论文标题
IR特性排放和星形星系的尘埃特性为4.5 $ <$ <$ z $ <$ 6.2
IR characteristic emission and dust properties of star-forming galaxies at 4.5 $<$ z $<$ 6.2
论文作者
论文摘要
Z <4-5的光度功能表明，大多数星系具有相对较低的恒星质量（LOGM_STAR = 10）和低灰尘衰减（A_FUV = 1.0）。这些对象的物理特性是相当均匀的。我们使用了一种方法，将他们的休息框架远红外和亚毫米排放组合在一起，并利用宇宙和红移作为光谱仪以集体方式增加信息量。从Z> 4.5处的27个Alma检测星系的子样本中，我们构建了一个红外光谱能量分布复合模板。它用于与Cigale配合，从FUV到FIR的样品中的105个星系（检测和上限）。派生的物理参数提供了信息，以解读这些星系中尘埃周期和恒星种群的性质。派生的IR复合模板与所研究样品中的星系一致。与最终突发或连续的恒星形成历史相比，统计分析的延迟恒星形成历史= 500 MYR被统计分析略有青睐。样品在星形形成速率（SFR）-M_STAR图中的位置与以前的论文一致。 log m_star与A_FUV关系的红移演变与此关系的红移中的演变一致。这种进化对于解释星系平均灰尘衰减的宇宙演变是必要的。在l_dust/ l_fuv（irx）与UV Slope beta_fuv图中也观察到进化：年轻的星系具有Bluer beta_fuv。我们建模了IRX中星系的移位与Beta_Fuv图，其大规模加权年龄为自由参数，我们提供了一个方程来进行预测。
The luminosity functions at z < 4 - 5 suggest that most galaxies have a relatively low stellar mass (logM_star = 10) and a low dust attenuation (A_FUV = 1.0). The physical properties of these objects are quite homogeneous. We used an approach where we combined their rest-frame far-infrared and submillimeter emissions and utilized the universe and the redshift as a spectrograph to increase the amount of information in a collective way. From a subsample of 27 ALMA-detected galaxies at z > 4.5, we built an infrared spectral energy distribution composite template. It was used to fit, with CIGALE, the 105 galaxies (detections and upper limits) in the sample from the FUV to the FIR. The derived physical parameters provide information to decipher the nature of the dust cycle and of the stellar populations in these galaxies. The derived IR composite template is consistent with the galaxies in the studied sample. A delayed star formation history with tau_main = 500 Myrs is slightly favored by the statistical analysis as compared to a delayed with a final burst or a continuous star formation history. The position of the sample in the star formation rate (SFR)- M_star diagram is consistent with previous papers. The redshift evolution of the log M_star versus A_FUV relation is in agreement with evolution in the redshift of this relation. This evolution is necessary to explain the cosmic evolution of the average dust attenuation of galaxies. Evolution is also observed in the L_dust/ L_FUV (IRX) versus UV slope beta_FUV diagram: younger galaxies have bluer beta_FUV. We modeled the shift of galaxies in the IRX versus the beta_FUV diagram with the mass-weighted age as a free parameter, and we provide an equation to make predictions.
