization. We post-process the TNG50 magnetohydrodynamical simulation from the IllustrisTNG project using the three-dimensional multifrequency radiative transfer code CRASH. Our work covers the stellar mass range of 106 ≲ M⋆/M⊙ ≲ 108 at redshifts 6 < z < 10. Adopting an unresolved, cloud-scale escape fraction parameter of unity, the average halo escape fraction fesc increases with mass from ∼0.3 at M⋆ = 106 M⊙ to ∼0.6 at M⋆ = 107.5 M⊙, after which we find hints of a turnover and decreasing escape fractions for even more massive galaxies. However, we demonstrate a strong and non-linear dependence of fesc on the adopted subgrid escape fraction, resulting in uncertainties for the absolute value of the escape fraction. In addition, fesc has significant scatter at fixed mass, driven by diversity in the ionizing photon rate together with a complex relationship between (stellar) source positions and the underling density distribution. The global emissivity is consistent with observations for reasonable cloud-scale absorption values, and haloes with a stellar mass ≲107.5 M⊙ contribute the majority of escaping ionizing photons at all redshifts. Incorporating dust reduces fesc by a few per cent at M⋆ ≲ 106.5 M⊙, and up to 10 per cent for larger haloes. Our multifrequency approach shows that fesc depends on photon energy, and is reduced substantially at E > 54.4 eV versus lower energies. This suggests that the impact of high-energy photons from binary stars is reduced when accounting for an energy-dependent escape fraction. Nelson, Dylan verfasserin (DE-588)115182805X (DE-627)101233600X (DE-576)42382581X aut Ciardi, Benedetta verfasserin aut Glatzle, Martin verfasserin aut Pillepich, Annalisa verfasserin (DE-588)1151829854 (DE-627)1012339327 (DE-576)423800841 aut Enthalten in Royal Astronomical Society Monthly notices of the Royal Astronomical Society Oxford : Oxford Univ. Press, 1827 521(2023), 2 vom: Mai, Seite 3077-3097 Online-Ressource (DE-627)314059164 (DE-600)2016084-7 (DE-576)090955420 1365-2966 nnns volume:521 year:2023 number:2 month:05 pages:3077-3097 extent:21 https://doi.org/10.1093/mnras/stad677 Verlag Resolving-System kostenfrei Volltext GBV_USEFLAG_U GBV_ILN_2013 ISIL_DE-16-250 SYSFLAG_1 GBV_KXP GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2007 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2018 GBV_ILN_2026 GBV_ILN_2088 GBV_ILN_2112 GBV_ILN_2190 GBV_ILN_4012 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 GBV_ILN_2403 GBV_ILN_2403 ISIL_DE-LFER AR 521 2023 2 5 3077-3097 21 2013 01 DE-16-250 4566034410 00 --%%-- --%%-- --%%-- --%%-- l01 14-08-24 2403 01 DE-LFER 4574110503 00 --%%-- --%%-- n --%%-- l01 03-09-24 2403 01 DE-LFER https://doi.org/10.1093/mnras/stad677 2013 01 DE-16-250 00 s hd2023 2013 01 DE-16-250 01 s (DE-627)1410508463 wissenschaftlicher Artikel (Zeitschrift) 2013 01 DE-16-250 02 s per_5 2013 01 DE-16-250 03 s s_21 2013 01 DE-16-250 04 p (DE-627)1750174588 Nelson, Dylan 2013 01 DE-16-250 04 k (DE-627)1416733752 ZAH Institut für Theoretische Astrophysik 2013 01 DE-16-250 04 s (DE-627)1410501914 Verfasser 2013 01 DE-16-250 04 s pos_2 2013 01 DE-16-250 05 p (DE-627)1587407663 Pillepich, Annalisa 2013 01 DE-16-250 05 k (DE-627)1416535055 Fakultät für Physik und Astronomie 2013 01 DE-16-250 05 s (DE-627)1410501914 Verfasser 2013 01 DE-16-250 05 s pos_5 |
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10.1093/mnras/stad677 doi (DE-627)1898660883 (DE-599)KXP1898660883 DE-627 ger DE-627 rda eng Kostyuk, Ivan 1994- verfasserin (DE-588)1270733850 (DE-627)1819468925 aut Ionizing photon production and escape fractions during cosmic reionization in the TNG50 simulation Ivan Kostyuk, Dylan Nelson, Benedetta Ciardi, Martin Glatzle and Annalisa Pillepich fifty May 2023 Illustrationen 21 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Veröffentlicht: 17. März 2023 Gesehen am 14.08.2024 In this work, we investigate the dependence of the escape fraction of ionizing photons, fesc, on various galaxy and host halo properties during the epoch of reionization. We post-process the TNG50 magnetohydrodynamical simulation from the IllustrisTNG project using the three-dimensional multifrequency radiative transfer code CRASH. Our work covers the stellar mass range of 106 ≲ M⋆/M⊙ ≲ 108 at redshifts 6 < z < 10. Adopting an unresolved, cloud-scale escape fraction parameter of unity, the average halo escape fraction fesc increases with mass from ∼0.3 at M⋆ = 106 M⊙ to ∼0.6 at M⋆ = 107.5 M⊙, after which we find hints of a turnover and decreasing escape fractions for even more massive galaxies. However, we demonstrate a strong and non-linear dependence of fesc on the adopted subgrid escape fraction, resulting in uncertainties for the absolute value of the escape fraction. In addition, fesc has significant scatter at fixed mass, driven by diversity in the ionizing photon rate together with a complex relationship between (stellar) source positions and the underling density distribution. The global emissivity is consistent with observations for reasonable cloud-scale absorption values, and haloes with a stellar mass ≲107.5 M⊙ contribute the majority of escaping ionizing photons at all redshifts. Incorporating dust reduces fesc by a few per cent at M⋆ ≲ 106.5 M⊙, and up to 10 per cent for larger haloes. Our multifrequency approach shows that fesc depends on photon energy, and is reduced substantially at E > 54.4 eV versus lower energies. This suggests that the impact of high-energy photons from binary stars is reduced when accounting for an energy-dependent escape fraction. Nelson, Dylan verfasserin (DE-588)115182805X (DE-627)101233600X (DE-576)42382581X aut Ciardi, Benedetta verfasserin aut Glatzle, Martin verfasserin aut Pillepich, Annalisa verfasserin (DE-588)1151829854 (DE-627)1012339327 (DE-576)423800841 aut Enthalten in Royal Astronomical Society Monthly notices of the Royal Astronomical Society Oxford : Oxford Univ. Press, 1827 521(2023), 2 vom: Mai, Seite 3077-3097 Online-Ressource (DE-627)314059164 (DE-600)2016084-7 (DE-576)090955420 1365-2966 nnns volume:521 year:2023 number:2 month:05 pages:3077-3097 extent:21 https://doi.org/10.1093/mnras/stad677 Verlag Resolving-System kostenfrei Volltext GBV_USEFLAG_U GBV_ILN_2013 ISIL_DE-16-250 SYSFLAG_1 GBV_KXP GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2007 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2018 GBV_ILN_2026 GBV_ILN_2088 GBV_ILN_2112 GBV_ILN_2190 GBV_ILN_4012 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 GBV_ILN_2403 GBV_ILN_2403 ISIL_DE-LFER AR 521 2023 2 5 3077-3097 21 2013 01 DE-16-250 4566034410 00 --%%-- --%%-- --%%-- --%%-- l01 14-08-24 2403 01 DE-LFER 4574110503 00 --%%-- --%%-- n --%%-- l01 03-09-24 2403 01 DE-LFER https://doi.org/10.1093/mnras/stad677 2013 01 DE-16-250 00 s hd2023 2013 01 DE-16-250 01 s (DE-627)1410508463 wissenschaftlicher Artikel (Zeitschrift) 2013 01 DE-16-250 02 s per_5 2013 01 DE-16-250 03 s s_21 2013 01 DE-16-250 04 p (DE-627)1750174588 Nelson, Dylan 2013 01 DE-16-250 04 k (DE-627)1416733752 ZAH Institut für Theoretische Astrophysik 2013 01 DE-16-250 04 s (DE-627)1410501914 Verfasser 2013 01 DE-16-250 04 s pos_2 2013 01 DE-16-250 05 p (DE-627)1587407663 Pillepich, Annalisa 2013 01 DE-16-250 05 k (DE-627)1416535055 Fakultät für Physik und Astronomie 2013 01 DE-16-250 05 s (DE-627)1410501914 Verfasser 2013 01 DE-16-250 05 s pos_5 |
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10.1093/mnras/stad677 doi (DE-627)1898660883 (DE-599)KXP1898660883 DE-627 ger DE-627 rda eng Kostyuk, Ivan 1994- verfasserin (DE-588)1270733850 (DE-627)1819468925 aut Ionizing photon production and escape fractions during cosmic reionization in the TNG50 simulation Ivan Kostyuk, Dylan Nelson, Benedetta Ciardi, Martin Glatzle and Annalisa Pillepich fifty May 2023 Illustrationen 21 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Veröffentlicht: 17. März 2023 Gesehen am 14.08.2024 In this work, we investigate the dependence of the escape fraction of ionizing photons, fesc, on various galaxy and host halo properties during the epoch of reionization. We post-process the TNG50 magnetohydrodynamical simulation from the IllustrisTNG project using the three-dimensional multifrequency radiative transfer code CRASH. Our work covers the stellar mass range of 106 ≲ M⋆/M⊙ ≲ 108 at redshifts 6 < z < 10. Adopting an unresolved, cloud-scale escape fraction parameter of unity, the average halo escape fraction fesc increases with mass from ∼0.3 at M⋆ = 106 M⊙ to ∼0.6 at M⋆ = 107.5 M⊙, after which we find hints of a turnover and decreasing escape fractions for even more massive galaxies. However, we demonstrate a strong and non-linear dependence of fesc on the adopted subgrid escape fraction, resulting in uncertainties for the absolute value of the escape fraction. In addition, fesc has significant scatter at fixed mass, driven by diversity in the ionizing photon rate together with a complex relationship between (stellar) source positions and the underling density distribution. The global emissivity is consistent with observations for reasonable cloud-scale absorption values, and haloes with a stellar mass ≲107.5 M⊙ contribute the majority of escaping ionizing photons at all redshifts. Incorporating dust reduces fesc by a few per cent at M⋆ ≲ 106.5 M⊙, and up to 10 per cent for larger haloes. Our multifrequency approach shows that fesc depends on photon energy, and is reduced substantially at E > 54.4 eV versus lower energies. This suggests that the impact of high-energy photons from binary stars is reduced when accounting for an energy-dependent escape fraction. Nelson, Dylan verfasserin (DE-588)115182805X (DE-627)101233600X (DE-576)42382581X aut Ciardi, Benedetta verfasserin aut Glatzle, Martin verfasserin aut Pillepich, Annalisa verfasserin (DE-588)1151829854 (DE-627)1012339327 (DE-576)423800841 aut Enthalten in Royal Astronomical Society Monthly notices of the Royal Astronomical Society Oxford : Oxford Univ. Press, 1827 521(2023), 2 vom: Mai, Seite 3077-3097 Online-Ressource (DE-627)314059164 (DE-600)2016084-7 (DE-576)090955420 1365-2966 nnns volume:521 year:2023 number:2 month:05 pages:3077-3097 extent:21 https://doi.org/10.1093/mnras/stad677 Verlag Resolving-System kostenfrei Volltext GBV_USEFLAG_U GBV_ILN_2013 ISIL_DE-16-250 SYSFLAG_1 GBV_KXP GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2007 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2018 GBV_ILN_2026 GBV_ILN_2088 GBV_ILN_2112 GBV_ILN_2190 GBV_ILN_4012 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 GBV_ILN_2403 GBV_ILN_2403 ISIL_DE-LFER AR 521 2023 2 5 3077-3097 21 2013 01 DE-16-250 4566034410 00 --%%-- --%%-- --%%-- --%%-- l01 14-08-24 2403 01 DE-LFER 4574110503 00 --%%-- --%%-- n --%%-- l01 03-09-24 2403 01 DE-LFER https://doi.org/10.1093/mnras/stad677 2013 01 DE-16-250 00 s hd2023 2013 01 DE-16-250 01 s (DE-627)1410508463 wissenschaftlicher Artikel (Zeitschrift) 2013 01 DE-16-250 02 s per_5 2013 01 DE-16-250 03 s s_21 2013 01 DE-16-250 04 p (DE-627)1750174588 Nelson, Dylan 2013 01 DE-16-250 04 k (DE-627)1416733752 ZAH Institut für Theoretische Astrophysik 2013 01 DE-16-250 04 s (DE-627)1410501914 Verfasser 2013 01 DE-16-250 04 s pos_2 2013 01 DE-16-250 05 p (DE-627)1587407663 Pillepich, Annalisa 2013 01 DE-16-250 05 k (DE-627)1416535055 Fakultät für Physik und Astronomie 2013 01 DE-16-250 05 s (DE-627)1410501914 Verfasser 2013 01 DE-16-250 05 s pos_5 |
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März 2023</subfield></datafield><datafield tag="500" ind1=" " ind2=" "><subfield code="a">Gesehen am 14.08.2024</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a">In this work, we investigate the dependence of the escape fraction of ionizing photons, fesc, on various galaxy and host halo properties during the epoch of reionization. We post-process the TNG50 magnetohydrodynamical simulation from the IllustrisTNG project using the three-dimensional multifrequency radiative transfer code CRASH. Our work covers the stellar mass range of 106 ≲ M⋆/M⊙ ≲ 108 at redshifts 6 < z < 10. Adopting an unresolved, cloud-scale escape fraction parameter of unity, the average halo escape fraction fesc increases with mass from ∼0.3 at M⋆ = 106 M⊙ to ∼0.6 at M⋆ = 107.5 M⊙, after which we find hints of a turnover and decreasing escape fractions for even more massive galaxies. However, we demonstrate a strong and non-linear dependence of fesc on the adopted subgrid escape fraction, resulting in uncertainties for the absolute value of the escape fraction. In addition, fesc has significant scatter at fixed mass, driven by diversity in the ionizing photon rate together with a complex relationship between (stellar) source positions and the underling density distribution. The global emissivity is consistent with observations for reasonable cloud-scale absorption values, and haloes with a stellar mass ≲107.5 M⊙ contribute the majority of escaping ionizing photons at all redshifts. Incorporating dust reduces fesc by a few per cent at M⋆ ≲ 106.5 M⊙, and up to 10 per cent for larger haloes. Our multifrequency approach shows that fesc depends on photon energy, and is reduced substantially at E > 54.4 eV versus lower energies. 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ionizing photon production and escape fractions during cosmic reionization in the tng50 simulation |
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Ionizing photon production and escape fractions during cosmic reionization in the TNG50 simulation |
| abstract |
In this work, we investigate the dependence of the escape fraction of ionizing photons, fesc, on various galaxy and host halo properties during the epoch of reionization. We post-process the TNG50 magnetohydrodynamical simulation from the IllustrisTNG project using the three-dimensional multifrequency radiative transfer code CRASH. Our work covers the stellar mass range of 106 ≲ M⋆/M⊙ ≲ 108 at redshifts 6 < z < 10. Adopting an unresolved, cloud-scale escape fraction parameter of unity, the average halo escape fraction fesc increases with mass from ∼0.3 at M⋆ = 106 M⊙ to ∼0.6 at M⋆ = 107.5 M⊙, after which we find hints of a turnover and decreasing escape fractions for even more massive galaxies. However, we demonstrate a strong and non-linear dependence of fesc on the adopted subgrid escape fraction, resulting in uncertainties for the absolute value of the escape fraction. In addition, fesc has significant scatter at fixed mass, driven by diversity in the ionizing photon rate together with a complex relationship between (stellar) source positions and the underling density distribution. The global emissivity is consistent with observations for reasonable cloud-scale absorption values, and haloes with a stellar mass ≲107.5 M⊙ contribute the majority of escaping ionizing photons at all redshifts. Incorporating dust reduces fesc by a few per cent at M⋆ ≲ 106.5 M⊙, and up to 10 per cent for larger haloes. Our multifrequency approach shows that fesc depends on photon energy, and is reduced substantially at E > 54.4 eV versus lower energies. This suggests that the impact of high-energy photons from binary stars is reduced when accounting for an energy-dependent escape fraction. Veröffentlicht: 17. März 2023 Gesehen am 14.08.2024 |
| abstractGer |
In this work, we investigate the dependence of the escape fraction of ionizing photons, fesc, on various galaxy and host halo properties during the epoch of reionization. We post-process the TNG50 magnetohydrodynamical simulation from the IllustrisTNG project using the three-dimensional multifrequency radiative transfer code CRASH. Our work covers the stellar mass range of 106 ≲ M⋆/M⊙ ≲ 108 at redshifts 6 < z < 10. Adopting an unresolved, cloud-scale escape fraction parameter of unity, the average halo escape fraction fesc increases with mass from ∼0.3 at M⋆ = 106 M⊙ to ∼0.6 at M⋆ = 107.5 M⊙, after which we find hints of a turnover and decreasing escape fractions for even more massive galaxies. However, we demonstrate a strong and non-linear dependence of fesc on the adopted subgrid escape fraction, resulting in uncertainties for the absolute value of the escape fraction. In addition, fesc has significant scatter at fixed mass, driven by diversity in the ionizing photon rate together with a complex relationship between (stellar) source positions and the underling density distribution. The global emissivity is consistent with observations for reasonable cloud-scale absorption values, and haloes with a stellar mass ≲107.5 M⊙ contribute the majority of escaping ionizing photons at all redshifts. Incorporating dust reduces fesc by a few per cent at M⋆ ≲ 106.5 M⊙, and up to 10 per cent for larger haloes. Our multifrequency approach shows that fesc depends on photon energy, and is reduced substantially at E > 54.4 eV versus lower energies. This suggests that the impact of high-energy photons from binary stars is reduced when accounting for an energy-dependent escape fraction. Veröffentlicht: 17. März 2023 Gesehen am 14.08.2024 |
| abstract_unstemmed |
In this work, we investigate the dependence of the escape fraction of ionizing photons, fesc, on various galaxy and host halo properties during the epoch of reionization. We post-process the TNG50 magnetohydrodynamical simulation from the IllustrisTNG project using the three-dimensional multifrequency radiative transfer code CRASH. Our work covers the stellar mass range of 106 ≲ M⋆/M⊙ ≲ 108 at redshifts 6 < z < 10. Adopting an unresolved, cloud-scale escape fraction parameter of unity, the average halo escape fraction fesc increases with mass from ∼0.3 at M⋆ = 106 M⊙ to ∼0.6 at M⋆ = 107.5 M⊙, after which we find hints of a turnover and decreasing escape fractions for even more massive galaxies. However, we demonstrate a strong and non-linear dependence of fesc on the adopted subgrid escape fraction, resulting in uncertainties for the absolute value of the escape fraction. In addition, fesc has significant scatter at fixed mass, driven by diversity in the ionizing photon rate together with a complex relationship between (stellar) source positions and the underling density distribution. The global emissivity is consistent with observations for reasonable cloud-scale absorption values, and haloes with a stellar mass ≲107.5 M⊙ contribute the majority of escaping ionizing photons at all redshifts. Incorporating dust reduces fesc by a few per cent at M⋆ ≲ 106.5 M⊙, and up to 10 per cent for larger haloes. Our multifrequency approach shows that fesc depends on photon energy, and is reduced substantially at E > 54.4 eV versus lower energies. This suggests that the impact of high-energy photons from binary stars is reduced when accounting for an energy-dependent escape fraction. Veröffentlicht: 17. März 2023 Gesehen am 14.08.2024 |
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Ionizing photon production and escape fractions during cosmic reionization in the TNG50 simulation |
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