First Light: exploring the Spectra of High-Redshift Galaxies in the Renaissance Simulations
First Light: exploring the Spectra of High-Redshift Galaxies in the Renaissance Simulations
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第一缕曙光：探索文艺复兴模拟中的高红移星系光谱
DOI：
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发表时间：
2017
期刊：
影响因子：
--
通讯作者：
Haoting Xu
中科院分区：
文献类型：
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作者：
Kirk S. S. Barrow;J. Wise;M. Norman;B. O’Shea;Haoting Xu
我们提出了宇宙中第一代星系的综合观测，并对未来红移大于6的深场观测进行了预测。由于星云发射线的强烈影响和HII区域相对紧凑的尺度，需要高分辨率的宇宙学模拟和一套强大的分析工具来正确模拟光谱。我们创建了一个由FSPS，Cloudy，Cloudy和我们自己的工具组成的软件管道，用于从气体，尘埃和恒星的完全三维排列中生成合成IR观测。我们的处方使我们能够包括完整化学网络的发射线，并解决各种视线中灰尘消光和散射的影响。我们提供光谱，2-D合并的光子图像HST和JWST红外滤波器，光度关系，和发射线强度的一个大样本的高红移星系在文艺复兴时期的模拟。我们得到的合成光谱显示星系晕之间的高度可变性与恒星质量，金属丰度，气体质量分数和形成历史的强烈依赖。恒星质量最低的晕在[OIII]/H$\beta$、[OIII]和CIII]方面具有最大的变化性，而质量较高的晕在其光谱和[OIII]等效宽度（EW）方面表现出一致性，介于1\AA\和10\AA之间。视角占三倍的流量差异，由于电离气体通道中的晕的存在。此外，JWST颜色图显示了红移，颜色和平均恒星年龄之间的明显关系。
We present synthetic observations for the first generations of galaxies in the Universe and make predictions for future deep field observations for redshifts greater than 6. Due to the strong impact of nebular emission lines and the relatively compact scale of HII regions, high resolution cosmological simulations and a robust suite of analysis tools are required to properly simulate spectra. We created a software pipeline consisting of FSPS, Hyperion, Cloudy and our own tools to generate synthetic IR observations from a fully three-dimensional arrangement of gas, dust, and stars. Our prescription allows us to include emission lines for a complete chemical network and tackle the effect of dust extinction and scattering in the various lines of sight. We provide spectra, 2-D binned photon imagery for both HST and JWST IR filters, luminosity relationships, and emission line strengths for a large sample of high redshift galaxies in the Renaissance Simulations. Our resulting synthetic spectra show high variability between galactic halos with a strong dependence on stellar mass, metallicity, gas mass fraction, and formation history. Halos with the lowest stellar mass have the greatest variability in [OIII]/H$\beta$, [OIII] and CIII] while halos with higher masses are seen to show consistency in their spectra and [OIII] equivalent widths (EW) between 1\AA\ and 10\AA. Viewing angle accounted for three-fold difference in flux due to the presence of ionized gas channels in a halo. Furthermore, JWST color plots show a discernible relationship between redshift, color, and mean stellar age.
DOI：
10.3847/1538-4357/833/2/201
发表时间：
2016-06
期刊：
The Astrophysical Journal
影响因子：
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作者：
K. Seon;B. Draine
通讯作者：
K. Seon;B. Draine