Dust attenuation in galaxies at cosmic dawn from the FirstLight simulations

被引：6

作者：

Mushtaq, Muzammil ^{[1
]}

Ceverino, Daniel ^{[2
,3
]}

Klessen, Ralf S. ^{[1
,4
]}

Reissl, Stefan ^{[1
]}

Puttasiddappa, Prajwal Hassan ^{[5
,6
]}

机构：

[1] Heidelberg Univ, Zentrum Astron, Albert Ueberle Str 2, D-69120 Heidelberg, Germany

[2] Univ Autonoma Madrid, Fac Ciencias, Dept Fis Teor Modulo 8, E-28049 Madrid, Spain

[3] Univ Autonoma Madrid, Fac Ciencias, CIAFF, E-28049 Madrid, Spain

[4] Heidelberg Univ, Interdisziplinares Zent Wissenschaftl Rechnen, INF 205, D-69120 Heidelberg, Germany

[5] Heidelberg Univ, Inst Theoret Phys, Philosophenweg 16, D-69120 Heidelberg, Germany

[6] Univ Fed Espirito Santo, PPGCosmo, BR-29075910 Vitoria, ES, Brazil

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2023年 / 525卷 / 04期

基金：

欧洲研究理事会;

关键词：

galaxies: evolution; galaxies: formation; galaxies: high-redshift; STAR-FORMING GALAXIES; HIGH-REDSHIFT; UV ATTENUATION; 1ST STARS; TO; EVOLUTION; ULTRAVIOLET; EXTINCTION; FEEDBACK; METALLICITY;

D O I：

10.1093/mnras/stad2602

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We study the behaviour of dust in galaxies at cosmic dawn, z = 6-8, by coupling the FirstLight simulations with the radiative transfer code POLARIS. The starburst nature of these galaxies and their complex distribution of dust lead to a large diversity of attenuation curves. These follow the Calzetti model only for relatively massive galaxies, M-stars similar or equal to 10(9) M-circle dot. Galaxies with lower masses have steeper curves, consistent with the model for the Small Magellanic Cloud. The ultraviolet and optical slopes of the attenuation curves are closer to the modified Calzetti model, with a slight preference for the power-law model for galaxies with the highest values of attenuation. We have also examined the relation between the slope in the far-ultraviolet, beta(UV), and the infrared excess, IRX. At z = 6, it follows the Calzetti model with a shift to slightly lower beta(UV) values due to lower metallicities at lower attenuation. The same relation at z = 8 shows a shift to higher IRX values due to a stronger CMB radiation at high z.

引用

页码：4976 / 4984

页数：9

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