Toward precise galaxy evolution : a comparison between spectral Indices of z ∼ 1 galaxies in the IllustrisTNG simulation and the LEGA-C survey
We present the first comparison of observed stellar continuum spectra of high-redshift galaxies and mock galaxy spectra generated from hydrodynamical simulations. The mock spectra are produced from the IllustrisTNG TNG100 simulation combined with stellar population models and take into account dust...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Wu, Po-Feng [verfasserIn] Nelson, Dylan [verfasserIn] Wel, Arjen van der [verfasserIn] Pillepich, Annalisa [verfasserIn] Zibetti, Stefano - 1976- [verfasserIn] Bezanson, Rachel [verfasserIn] DEugenio, Francesco [verfasserIn] Gallazzi, Anna - 1978- [verfasserIn] Pacifici, Camilla [verfasserIn] Straatman, Caroline M. S. [verfasserIn] Barišić, Ivana - 1992- [verfasserIn] Bell, Eric F. [verfasserIn] Maseda, Michael V. [verfasserIn] Muzzin, Adam [verfasserIn] Sobral, David [verfasserIn] Whitaker, Katherine E. [verfasserIn] |
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| Format: |
E-Artikel |
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| Sprache: |
Englisch |
| Erschienen: |
2021 October 18 |
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| Anmerkung: |
Gesehen am 10.08.2022 |
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| Umfang: |
14 |
| Übergeordnetes Werk: |
Enthalten in: The astronomical journal - Washington, DC : AAS Publishing, American Astronomical Society, 1998, 162(2021), 5, Artikel-ID 201, Seite 1-14 |
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| Übergeordnetes Werk: |
volume:162 ; year:2021 ; number:5 ; elocationid:201 ; pages:1-14 ; extent:14 |
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| DOI / URN: |
10.3847/1538-3881/ac20d6 |
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| Katalog-ID: |
1810859166 |
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| 100 | 1 | |a Wu, Po-Feng |e verfasserin |0 (DE-588)1251263216 |0 (DE-627)1788678303 |4 aut | |
| 245 | 1 | 0 | |a Toward precise galaxy evolution |b a comparison between spectral Indices of z ∼ 1 galaxies in the IllustrisTNG simulation and the LEGA-C survey |c Po-Feng Wu, Dylan Nelson, Arjen van der Wel, Annalisa Pillepich, Stefano Zibetti, Rachel Bezanson, Francesco DEugenio, Anna Gallazzi, Camilla Pacifici, Caroline M.S. Straatman, Ivana Barišić, Eric F. Bell, Michael V. Maseda, Adam Muzzin, David Sobral, and Katherine E. Whitaker |
| 246 | 3 | 3 | |a Toward precise galaxy evolution$da comparison between spectral Indices of z approximately one galaxies in the IllustrisTNG simulation and the LEGA-C survey |
| 264 | 1 | |c 2021 October 18 | |
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| 520 | |a We present the first comparison of observed stellar continuum spectra of high-redshift galaxies and mock galaxy spectra generated from hydrodynamical simulations. The mock spectra are produced from the IllustrisTNG TNG100 simulation combined with stellar population models and take into account dust attenuation and realistic observational effects (aperture effects and noise). We compare the simulated Dn4000 and EW(Hδ) of galaxies with at 0.6 ≤ z ≤ 1.0 to the observed distributions from the LEGA-C survey. TNG100 globally reproduces the observed distributions of spectral indices, implying that the age distribution of galaxies in TNG100 is generally realistic. Yet there are small but significant differences. For old galaxies, TNG100 shows small Dn4000 when compared to LEGA-C, while LEGA-C galaxies have larger EW(Hδ) at fixed Dn4000 . There are several possible explanations: (1) LEGA-C galaxies have overall older ages combined with small contributions (a few percent in mass) from younger (<1 Gyr) stars, while TNG100 galaxies may not have such young subpopulations; (2) the spectral mismatch could be due to systematic uncertainties in the stellar population models used to convert stellar ages and metallicities to observables. In conclusion, the latest cosmological galaxy-formation simulations broadly reproduce the global age distribution of galaxies at z ∼ 1 and, at the same time, the high quality of the latest observed and simulated data sets help constrain stellar population synthesis models as well as the physical models underlying the simulations. | ||
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10.3847/1538-3881/ac20d6 doi (DE-627)1810859166 (DE-599)KXP1810859166 (OCoLC)1341464260 DE-627 ger DE-627 rda eng Wu, Po-Feng verfasserin (DE-588)1251263216 (DE-627)1788678303 aut Toward precise galaxy evolution a comparison between spectral Indices of z ∼ 1 galaxies in the IllustrisTNG simulation and the LEGA-C survey Po-Feng Wu, Dylan Nelson, Arjen van der Wel, Annalisa Pillepich, Stefano Zibetti, Rachel Bezanson, Francesco DEugenio, Anna Gallazzi, Camilla Pacifici, Caroline M.S. Straatman, Ivana Barišić, Eric F. Bell, Michael V. Maseda, Adam Muzzin, David Sobral, and Katherine E. Whitaker Toward precise galaxy evolution$da comparison between spectral Indices of z approximately one galaxies in the IllustrisTNG simulation and the LEGA-C survey 2021 October 18 14 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Gesehen am 10.08.2022 We present the first comparison of observed stellar continuum spectra of high-redshift galaxies and mock galaxy spectra generated from hydrodynamical simulations. The mock spectra are produced from the IllustrisTNG TNG100 simulation combined with stellar population models and take into account dust attenuation and realistic observational effects (aperture effects and noise). We compare the simulated Dn4000 and EW(Hδ) of galaxies with at 0.6 ≤ z ≤ 1.0 to the observed distributions from the LEGA-C survey. TNG100 globally reproduces the observed distributions of spectral indices, implying that the age distribution of galaxies in TNG100 is generally realistic. Yet there are small but significant differences. For old galaxies, TNG100 shows small Dn4000 when compared to LEGA-C, while LEGA-C galaxies have larger EW(Hδ) at fixed Dn4000 . There are several possible explanations: (1) LEGA-C galaxies have overall older ages combined with small contributions (a few percent in mass) from younger (<1 Gyr) stars, while TNG100 galaxies may not have such young subpopulations; (2) the spectral mismatch could be due to systematic uncertainties in the stellar population models used to convert stellar ages and metallicities to observables. In conclusion, the latest cosmological galaxy-formation simulations broadly reproduce the global age distribution of galaxies at z ∼ 1 and, at the same time, the high quality of the latest observed and simulated data sets help constrain stellar population synthesis models as well as the physical models underlying the simulations. Nelson, Dylan verfasserin (DE-588)115182805X (DE-627)101233600X (DE-576)42382581X aut Wel, Arjen van der verfasserin (DE-588)1139869825 (DE-627)897777638 (DE-576)473002418 aut Pillepich, Annalisa verfasserin (DE-588)1151829854 (DE-627)1012339327 (DE-576)423800841 aut Zibetti, Stefano 1976- verfasserin (DE-588)129777757 (DE-627)479505128 (DE-576)297830767 aut Bezanson, Rachel verfasserin aut DEugenio, Francesco verfasserin aut Gallazzi, Anna 1978- verfasserin (DE-588)132136643 (DE-627)518396401 (DE-576)298964325 aut Pacifici, Camilla verfasserin aut Straatman, Caroline M. S. verfasserin aut Barišić, Ivana 1992- verfasserin (DE-588)1213102537 (DE-627)1703423593 aut Bell, Eric F. verfasserin aut Maseda, Michael V. verfasserin aut Muzzin, Adam verfasserin aut Sobral, David verfasserin aut Whitaker, Katherine E. verfasserin aut Enthalten in The astronomical journal Washington, DC : AAS Publishing, American Astronomical Society, 1998 162(2021), 5, Artikel-ID 201, Seite 1-14 (DE-627)312175647 (DE-600)2003104-X (DE-576)090883306 1538-3881 nnns volume:162 year:2021 number:5 elocationid:201 pages:1-14 extent:14 https://doi.org/10.3847/1538-3881/ac20d6 Verlag Resolving-System lizenzpflichtig 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_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2006 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2110 GBV_ILN_2129 GBV_ILN_2190 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 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 AR 162 2021 5 201 1-14 14 2013 01 DE-16-250 4170240081 00 --%%-- --%%-- --%%-- --%%-- l01 19-07-22 2013 01 DE-16-250 00 s hd2021 2013 01 DE-16-250 01 s (DE-627)1410508463 wissenschaftlicher Artikel (Zeitschrift) 2013 01 DE-16-250 02 s per_16 2013 01 DE-16-250 03 s s_14 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 k (DE-627)1583940421 Exzellenzcluster "STRUKTUREN: Emergenz in Natur, Mathematik und komplexen Daten" 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 k (DE-627)1583940421 Exzellenzcluster "STRUKTUREN: Emergenz in Natur, Mathematik und komplexen Daten" 2013 01 DE-16-250 05 s (DE-627)1410501914 Verfasser 2013 01 DE-16-250 05 s pos_4 |
| spelling |
10.3847/1538-3881/ac20d6 doi (DE-627)1810859166 (DE-599)KXP1810859166 (OCoLC)1341464260 DE-627 ger DE-627 rda eng Wu, Po-Feng verfasserin (DE-588)1251263216 (DE-627)1788678303 aut Toward precise galaxy evolution a comparison between spectral Indices of z ∼ 1 galaxies in the IllustrisTNG simulation and the LEGA-C survey Po-Feng Wu, Dylan Nelson, Arjen van der Wel, Annalisa Pillepich, Stefano Zibetti, Rachel Bezanson, Francesco DEugenio, Anna Gallazzi, Camilla Pacifici, Caroline M.S. Straatman, Ivana Barišić, Eric F. Bell, Michael V. Maseda, Adam Muzzin, David Sobral, and Katherine E. Whitaker Toward precise galaxy evolution$da comparison between spectral Indices of z approximately one galaxies in the IllustrisTNG simulation and the LEGA-C survey 2021 October 18 14 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Gesehen am 10.08.2022 We present the first comparison of observed stellar continuum spectra of high-redshift galaxies and mock galaxy spectra generated from hydrodynamical simulations. The mock spectra are produced from the IllustrisTNG TNG100 simulation combined with stellar population models and take into account dust attenuation and realistic observational effects (aperture effects and noise). We compare the simulated Dn4000 and EW(Hδ) of galaxies with at 0.6 ≤ z ≤ 1.0 to the observed distributions from the LEGA-C survey. TNG100 globally reproduces the observed distributions of spectral indices, implying that the age distribution of galaxies in TNG100 is generally realistic. Yet there are small but significant differences. For old galaxies, TNG100 shows small Dn4000 when compared to LEGA-C, while LEGA-C galaxies have larger EW(Hδ) at fixed Dn4000 . There are several possible explanations: (1) LEGA-C galaxies have overall older ages combined with small contributions (a few percent in mass) from younger (<1 Gyr) stars, while TNG100 galaxies may not have such young subpopulations; (2) the spectral mismatch could be due to systematic uncertainties in the stellar population models used to convert stellar ages and metallicities to observables. In conclusion, the latest cosmological galaxy-formation simulations broadly reproduce the global age distribution of galaxies at z ∼ 1 and, at the same time, the high quality of the latest observed and simulated data sets help constrain stellar population synthesis models as well as the physical models underlying the simulations. Nelson, Dylan verfasserin (DE-588)115182805X (DE-627)101233600X (DE-576)42382581X aut Wel, Arjen van der verfasserin (DE-588)1139869825 (DE-627)897777638 (DE-576)473002418 aut Pillepich, Annalisa verfasserin (DE-588)1151829854 (DE-627)1012339327 (DE-576)423800841 aut Zibetti, Stefano 1976- verfasserin (DE-588)129777757 (DE-627)479505128 (DE-576)297830767 aut Bezanson, Rachel verfasserin aut DEugenio, Francesco verfasserin aut Gallazzi, Anna 1978- verfasserin (DE-588)132136643 (DE-627)518396401 (DE-576)298964325 aut Pacifici, Camilla verfasserin aut Straatman, Caroline M. S. verfasserin aut Barišić, Ivana 1992- verfasserin (DE-588)1213102537 (DE-627)1703423593 aut Bell, Eric F. verfasserin aut Maseda, Michael V. verfasserin aut Muzzin, Adam verfasserin aut Sobral, David verfasserin aut Whitaker, Katherine E. verfasserin aut Enthalten in The astronomical journal Washington, DC : AAS Publishing, American Astronomical Society, 1998 162(2021), 5, Artikel-ID 201, Seite 1-14 (DE-627)312175647 (DE-600)2003104-X (DE-576)090883306 1538-3881 nnns volume:162 year:2021 number:5 elocationid:201 pages:1-14 extent:14 https://doi.org/10.3847/1538-3881/ac20d6 Verlag Resolving-System lizenzpflichtig 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_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2006 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2110 GBV_ILN_2129 GBV_ILN_2190 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 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 AR 162 2021 5 201 1-14 14 2013 01 DE-16-250 4170240081 00 --%%-- --%%-- --%%-- --%%-- l01 19-07-22 2013 01 DE-16-250 00 s hd2021 2013 01 DE-16-250 01 s (DE-627)1410508463 wissenschaftlicher Artikel (Zeitschrift) 2013 01 DE-16-250 02 s per_16 2013 01 DE-16-250 03 s s_14 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 k (DE-627)1583940421 Exzellenzcluster "STRUKTUREN: Emergenz in Natur, Mathematik und komplexen Daten" 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 k (DE-627)1583940421 Exzellenzcluster "STRUKTUREN: Emergenz in Natur, Mathematik und komplexen Daten" 2013 01 DE-16-250 05 s (DE-627)1410501914 Verfasser 2013 01 DE-16-250 05 s pos_4 |
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10.3847/1538-3881/ac20d6 doi (DE-627)1810859166 (DE-599)KXP1810859166 (OCoLC)1341464260 DE-627 ger DE-627 rda eng Wu, Po-Feng verfasserin (DE-588)1251263216 (DE-627)1788678303 aut Toward precise galaxy evolution a comparison between spectral Indices of z ∼ 1 galaxies in the IllustrisTNG simulation and the LEGA-C survey Po-Feng Wu, Dylan Nelson, Arjen van der Wel, Annalisa Pillepich, Stefano Zibetti, Rachel Bezanson, Francesco DEugenio, Anna Gallazzi, Camilla Pacifici, Caroline M.S. Straatman, Ivana Barišić, Eric F. Bell, Michael V. Maseda, Adam Muzzin, David Sobral, and Katherine E. Whitaker Toward precise galaxy evolution$da comparison between spectral Indices of z approximately one galaxies in the IllustrisTNG simulation and the LEGA-C survey 2021 October 18 14 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Gesehen am 10.08.2022 We present the first comparison of observed stellar continuum spectra of high-redshift galaxies and mock galaxy spectra generated from hydrodynamical simulations. The mock spectra are produced from the IllustrisTNG TNG100 simulation combined with stellar population models and take into account dust attenuation and realistic observational effects (aperture effects and noise). We compare the simulated Dn4000 and EW(Hδ) of galaxies with at 0.6 ≤ z ≤ 1.0 to the observed distributions from the LEGA-C survey. TNG100 globally reproduces the observed distributions of spectral indices, implying that the age distribution of galaxies in TNG100 is generally realistic. Yet there are small but significant differences. For old galaxies, TNG100 shows small Dn4000 when compared to LEGA-C, while LEGA-C galaxies have larger EW(Hδ) at fixed Dn4000 . There are several possible explanations: (1) LEGA-C galaxies have overall older ages combined with small contributions (a few percent in mass) from younger (<1 Gyr) stars, while TNG100 galaxies may not have such young subpopulations; (2) the spectral mismatch could be due to systematic uncertainties in the stellar population models used to convert stellar ages and metallicities to observables. In conclusion, the latest cosmological galaxy-formation simulations broadly reproduce the global age distribution of galaxies at z ∼ 1 and, at the same time, the high quality of the latest observed and simulated data sets help constrain stellar population synthesis models as well as the physical models underlying the simulations. Nelson, Dylan verfasserin (DE-588)115182805X (DE-627)101233600X (DE-576)42382581X aut Wel, Arjen van der verfasserin (DE-588)1139869825 (DE-627)897777638 (DE-576)473002418 aut Pillepich, Annalisa verfasserin (DE-588)1151829854 (DE-627)1012339327 (DE-576)423800841 aut Zibetti, Stefano 1976- verfasserin (DE-588)129777757 (DE-627)479505128 (DE-576)297830767 aut Bezanson, Rachel verfasserin aut DEugenio, Francesco verfasserin aut Gallazzi, Anna 1978- verfasserin (DE-588)132136643 (DE-627)518396401 (DE-576)298964325 aut Pacifici, Camilla verfasserin aut Straatman, Caroline M. S. verfasserin aut Barišić, Ivana 1992- verfasserin (DE-588)1213102537 (DE-627)1703423593 aut Bell, Eric F. verfasserin aut Maseda, Michael V. verfasserin aut Muzzin, Adam verfasserin aut Sobral, David verfasserin aut Whitaker, Katherine E. verfasserin aut Enthalten in The astronomical journal Washington, DC : AAS Publishing, American Astronomical Society, 1998 162(2021), 5, Artikel-ID 201, Seite 1-14 (DE-627)312175647 (DE-600)2003104-X (DE-576)090883306 1538-3881 nnns volume:162 year:2021 number:5 elocationid:201 pages:1-14 extent:14 https://doi.org/10.3847/1538-3881/ac20d6 Verlag Resolving-System lizenzpflichtig 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_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2006 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2110 GBV_ILN_2129 GBV_ILN_2190 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 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 AR 162 2021 5 201 1-14 14 2013 01 DE-16-250 4170240081 00 --%%-- --%%-- --%%-- --%%-- l01 19-07-22 2013 01 DE-16-250 00 s hd2021 2013 01 DE-16-250 01 s (DE-627)1410508463 wissenschaftlicher Artikel (Zeitschrift) 2013 01 DE-16-250 02 s per_16 2013 01 DE-16-250 03 s s_14 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 k (DE-627)1583940421 Exzellenzcluster "STRUKTUREN: Emergenz in Natur, Mathematik und komplexen Daten" 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 k (DE-627)1583940421 Exzellenzcluster "STRUKTUREN: Emergenz in Natur, Mathematik und komplexen Daten" 2013 01 DE-16-250 05 s (DE-627)1410501914 Verfasser 2013 01 DE-16-250 05 s pos_4 |
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10.3847/1538-3881/ac20d6 doi (DE-627)1810859166 (DE-599)KXP1810859166 (OCoLC)1341464260 DE-627 ger DE-627 rda eng Wu, Po-Feng verfasserin (DE-588)1251263216 (DE-627)1788678303 aut Toward precise galaxy evolution a comparison between spectral Indices of z ∼ 1 galaxies in the IllustrisTNG simulation and the LEGA-C survey Po-Feng Wu, Dylan Nelson, Arjen van der Wel, Annalisa Pillepich, Stefano Zibetti, Rachel Bezanson, Francesco DEugenio, Anna Gallazzi, Camilla Pacifici, Caroline M.S. Straatman, Ivana Barišić, Eric F. Bell, Michael V. Maseda, Adam Muzzin, David Sobral, and Katherine E. Whitaker Toward precise galaxy evolution$da comparison between spectral Indices of z approximately one galaxies in the IllustrisTNG simulation and the LEGA-C survey 2021 October 18 14 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Gesehen am 10.08.2022 We present the first comparison of observed stellar continuum spectra of high-redshift galaxies and mock galaxy spectra generated from hydrodynamical simulations. The mock spectra are produced from the IllustrisTNG TNG100 simulation combined with stellar population models and take into account dust attenuation and realistic observational effects (aperture effects and noise). We compare the simulated Dn4000 and EW(Hδ) of galaxies with at 0.6 ≤ z ≤ 1.0 to the observed distributions from the LEGA-C survey. TNG100 globally reproduces the observed distributions of spectral indices, implying that the age distribution of galaxies in TNG100 is generally realistic. Yet there are small but significant differences. For old galaxies, TNG100 shows small Dn4000 when compared to LEGA-C, while LEGA-C galaxies have larger EW(Hδ) at fixed Dn4000 . There are several possible explanations: (1) LEGA-C galaxies have overall older ages combined with small contributions (a few percent in mass) from younger (<1 Gyr) stars, while TNG100 galaxies may not have such young subpopulations; (2) the spectral mismatch could be due to systematic uncertainties in the stellar population models used to convert stellar ages and metallicities to observables. In conclusion, the latest cosmological galaxy-formation simulations broadly reproduce the global age distribution of galaxies at z ∼ 1 and, at the same time, the high quality of the latest observed and simulated data sets help constrain stellar population synthesis models as well as the physical models underlying the simulations. Nelson, Dylan verfasserin (DE-588)115182805X (DE-627)101233600X (DE-576)42382581X aut Wel, Arjen van der verfasserin (DE-588)1139869825 (DE-627)897777638 (DE-576)473002418 aut Pillepich, Annalisa verfasserin (DE-588)1151829854 (DE-627)1012339327 (DE-576)423800841 aut Zibetti, Stefano 1976- verfasserin (DE-588)129777757 (DE-627)479505128 (DE-576)297830767 aut Bezanson, Rachel verfasserin aut DEugenio, Francesco verfasserin aut Gallazzi, Anna 1978- verfasserin (DE-588)132136643 (DE-627)518396401 (DE-576)298964325 aut Pacifici, Camilla verfasserin aut Straatman, Caroline M. S. verfasserin aut Barišić, Ivana 1992- verfasserin (DE-588)1213102537 (DE-627)1703423593 aut Bell, Eric F. verfasserin aut Maseda, Michael V. verfasserin aut Muzzin, Adam verfasserin aut Sobral, David verfasserin aut Whitaker, Katherine E. verfasserin aut Enthalten in The astronomical journal Washington, DC : AAS Publishing, American Astronomical Society, 1998 162(2021), 5, Artikel-ID 201, Seite 1-14 (DE-627)312175647 (DE-600)2003104-X (DE-576)090883306 1538-3881 nnns volume:162 year:2021 number:5 elocationid:201 pages:1-14 extent:14 https://doi.org/10.3847/1538-3881/ac20d6 Verlag Resolving-System lizenzpflichtig 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_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2006 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2110 GBV_ILN_2129 GBV_ILN_2190 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 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 AR 162 2021 5 201 1-14 14 2013 01 DE-16-250 4170240081 00 --%%-- --%%-- --%%-- --%%-- l01 19-07-22 2013 01 DE-16-250 00 s hd2021 2013 01 DE-16-250 01 s (DE-627)1410508463 wissenschaftlicher Artikel (Zeitschrift) 2013 01 DE-16-250 02 s per_16 2013 01 DE-16-250 03 s s_14 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 k (DE-627)1583940421 Exzellenzcluster "STRUKTUREN: Emergenz in Natur, Mathematik und komplexen Daten" 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 k (DE-627)1583940421 Exzellenzcluster "STRUKTUREN: Emergenz in Natur, Mathematik und komplexen Daten" 2013 01 DE-16-250 05 s (DE-627)1410501914 Verfasser 2013 01 DE-16-250 05 s pos_4 |
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10.3847/1538-3881/ac20d6 doi (DE-627)1810859166 (DE-599)KXP1810859166 (OCoLC)1341464260 DE-627 ger DE-627 rda eng Wu, Po-Feng verfasserin (DE-588)1251263216 (DE-627)1788678303 aut Toward precise galaxy evolution a comparison between spectral Indices of z ∼ 1 galaxies in the IllustrisTNG simulation and the LEGA-C survey Po-Feng Wu, Dylan Nelson, Arjen van der Wel, Annalisa Pillepich, Stefano Zibetti, Rachel Bezanson, Francesco DEugenio, Anna Gallazzi, Camilla Pacifici, Caroline M.S. Straatman, Ivana Barišić, Eric F. Bell, Michael V. Maseda, Adam Muzzin, David Sobral, and Katherine E. Whitaker Toward precise galaxy evolution$da comparison between spectral Indices of z approximately one galaxies in the IllustrisTNG simulation and the LEGA-C survey 2021 October 18 14 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Gesehen am 10.08.2022 We present the first comparison of observed stellar continuum spectra of high-redshift galaxies and mock galaxy spectra generated from hydrodynamical simulations. The mock spectra are produced from the IllustrisTNG TNG100 simulation combined with stellar population models and take into account dust attenuation and realistic observational effects (aperture effects and noise). We compare the simulated Dn4000 and EW(Hδ) of galaxies with at 0.6 ≤ z ≤ 1.0 to the observed distributions from the LEGA-C survey. TNG100 globally reproduces the observed distributions of spectral indices, implying that the age distribution of galaxies in TNG100 is generally realistic. Yet there are small but significant differences. For old galaxies, TNG100 shows small Dn4000 when compared to LEGA-C, while LEGA-C galaxies have larger EW(Hδ) at fixed Dn4000 . There are several possible explanations: (1) LEGA-C galaxies have overall older ages combined with small contributions (a few percent in mass) from younger (<1 Gyr) stars, while TNG100 galaxies may not have such young subpopulations; (2) the spectral mismatch could be due to systematic uncertainties in the stellar population models used to convert stellar ages and metallicities to observables. In conclusion, the latest cosmological galaxy-formation simulations broadly reproduce the global age distribution of galaxies at z ∼ 1 and, at the same time, the high quality of the latest observed and simulated data sets help constrain stellar population synthesis models as well as the physical models underlying the simulations. Nelson, Dylan verfasserin (DE-588)115182805X (DE-627)101233600X (DE-576)42382581X aut Wel, Arjen van der verfasserin (DE-588)1139869825 (DE-627)897777638 (DE-576)473002418 aut Pillepich, Annalisa verfasserin (DE-588)1151829854 (DE-627)1012339327 (DE-576)423800841 aut Zibetti, Stefano 1976- verfasserin (DE-588)129777757 (DE-627)479505128 (DE-576)297830767 aut Bezanson, Rachel verfasserin aut DEugenio, Francesco verfasserin aut Gallazzi, Anna 1978- verfasserin (DE-588)132136643 (DE-627)518396401 (DE-576)298964325 aut Pacifici, Camilla verfasserin aut Straatman, Caroline M. S. verfasserin aut Barišić, Ivana 1992- verfasserin (DE-588)1213102537 (DE-627)1703423593 aut Bell, Eric F. verfasserin aut Maseda, Michael V. verfasserin aut Muzzin, Adam verfasserin aut Sobral, David verfasserin aut Whitaker, Katherine E. verfasserin aut Enthalten in The astronomical journal Washington, DC : AAS Publishing, American Astronomical Society, 1998 162(2021), 5, Artikel-ID 201, Seite 1-14 (DE-627)312175647 (DE-600)2003104-X (DE-576)090883306 1538-3881 nnns volume:162 year:2021 number:5 elocationid:201 pages:1-14 extent:14 https://doi.org/10.3847/1538-3881/ac20d6 Verlag Resolving-System lizenzpflichtig 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_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2006 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2110 GBV_ILN_2129 GBV_ILN_2190 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 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 AR 162 2021 5 201 1-14 14 2013 01 DE-16-250 4170240081 00 --%%-- --%%-- --%%-- --%%-- l01 19-07-22 2013 01 DE-16-250 00 s hd2021 2013 01 DE-16-250 01 s (DE-627)1410508463 wissenschaftlicher Artikel (Zeitschrift) 2013 01 DE-16-250 02 s per_16 2013 01 DE-16-250 03 s s_14 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 k (DE-627)1583940421 Exzellenzcluster "STRUKTUREN: Emergenz in Natur, Mathematik und komplexen Daten" 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 k (DE-627)1583940421 Exzellenzcluster "STRUKTUREN: Emergenz in Natur, Mathematik und komplexen Daten" 2013 01 DE-16-250 05 s (DE-627)1410501914 Verfasser 2013 01 DE-16-250 05 s pos_4 |
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Wu, Po-Feng @@aut@@ Nelson, Dylan @@aut@@ Wel, Arjen van der @@aut@@ Pillepich, Annalisa @@aut@@ Zibetti, Stefano @@aut@@ Bezanson, Rachel @@aut@@ DEugenio, Francesco @@aut@@ Gallazzi, Anna @@aut@@ Pacifici, Camilla @@aut@@ Straatman, Caroline M. S. @@aut@@ Barišić, Ivana @@aut@@ Bell, Eric F. @@aut@@ Maseda, Michael V. @@aut@@ Muzzin, Adam @@aut@@ Sobral, David @@aut@@ Whitaker, Katherine E. @@aut@@ |
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The mock spectra are produced from the IllustrisTNG TNG100 simulation combined with stellar population models and take into account dust attenuation and realistic observational effects (aperture effects and noise). We compare the simulated Dn4000 and EW(Hδ) of galaxies with at 0.6 ≤ z ≤ 1.0 to the observed distributions from the LEGA-C survey. TNG100 globally reproduces the observed distributions of spectral indices, implying that the age distribution of galaxies in TNG100 is generally realistic. Yet there are small but significant differences. For old galaxies, TNG100 shows small Dn4000 when compared to LEGA-C, while LEGA-C galaxies have larger EW(Hδ) at fixed Dn4000 . There are several possible explanations: (1) LEGA-C galaxies have overall older ages combined with small contributions (a few percent in mass) from younger (<1 Gyr) stars, while TNG100 galaxies may not have such young subpopulations; (2) the spectral mismatch could be due to systematic uncertainties in the stellar population models used to convert stellar ages and metallicities to observables. 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Elektronische Aufsätze |
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Wu, Po-Feng |
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a comparison between spectral Indices of z ∼ 1 galaxies in the IllustrisTNG simulation and the LEGA-C survey |
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verfasserin |
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toward precise galaxy evolutiona comparison between spectral indices of z ∼ 1 galaxies in the illustristng simulation and the lega-c survey |
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Toward precise galaxy evolution a comparison between spectral Indices of z ∼ 1 galaxies in the IllustrisTNG simulation and the LEGA-C survey |
| abstract |
We present the first comparison of observed stellar continuum spectra of high-redshift galaxies and mock galaxy spectra generated from hydrodynamical simulations. The mock spectra are produced from the IllustrisTNG TNG100 simulation combined with stellar population models and take into account dust attenuation and realistic observational effects (aperture effects and noise). We compare the simulated Dn4000 and EW(Hδ) of galaxies with at 0.6 ≤ z ≤ 1.0 to the observed distributions from the LEGA-C survey. TNG100 globally reproduces the observed distributions of spectral indices, implying that the age distribution of galaxies in TNG100 is generally realistic. Yet there are small but significant differences. For old galaxies, TNG100 shows small Dn4000 when compared to LEGA-C, while LEGA-C galaxies have larger EW(Hδ) at fixed Dn4000 . There are several possible explanations: (1) LEGA-C galaxies have overall older ages combined with small contributions (a few percent in mass) from younger (<1 Gyr) stars, while TNG100 galaxies may not have such young subpopulations; (2) the spectral mismatch could be due to systematic uncertainties in the stellar population models used to convert stellar ages and metallicities to observables. In conclusion, the latest cosmological galaxy-formation simulations broadly reproduce the global age distribution of galaxies at z ∼ 1 and, at the same time, the high quality of the latest observed and simulated data sets help constrain stellar population synthesis models as well as the physical models underlying the simulations. Gesehen am 10.08.2022 |
| abstractGer |
We present the first comparison of observed stellar continuum spectra of high-redshift galaxies and mock galaxy spectra generated from hydrodynamical simulations. The mock spectra are produced from the IllustrisTNG TNG100 simulation combined with stellar population models and take into account dust attenuation and realistic observational effects (aperture effects and noise). We compare the simulated Dn4000 and EW(Hδ) of galaxies with at 0.6 ≤ z ≤ 1.0 to the observed distributions from the LEGA-C survey. TNG100 globally reproduces the observed distributions of spectral indices, implying that the age distribution of galaxies in TNG100 is generally realistic. Yet there are small but significant differences. For old galaxies, TNG100 shows small Dn4000 when compared to LEGA-C, while LEGA-C galaxies have larger EW(Hδ) at fixed Dn4000 . There are several possible explanations: (1) LEGA-C galaxies have overall older ages combined with small contributions (a few percent in mass) from younger (<1 Gyr) stars, while TNG100 galaxies may not have such young subpopulations; (2) the spectral mismatch could be due to systematic uncertainties in the stellar population models used to convert stellar ages and metallicities to observables. In conclusion, the latest cosmological galaxy-formation simulations broadly reproduce the global age distribution of galaxies at z ∼ 1 and, at the same time, the high quality of the latest observed and simulated data sets help constrain stellar population synthesis models as well as the physical models underlying the simulations. Gesehen am 10.08.2022 |
| abstract_unstemmed |
We present the first comparison of observed stellar continuum spectra of high-redshift galaxies and mock galaxy spectra generated from hydrodynamical simulations. The mock spectra are produced from the IllustrisTNG TNG100 simulation combined with stellar population models and take into account dust attenuation and realistic observational effects (aperture effects and noise). We compare the simulated Dn4000 and EW(Hδ) of galaxies with at 0.6 ≤ z ≤ 1.0 to the observed distributions from the LEGA-C survey. TNG100 globally reproduces the observed distributions of spectral indices, implying that the age distribution of galaxies in TNG100 is generally realistic. Yet there are small but significant differences. For old galaxies, TNG100 shows small Dn4000 when compared to LEGA-C, while LEGA-C galaxies have larger EW(Hδ) at fixed Dn4000 . There are several possible explanations: (1) LEGA-C galaxies have overall older ages combined with small contributions (a few percent in mass) from younger (<1 Gyr) stars, while TNG100 galaxies may not have such young subpopulations; (2) the spectral mismatch could be due to systematic uncertainties in the stellar population models used to convert stellar ages and metallicities to observables. In conclusion, the latest cosmological galaxy-formation simulations broadly reproduce the global age distribution of galaxies at z ∼ 1 and, at the same time, the high quality of the latest observed and simulated data sets help constrain stellar population synthesis models as well as the physical models underlying the simulations. Gesehen am 10.08.2022 |
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Toward precise galaxy evolution |
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