论文标题
阿尔玛（Alma
ALMA reveals extended cool gas and hot ionized outflows in a typical star-forming galaxy at $z=7.13$
论文作者
论文摘要
我们介绍了[CII] 158 $ $ m，[oiii] 88 $ $ m，尘埃和静止型紫外线（UV）a1689-Zd1的连续量的空间形态学特性，用于$ z = 7.13 $/sibter（us），unimimimimimimimimimimimimimimimimime（uv）和哈勃太空望远镜（HST）观测值。虽然[OIII]线和UV连续体紧凑，但[CII]线延长至$ r \ sim 12 $ kpc的半径。使用从52-400 $ $ m m的多频段式式式远红外（FIR）连续数据，我们发现平均灰尘温度和发射率指数为$ t _ {\ rm dust} = 41^{+17} _ {+17} _ {-14} _ { - 14} $ k和$ k和$ k and $ k and $β= 1.7^= 1.7^= 1.7^{+1.11} $} $} $}。我们发现在不同波长处的灰尘连续剖面有轻微的差异，这可能表明灰尘温度随距离而降低。我们通过IR和UV Luminosities绘制恒星形成率（SFR），并确定总SFR为$ 37 \ pm 1〜M_ \ odot〜 {\ rm yr}^{ - 1} $，其模糊分数为$ 87 \％$。尽管[OIII]线是SFR的良好示踪剂，但[CII]行显示了与当地$ L _ {\ rm [CII]} $ - SFR关系的偏差。最后，我们观察到[CII]和[OIII]之间的线轮廓有明显的差异，在减去单个高斯模型后，[OIIII]线频谱中有重要的残差（$ \ sim5σ$）。这表明，热离子流出的流出的冷却可能是扩展的[CII]结构的起源。扩展的[CII]和高速度[OIII]发射可能部分促进了高$ L _ {\ rm [oiii]} $/$ l _ {\ rm [cii]} $比率最近在$ z> 6 $ galaxies中最近报道的。
We present spatially-resolved morphological properties of [CII] 158 $μ$m, [OIII] 88 $μ$m, dust, and rest-frame ultraviolet (UV) continuum emission for A1689-zD1, a strongly lensed, sub-L* galaxy at $z=7.13$, by utilizing deep Atacama Large Millimeter/submillimeter Array (ALMA) and Hubble Space Telescope (HST) observations. While the [OIII] line and UV continuum are compact, the [CII] line is extended up to a radius of $r \sim 12$ kpc. Using multi-band rest-frame far-infrared (FIR) continuum data ranging from 52-400 $μ$m, we find an average dust temperature and emissivity index of $T_{\rm dust} = 41^{+17}_{-14}$ K and $β= 1.7^{+1.1}_{-0.7}$, respectively, across the galaxy. We find slight differences in the dust continuum profiles at different wavelengths, which may indicate that the dust temperature decreases with distance. We map the star-formation rate (SFR) via IR and UV luminosities and determine a total SFR of $37\pm 1~M_\odot~{\rm yr}^{-1}$ with an obscured fraction of $87\%$. While the [OIII] line is a good tracer of the SFR, the [CII] line shows deviation from the local $L_{\rm [CII]}$-SFR relations in the outskirts of the galaxy. Finally, we observe a clear difference in the line profile between [CII] and [OIII], with significant residuals ($\sim 5σ$) in the [OIII] line spectrum after subtracting a single Gaussian model. This suggests a possible origin of the extended [CII] structure from the cooling of hot ionized outflows. The extended [CII] and high-velocity [OIII] emission may both contribute in part to the high $L_{\rm [OIII]}$/$L_{\rm [CII]}$ ratios recently reported in $z>6$ galaxies.
