论文标题
$ z = 9.1 $ Galaxy的成熟恒星种群中可能的系统旋转
Possible Systematic Rotation in the Mature Stellar Population of a $z=9.1$ Galaxy
论文作者
论文摘要
我们以$ z = 9.1 $，macs1149-jd1的重力静态星系进行了Atacama大型毫米/亚毫米阵列的新观察结果。 [O iii] 88- $μ$ m的排放量以10 $σ$检测到，空间分辨率为$ \ sim0.3 $ kpc在源平面中，从而实现了银河系最遥远的形态研究。 [O III]发射的分布平稳，没有任何分解的团块，并显示出$ΔV_{\ rm obs}/2σ_ {\ rm tot} = 0.84 \ pm0.23 $的清晰速度梯度，$ΔV_{在空间综合的线轮廓中测量的速度分散体，表明旋转系统。假设有几何薄的自我修剪旋转磁盘模型，我们获得了$ v _ {\ rm rot}/σ_v=0.67_ { - 0.26}^{+0.73} $，其中$ v _ {\ rm rot} $和$σ_V$是旋转效率的旋转效率和亲velocity and Notiention ofertiantial ofertional ofertiantial ofertional ofertional oferiation notively oferiation notimity oferiation of oferiation of oferiatiential offiention。由此产生的磁盘质量为$ 0.65 _ { - 0.40}^{+1.37} \ times10^{9} $ m $ _ \ odot $与与恒星质量相关的与300 Myr少的恒星人群相关的一致，该巨大的恒星人群由光谱分布中的A Balmer Break breake breakent optional spectral spectral spection spectral Enproments分布。我们得出的结论是，大部分动态质量与以$ z \ sim15 $形成的先前确定的成熟恒星种群有关。
We present new observations with the Atacama Large Millimeter/submillimeter Array for a gravitationally-lensed galaxy at $z=9.1$, MACS1149-JD1. [O III] 88-$μ$m emission is detected at 10$σ$ with a spatial resolution of $\sim0.3$ kpc in the source plane, enabling the most distant morpho-kinematic study of a galaxy. The [O III] emission is distributed smoothly without any resolved clumps and shows a clear velocity gradient with $ΔV_{\rm obs}/2σ_{\rm tot}=0.84\pm0.23$, where $ΔV_{\rm obs}$ is the observed maximum velocity difference and $σ_{\rm tot}$ is the velocity dispersion measured in the spatially-integrated line profile, suggesting a rotating system. Assuming a geometrically thin self-gravitating rotation disk model, we obtain $V_{\rm rot}/σ_V=0.67_{-0.26}^{+0.73}$, where $V_{\rm rot}$ and $σ_V$ are the rotation velocity and velocity dispersion, respectively, still consistent with rotation. The resulting disk mass of $0.65_{-0.40}^{+1.37}\times10^{9}$ M$_\odot$ is consistent with being associated with the stellar mass identified with a 300 Myr-old stellar population independently indicated by a Balmer break in the spectral energy distribution. We conclude that the most of the dynamical mass is associated with the previously-identified mature stellar population that formed at $z\sim15$.
