论文标题
使用Alma单频段连续观测来估计高红移星系的尘埃温度和远射光度
Estimating Dust Temperature and Far-IR Luminosity of High-Redshift Galaxies using ALMA Single-Band Continuum Observations
论文作者
论文摘要
我们提出了一种方法，该方法衍生了高红移星系的灰尘温度和红外（IR）亮度，假设在简单的灰尘和恒星分布几何形状中辐射平衡。使用Atacama大毫米/亚毫米阵列（ALMA）档案中的公共数据，我们研究了灰尘温度，假设高红移星系的块状星际介质（ISM）模型，然后测试了我们使用其他方法获得的结果的一致性。我们发现，假设$ {\ rm log} \，ξ_ {\ rm clp} = -1.02 \ pm0.41 $的灰尘分配模型可以准确地代表高降射星形星系的ISM。通过假设$ξ_ {\ rm {clp}} $的值，我们的方法可以从灰尘连续磁通量和从单带ALMA观测中获得的灰尘连续磁通和发射尺寸的高红色星系的灰尘温度和IR发光度推导。为了证明此处提出的方法，我们确定了$ z \ sim8.3 $ star-forming Galaxy，Macs0416-Y1的灰尘温度（$ t _ {\ rm d} = 95^{+13} _ { - 17} \，\ rm {k} $。由于该方法仅需要单带灰尘观察即可得出灰尘温度，因此比多带观测值或高红移发射线搜索更容易获得，并且可以在未来的研究中使用高分辨率干涉仪（例如ALMA）在未来的研究中应用于大型星系。
We present a method that derives the dust temperatures and infrared (IR) luminosities of high-redshift galaxies assuming radiation equilibrium in a simple dust and stellar distribution geometry. Using public data from the Atacama Large Millimeter/submillimeter Array (ALMA) archive, we studied dust temperatures assuming a clumpy interstellar medium (ISM) model for high-redshift galaxies, then tested the consistency of our results with those obtained using other methods. We find that a dust distribution model assuming a clumpiness of ${\rm log}\,ξ_{\rm clp}=-1.02\pm0.41$ may accurately represent the ISM of high-redshift star-forming galaxies. By assuming a value of $ξ_{\rm{clp}}$, our method enables the derivation of dust temperatures and IR luminosities of high-redshift galaxies from dust continuum fluxes and emission sizes obtained from single-band ALMA observations. to demonstrate the method proposed herein, we determined the dust temperature ($T_{\rm d}=95^{+13}_{-17}\,\rm{K}$) of a $z\sim8.3$ star-forming galaxy, MACS0416-Y1. Because the method only requires a single-band dust observation to derive a dust temperature, it is more easily accessible than multi-band observations or high-redshift emission line searches and can be applied to large samples of galaxies in future studies using high resolution interferometers such as ALMA.
