论文标题
从CO与Alma的两个过渡推断出的年轻星星的动态质量
Dynamical Masses of Young Stars Inferred from Two Transitions of CO with ALMA
论文作者
论文摘要
恒星质量是基本的，但通常很难衡量。得益于Atacama大毫米阵列（ALMA）和$ GAIA $，可以使用原行星磁盘的开普勒旋转来精确测量预梅因序列星的动态质量。我们使用CT CHA和DS TAU的Alma CO（2-1）和CO（3-2）观察结果来确定其质量，通过使用基于贝叶斯的辐射转移模型代码$ PDSPY $对其磁盘的几何形状，运动学和物理性质进行建模。我们发现，在2-4 $σ$水平下，两个过渡的质量的后部分布不一致。这些系统的错误可能源于磁盘模型中的假设，或者可能是本研究中使用的适度空间或光谱分辨率。无论如何，这表明由于这些系统误差，应谨慎使用磁盘运动学的动态质量测量值。
Stellar masses are fundamental but often difficult to measure. Thanks to the Atacama Large Millimeter Array (ALMA) and $Gaia$, dynamical masses of pre-main sequence stars can be precisely measured using the Keplerian rotation of protoplanetary disks. We used ALMA CO(2-1) and CO(3-2) observations of CT Cha and DS Tau to determine their masses by modeling the geometry, kinematics, and physical properties of their disks with a Bayesian-based radiative transfer modeling code $pdspy$. We found that the posterior distributions of the masses from the two transitions are inconsistent at the 2-4 $σ$ level. These systematic errors may originate from assumptions in the disk model, or perhaps the modest spatial or spectral resolutions used in this study. Regardless, this indicates that dynamical mass measurements using disk kinematics should be treated with caution when using only a single transition line because of these systematic errors.
