论文标题
阿尔玛（Alma
ALMA uncovers the [CII] emission and warm dust continuum in a z = 8.31 Lyman break galaxy
论文作者
论文摘要
我们通过使用Atacama大毫米/毫米阵列（ALMA）报告了从Lyman Break Galaxy（LBG）MacS0416_Y1中检测到[CII] 157.7 $ $ m $ M的检测。 [OIII] 88 $μ$ m（从以前的广告系列）到[CII]的发光比为9.31 $ \ pm $ 2.6，表明硬星际辐射场和/或较低的照片分解区域的覆盖范围低。 [CII]的排放是对850 $ $ m灰尘排放（90美元$ $ $ $ m的休息框架，从以前的广告系列中）的同级，但是峰值[CII]发射与峰值[OIII]的发射不一致，这表明该线的线是源于星际介质中不同条件的线。我们无法以1.5毫米（160美元$ $ m retsframe）的速度检测到连续排放，至18美元$ $ $ jy（3 $σ$）。考虑到137美元$ \ pm $ 26 $μ$ $ jy Continuum排放量为850 $μ$ m。这表明与较低的红色降低的星系范围内的灰尘排放相比，与较低的灰尘排放相比，异常温暖的灰尘成分（T $> $ 80 K，90％的置信度限制）和/或陡峭的灰尘发射率指数（$β_ {\ rm dust} $ $> $ 2）（通常是在较低的红色什至红色的尘埃粉尘上）（通常是T $ \ sim $ \ sim $ 30-50-50-50-50-50 k，$ $ pust $ pult $ pult）如果这种温度很常见，这将减少所需的尘埃质量并在最高的红移下放松灰尘生产问题。因此，我们警告不要仅使用单波长信息来得出物理特性，建议对早期宇宙中的灰尘温度进行更彻底的检查，并强调需要探测电离时代温暖灰尘峰的仪器。
We report on the detection of the [CII] 157.7 $μ$m emission from the Lyman break galaxy (LBG) MACS0416_Y1 at z = 8.3113, by using the Atacama Large Millimeter/submillimeter Array (ALMA). The luminosity ratio of [OIII] 88 $μ$m (from previous campaigns) to [CII] is 9.31 $\pm$ 2.6, indicative of hard interstellar radiation fields and/or a low covering fraction of photo-dissociation regions. The emission of [CII] is cospatial to the 850 $μ$m dust emission (90 $μ$m rest-frame, from previous campaigns), however the peak [CII] emission does not agree with the peak [OIII] emission, suggesting that the lines originate from different conditions in the interstellar medium. We fail to detect continuum emission at 1.5 mm (160 $μ$m rest-frame) down to 18 $μ$Jy (3$σ$). This nondetection places a strong limit on the dust spectrum, considering the 137 $\pm$ 26 $μ$Jy continuum emission at 850 $μ$m. This suggests an unusually warm dust component (T $>$ 80 K, 90% confidence limit), and/or a steep dust-emissivity index ($β_{\rm dust}$ $>$ 2), compared to galaxy-wide dust emission found at lower redshifts (typically T $\sim$ 30 - 50 K, $β_{\rm dust}$ $\sim$ 1 - 2). If such temperatures are common, this would reduce the required dust mass and relax the dust production problem at the highest redshifts. We therefore warn against the use of only single-wavelength information to derive physical properties, recommend a more thorough examination of dust temperatures in the early Universe, and stress the need for instrumentation that probes the peak of warm dust in the Epoch of Reionization.
