论文标题
Alma [Nıı]205μm成像光谱镜头的镜头亚曲线尺寸ID 141在红移4.24
ALMA [N ıı] 205 μm Imaging Spectroscopy of the Lensed Submillimeter galaxy ID 141 at redshift 4.24
论文作者
论文摘要
我们介绍了Atacama大毫米/亚毫米阵列（ALMA）在[N II] 205 $μ$ M线（以下[n ii]）和（RESTFRAME）197.6 $μ$ m的[n ii] 205 $ $ m $ m线（以下[n ii]）中，z = 4.24的亚毫米毫米（SMG）ID 141。从Z = 0.595处的星系对镜头放大镜头，ID 141是最亮的Z $> 4 $ SMG之一。在$ \ sim1.2“ $至$ 1.5” $（$ 1“ \ sim6.9 $ kpc）的角度决议中Continuum Image具有sérsic索引$ \ simeq 0.95 $，$ \ sim0.18”（\ sim 1.24 $ kpc）的sérsic半径。此外，源平面中的重建[n ii]速度场由旋转组件支配，最大速度为$ \ sim 300 $ km/s在大radii处，表明暗物质halo质量为$ \ sim 10^{12} {12} {12} m _ {\ odot} $。这与重建的速度分散场在星系的大部分外部相比具有光滑和适度的价值（$ <100 $ km/s），有利于ID 141的解释是旋转动态支持的磁盘星系。 The observed [N II]/CO (7-6) and [N II]/[C II] 158 $μ$m line luminosity ratios, which are consistent with the corresponding line ratio vs. far-infrared color correlation from local luminous infrared galaxies, imply a de-lensed star formation rate of ($1.8\pm 0.6)\times10^3M_\odot$/yr and provide an independent estimate on the size of恒星形成区域$ 0.7^{+0.3} _ { - 0.3} $ kpc in Radius。
We present the Atacama Large Millimeter/submillimeter Array (ALMA) observation of the Sub-millimeter galaxy (SMG) ID 141 at z=4.24 in the [N II] 205 $μ$m line (hereafter [N II]) and the underlying continuum at (rest-frame) 197.6 $μ$m. Benefiting from lensing magnification by a galaxy pair at z=0.595, ID 141 is one of the brightest z$>4$ SMGs. At the angular resolutions of $\sim1.2"$ to $1.5"$ ($1" \sim6.9$ kpc), our observation clearly separates, and moderately resolves the two lensed images in both continuum and line emission at $\rm S/N>5$ . Our continuum-based lensing model implies an averaged amplification factor of $\sim5.8$ and reveals that the de-lensed continuum image has the Sérsic index $\simeq 0.95$ and the Sérsic radius of $\sim0.18" (\sim 1.24$ kpc). Furthermore, the reconstructed [N II] velocity field in the source plane is dominated by a rotation component with a maximum velocity of $\sim 300$ km/s at large radii, indicating a dark matter halo mass of $\sim 10^{12}M_{\odot}$. This, together with the reconstructed velocity dispersion field being smooth and modest in value ($<100$ km/s) over much of the outer parts of the galaxy, favours the interpretation of ID 141 being a disk galaxy dynamically supported by rotation. The observed [N II]/CO (7-6) and [N II]/[C II] 158 $μ$m line luminosity ratios, which are consistent with the corresponding line ratio vs. far-infrared color correlation from local luminous infrared galaxies, imply a de-lensed star formation rate of ($1.8\pm 0.6)\times10^3M_\odot$/yr and provide an independent estimate on the size of the star-forming region $0.7^{+0.3}_{-0.3}$ kpc in radius.
