论文标题
以低于MM颜色的4 $ <$ <$ <$ <$ <$ <$ <$ <6 $ <$ 6的大宽度星系识别
Identification of Large Equivalent Width Dusty Galaxies at 4 $<$ z $<$ 6 from Sub-mm Colours
论文作者
论文摘要
红外线（IR），亚毫米计（sub-mm）和毫米（mm）数据库包含大量高质量数据。但是，这些数据的很大一部分是光度法，并且被认为对于得出有关星系中的卵形发射的定量信息并不有用。该项目的目的是首先在Z> 4-6处识别星系，并在其亚MM颜色的电离时期内识别星系。我们还旨在表明颜色可用于在计算IR精细结构线对这些光度波段的贡献时，可以从光度带中尝试并从光度带中得出物理约束。我们用云层对红外良好结构线的通量进行建模，并用雪茄添加到灰尘连续发射中。模拟光谱能分布（SED）中的发射线（包括或不包括发射线）会修饰宽带的发射和颜色。线的引入允许从log10（psw_250um/pmw_350um）与log10（laboca_870um/plw_500um）颜色彩色图表识别z> 4-6的强星形成星系。通过将相关模型与每个观察到的星系颜色进行比较，我们能够大致估计线的通量和相关的nebular参数。该方法允许在从电离参数和气体金属性构建的图中识别双序列。 HII和光电分离区（PDR）良好的结构线是SED的重要组成部分。在对光谱进行建模时，尤其是在z> 4-6时添加它们很重要，其中它们的等效宽度可能很大。相反，我们表明我们可以提取有关强IR精细结构线的一些信息以及与IR颜色颜色图的纯净发射有关的物理参数。
Infrared (IR), sub-millimetre (sub-mm) and millimetre (mm) databases contain a huge quantity of high quality data. However, a large part of these data are photometric, and are thought not to be useful to derive a quantitative information on the nebular emission of galaxies. The aim of this project is first to identify galaxies at z > 4-6, and in the epoch of reionization from their sub-mm colours. We also aim at showing that the colours can be used to try and derive physical constraints from photometric bands, when accounting for the contribution from the IR fine structure lines to these photometric bands. We model the flux of IR fine structure lines with CLOUDY, and add them to the dust continuum emission with CIGALE. Including or not emission lines in the simulated spectral energy distribution (SED) modifies the broad band emission and colours. The introduction of the lines allows to identify strong star forming galaxies at z > 4 - 6 from the log10 (PSW_250um/PMW_350um) versus log10 (LABOCA_870um/PLW_500um) colour-colour diagramme. By comparing the relevant models to each observed galaxy colour, we are able to roughly estimate the fluxes of the lines, and the associated nebular parameters. This method allows to identify a double sequence in a plot built from the ionization parameter and the gas metallicity. The HII and photodissociation region (PDR) fine structure lines are an essential part of the SEDs. It is important to add them when modelling the spectra, especially at z > 4 - 6 where their equivalent widths can be large. Conversely, we show that we can extract some information on strong IR fine structure lines and on the physical parameters related to the nebular emission from IR colour-colour diagrams.
