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Verfasst von:Shen, Xuejian [VerfasserIn]   i
 Vogelsberger, Mark [VerfasserIn]   i
 Nelson, Dylan [VerfasserIn]   i
 Pillepich, Annalisa [VerfasserIn]   i
 Tacchella, Sandro [VerfasserIn]   i
 Marinacci, Federico [VerfasserIn]   i
 Torrey, Paul [VerfasserIn]   i
 Hernquist, Lars [VerfasserIn]   i
 Springel, Volker [VerfasserIn]   i
Titel:High-redshift JWST predictions from IllustrisTNG
Titelzusatz:II. Galaxy line and continuum spectral indices and dust attenuation curves
Verf.angabe:Xuejian Shen, Mark Vogelsberger, Dylan Nelson, Annalisa Pillepich, Sandro Tacchella, Federico Marinacci, Paul Torrey, Lars Hernquist and Volker Springel
E-Jahr:2020
Jahr:2020 May 22
Umfang:22 S.
Fussnoten:Gesehen am 10.08.2022
Titel Quelle:Enthalten in: Royal Astronomical SocietyMonthly notices of the Royal Astronomical Society
Ort Quelle:Oxford : Oxford Univ. Press, 1827
Jahr Quelle:2020
Band/Heft Quelle:495(2020), 4, Seite 4747-4768
ISSN Quelle:1365-2966
Abstract:We present predictions for high redshift (z = 2−10) galaxy populations based on the IllustrisTNG simulation suite and a full Monte Carlo dust radiative transfer post-processing. Specifically, we discuss the H α and H β + $[\rm O \,{\small III}]$ luminosity functions up to z = 8. The predicted H β + $[\rm O \,{\small III}]$ luminosity functions are consistent with present observations at z ≲ 3 with ${\lesssim} 0.1\, {\rm dex}$ differences in luminosities. However, the predicted H α luminosity function is ${\sim }0.3\, {\rm dex}$ dimmer than the observed one at z ≃ 2. Furthermore, we explore continuum spectral indices, the Balmer break at 4000 Å; (D4000) and the UV continuum slope β. The median D4000 versus specific star formation rate relation predicted at z = 2 is in agreement with the local calibration despite a different distribution pattern of galaxies in this plane. In addition, we reproduce the observed AUV versus β relation and explore its dependence on galaxy stellar mass, providing an explanation for the observed complexity of this relation. We also find a deficiency in heavily attenuated, UV red galaxies in the simulations. Finally, we provide predictions for the dust attenuation curves of galaxies at z = 2−6 and investigate their dependence on galaxy colours and stellar masses. The attenuation curves are steeper in galaxies at higher redshifts, with bluer colours, or with lower stellar masses. We attribute these predicted trends to dust geometry. Overall, our results are consistent with present observations of high-redshift galaxies. Future James Webb Space Telecope observations will further test these predictions.
DOI:doi:10.1093/mnras/staa1423
URL:Bitte beachten Sie: Dies ist ein Bibliographieeintrag. Ein Volltextzugriff für Mitglieder der Universität besteht hier nur, falls für die entsprechende Zeitschrift/den entsprechenden Sammelband ein Abonnement besteht oder es sich um einen OpenAccess-Titel handelt.

Volltext: https://doi.org/10.1093/mnras/staa1423
 DOI: https://doi.org/10.1093/mnras/staa1423
Datenträger:Online-Ressource
Sprache:eng
K10plus-PPN:1810864720
Verknüpfungen:→ Zeitschrift

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