Dust attenuation in galaxies up to redshift ≃ 2
Dust attenuation in galaxies up to redshift ≃ 2
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星系中的尘埃衰减高达红移 ≃ 2
DOI：
10.5047/eps.2013.02.001
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发表时间：
2013
期刊：
影响因子：
--
通讯作者：
V. Buat
中科院分区：
文献类型：
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作者：
V. Buat
我们想要研究高红移条件下紫外线 (UV) 波长的尘埃衰减，其中紫外线红移到观察到的可见光波长范围。特别是，我们在 2175 Å 处寻找凸点。我们使用 MUSYC 项目在中频和宽带滤光片中获得的钱德拉深场南 (CDFS) 光度数据，对 751 个 0.95 < z < 2.2 星系的 UV 静止框架进行采样。如果可用，来自 GOODS-Herschel 项目的红外 (IR) Herschel/PACS* 数据与 Spitzer/MIPS 测量相结合，用于估计粉尘排放并限制粉尘衰减。使用 CIGALE 代码† 拟合每个光源的光谱能量分布。我们的样本星系的平均衰减曲线显示出一个 UV 凸起，其幅度与在 LMC 超壳层区域的消光曲线中观察到的相似。发现紫外波长处的平均衰减曲线的斜率比局部星暴星系的斜率更陡。研究发现，紫外线波长下的尘埃衰减量随着恒星质量的增加而增加，并随着紫外线光度的增加而减少。
We want to study dust attenuation at ultraviolet (UV) wavelengths at high redshift, where the UV is redshifted to the observed visible light wavelength range. In particular, we search for a bump at 2175 Å. We use photometric data in the Chandra Deep Field South (CDFS), obtained in intermediate and broad band filters by the MUSYC project, to sample the UV rest-frame of 751 galaxies with 0.95 < z < 2.2. When available, infrared (IR) Herschel/PACS* data from the GOODS-Herschel project, coupled with Spitzer/MIPS measurements, are used to estimate the dust emission and to constrain dust attenuation. The spectral energy distribution of each source is fit using the CIGALE code†. The average attenuation curve found for our sample galaxies exhibits a UV bump whose amplitude is similar to that observed in the extinction curve of the LMC super-shell region. The slope of the average attenuation curve at UV wavelength is found steeper than that for local starburst galaxies. The amount of dust attenuation at UV wavelengths is found to increase with stellar mass and to decrease as UV luminosity increases.