REBELS-IFU: dust attenuation curves of 12 massive galaxies at z ≃ 7

被引：3

作者：

Fisher, R. ^{[1
]}

Bowler, R. A. A. ^{[1
]}

Stefanon, M. ^{[2
,3
]}

Rowland, L. E. ^{[4
]}

Algera, H. S. B. ^{[5
,6
,7
]}

Aravena, M. ^{[8
]}

Bouwens, R.

Dayal, P. ^{[9
]}

Ferrara, A. ^{[10
]}

Fudamoto, Y. ^{[11
,12
]}

Gulis, C. ^{[13
]}

Hodge, J. A. ^{[4
]}

Inami, H. ^{[6
]}

Ormerod, K. ^{[14
]}

Pallottini, A. ^{[10
]}

Phillips, S. G. ^{[14
]}

Sartorio, N. S. ^{[15
]}

Schouws, S. ^{[4
]}

Smit, R. ^{[14
]}

Sommovigo, L. ^{[16
]}

Stark, D. P. ^{[12
]}

van der Werf, P. P. ^{[4
]}

机构：

[1] Univ Manchester, Jodrell Bank Ctr Astrophys, Oxford Rd, Manchester M13 9PL, England

[2] Univ Valencia, Dept Astron & Astrofis, C Dr Moliner 50, E-46100 Valencia, Spain

[3] Univ Valencia, Unidad Asociada CSIC Grp Astrofis Extragalact & Co, Instituto Fis Cantabria, Valencia, Spain

[4] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands

[5] Acad Sinica, Inst Astron & Astrophys, 11F Astron Math Bldg 1,Sect 4,Roosevelt Rd, Taipei 106216, Taiwan

[6] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, 1-3-1 Kagamiyama, Higashihiroshima, Hiroshima 7398526, Japan

[7] Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo, Japan

[8] Univ Diego Portales, Fac Ingn & Ciencias, Inst Estudios Astrofis, Ave Ejercito 441, Santiago, Chile

[9] Univ Groningen, Kapteyn Astron Inst, POB 800, NL-9700 AV Groningen, Netherlands

[10] Scuola Normale Super Pisa, Piazza Cavalieri 7, I-56126 Pisa, Italy

[11] Chiba Univ, Ctr Frontier Sci, 1-33 Yayoi Cho,Inage Ku, Chiba 2638522, Japan

[12] Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA

[13] Penn State Univ, Dept Astron, Davey Lab 525, University Pk, PA 16802 USA

[14] Liverpool John Moores Univ, Astrophys Res Inst, 146 Brownlow Hill, Liverpool L3 5RF, England

[15] Sterrenkundig Observ, Krijgslaan 281-S9, B-9000 Ghent, Belgium

[16] Flatiron Inst, Ctr Computat Astrophys, 162 5th Ave, New York, NY 10010 USA

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2025年 / 539卷 / 01期

基金：

欧盟地平线“2020”; 比利时弗兰德研究基金会;

关键词：

dust; extinction; galaxies: high-redshift; STAR-FORMING GALAXIES; 1ST BILLION YEARS; SMALL-MAGELLANIC-CLOUD; UV-CONTINUUM SLOPES; HIGH-REDSHIFT; MOSDEF SURVEY; STELLAR MASS; EXTINCTION CURVES; C II; INTERSTELLAR-MEDIUM;

D O I：

10.1093/mnras/staf485

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present measurements of the dust attenuation curves of 12 massive (9 < log(M-star/M-circle dot) < 10) Lyman-break galaxies at z = 6.5-7.7 derived from JWST NIRSpec integral field unit spectroscopy. The galaxies are drawn from the Atacama Large Millimeter/submillimeter Array Reionization Era Bright Emission Line Survey (REBELS) large program. The dust attenuation curves were obtained by fitting spectral energy distribution (SED) models with a flexible dust attenuation curve to the full galaxy spectra over observed wavelengths 0.6-5.3 mu m. These attenuation curves show a range of recovered slopes (-0.41 <= delta <= 0.09) that are on average slightly flatter than seen in local sources of the same stellar masses, with none exhibiting very steep slopes. Three galaxies exhibit evidence for a 2175 & Aring; dust bump (>4 sigma) and we find that SED fitting excluding the bump can overestimate derived stellar masses by up to 0.4 dex. Correcting for the dust attenuation with our best-fitting attenuation curves, we recover a range of intrinsic ultraviolet slopes (-2.4 < beta(0 )< -2.0). The galaxies show moderate reddening (A(V, stellar) = 0.1-0.6 mag) and the A(V, stellar) to stellar mass relation is consistent with local sources. The attenuation curve slope is found to correlate with A(V, stellar), while we see no strong correlation with stellar mass, M-UV, or gas-phase metallicity. Overall, our results show little evolution in dust properties in the REBELS sources compared to the local Universe. Comparing our recovered trends to empirical models suggests that the most important factor driving the variation in the attenuation curves in our sample is the dust-star geometry, not the properties of the dust grains themselves.

引用

页码：109 / 126

页数：18

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