论文标题
阿尔玛叛军调查。电离巨头时代：$ z \ $ z \ 7 $的尘土星系的特性
The ALMA REBELS Survey. Epoch of Reionization giants: properties of dusty galaxies at $z \approx 7$
论文作者
论文摘要
我们分析了Alma Rebels LP中14个星系（$ Z \ 7 $）的FIR粉尘连续测量，以得出其物理特性。 Our model uses three input data: (a) the UV spectral slope, $β$, (b) the observed UV continuum flux at $1500$A, $F_{\rm UV}$, (c) the observed continuum flux at $\approx 158μ$m, $F_{158}$, and considers Milky Way (MW) and SMC extinction curves, along with different dust几何。我们发现叛军星系（28-90.5）的恒星形成被遮盖了；总（UV+IR）星形的形成率在$ 31.5 <{\ rm sfr}/（m_ \ odot {\ rm yr}^{ - 1}）<129.5 $的范围内。样品平均灰尘质量和温度分别为$（1.3 \ pm 1.1）\ times 10^7 m_ \ odot $和$ 52 \ pm 11 $ k。在某些星系中，灰尘很丰富（Rebels-14，$ M'_D \约3.4 \ times 10^7 m_ \ odot $）或热（Rebels-18，$ t'_d \ of 67 $ k）。灰尘分布紧凑（对于70％的星系，$ <0.3 $ kpc）。每个超新星的尘埃收益率为$ 0.1 \ le y_d/m_ \ odot \ le 3.3 $，其中70％的星系需要$ y_d <0.25 m_ \ odot $。三个星系（Rebels-12，14，39）需要$ y_d> 1 m_ \ odot $。通过模型预测的SFR和MW灭绝曲线，在[CII]中检测到的叛军星系很好地遵循局部$ L _ {\ rm CII} - $ SFR关系，并且大约位于Kennicutt-Schmidt关系上。样品平均气体耗竭时间为$ 0.11 \，y_p^{ - 2} $ gyr，其中$ y_p $是气体与恒星分配半径的比率。对于某些系统，无法找到与观察到的（$β，f _ {\ rm UV}，f_ {158} $）值匹配的解决方案。当索引$ i_m =（f_ {158}/f _ {\ rm uv}）/（β-β_ {\ rm int}）$时，发生这种情况，其中$β_ {\ rm int} $是内在的UV slope，超过了$ i_m^**1120 $，超过了$ i_m^**1120 $。对于这些对象，我们认为FIR和UV排放区域不是共同空间的，质疑使用IRX- $β$关系。
We analyse FIR dust continuum measurements for 14 galaxies ($z\approx 7$) in the ALMA REBELS LP to derive their physical properties. Our model uses three input data: (a) the UV spectral slope, $β$, (b) the observed UV continuum flux at $1500$A, $F_{\rm UV}$, (c) the observed continuum flux at $\approx 158μ$m, $F_{158}$, and considers Milky Way (MW) and SMC extinction curves, along with different dust geometries. We find that REBELS galaxies have (28-90.5)% of their star formation obscured; the total (UV+IR) star formation rates are in the range $31.5 < {\rm SFR}/ (M_\odot {\rm yr}^{-1}) < 129.5$. The sample-averaged dust mass and temperature are $(1.3\pm 1.1)\times 10^7 M_\odot$ and $52 \pm 11$ K, respectively. In some galaxies dust is abundant (REBELS-14, $M'_d \approx 3.4 \times 10^7 M_\odot$), or hot (REBELS-18, $T'_d \approx 67$ K). The dust distribution is compact ($<0.3$ kpc for 70% of the galaxies). The dust yield per supernova is $0.1 \le y_d/M_\odot \le 3.3$, with 70% of the galaxies requiring $y_d < 0.25 M_\odot$. Three galaxies (REBELS-12, 14, 39) require $y_d > 1 M_\odot$. With the SFR predicted by the model and a MW extinction curve, REBELS galaxies detected in [CII] nicely follow the local $L_{\rm CII}-$SFR relation, and are approximately located on the Kennicutt-Schmidt relation. The sample-averaged gas depletion time is of $0.11\, y_P^{-2}$ Gyr, where $y_P$ is the ratio of the gas-to-stellar distribution radius. For some systems a solution simultaneously matching the observed ($β, F_{\rm UV}, F_{158}$) values cannot be found. This occurs when the index $I_m = (F_{158}/F_{\rm UV})/(β-β_{\rm int})$, where $β_{\rm int}$ is the intrinsic UV slope, exceeds $I_m^*\approx 1120$ for a MW curve. For these objects we argue that the FIR and UV emitting regions are not co-spatial, questioning the use of the IRX-$β$ relation.
