$z\sim 1.5$星系的Angular momentum及其具有自适应光学的局域类似物
Angular momentum of $z\sim 1.5$ galaxies and their local analogues with adaptive optics
摘要：
我们提出恒星比角动量$j_*$测量的两个$z\sim 1.5$星系的KGES样本和12个$z\sim 0.1$类似物的高红移星系。我们结合自然看到积分场光谱数据跟踪线发射到高倍数的有效半径$r_e$，与自适应光学辅助凯克/OSIRIS观测跟踪旋转曲线的快速上升的内部区域。我们的空间坐标积分方法给出的结果平均在传统旋转曲线模型方法的测量不确定性范围内。在$z\sim 0$中，结合GMOS和OSIRIS数据集将$j_*$中的测量不确定性从13%（仅GMOS）或16%（仅OSIRIS）提高到10%。在$z\sim 1.5$，系统学允许$j_*$最多20%的不确定性。高$z$星系的类似物，其恒星质量$M_*$的$j_*$较低，而其$j_*/M_*$的膨胀与总光比$β$较低。高$z$星系COSMOS 127977的$j_*/M_*$与正常的本地盘星系一致，而UDS 78317与本地类似物一致。然而，我们的高分辨率OSIRIS数据显示，UDS 78317可能是一个合并系统。我们报告的距离之间的关系的$β-j_*/M_*$平面和速度色散旋转速度$σ/v_{max}$，其中星系偏离更多的平面是更多的分散为主，由于湍流。$M_*-j_*$的大部分散射不能用膨胀与总膨胀比的变化或红移的演化来解释，可能是由于恒星形成引起的湍流增加，或者将合并视为旋转的圆盘。
英文摘要：
We present stellar specific angular momentum $j_*$ measurements of two $z\sim 1.5$ galaxies in the KGES sample and 12 DYNAMO $z\sim 0.1$ analogues of high-redshift galaxies. We combine natural seeing integral field spectroscopic data to trace line emission out to high multiples of effective radius $r_e$, with adaptive optics assisted Keck/OSIRIS observations to trace the rapid rise in rotation curve in the inner regions. Our spaxel-wise integration method gives results that are on average within measurement uncertainty of the traditional rotation curve model method. At $z\sim 0$, combining GMOS and OSIRIS datasets improves the measurement uncertainty in $j_*$ from 13\% (GMOS only) or 16\% (OSIRIS only) to 10\%. At $z\sim 1.5$, systematics allow for at best 20\% uncertainty on $j_*$. DYNAMO analogues of high-$z$ galaxies have low $j_*$ for their stellar mass $M_*$, and low bulge-to-total light ratio $β$ for their $j_*/M_*$. The high-$z$ galaxy COSMOS 127977 has $j_*/M_*$ consistent with normal local disk galaxies, while UDS 78317 is consistent with local analogues. However, our high-resolution OSIRIS data reveal that UDS 78317 may be a merging system. We report a relationship between distance to the $β-j_*/M_*$ plane and the ratio of velocity dispersion to rotational velocity $σ/v_{max}$, where galaxies that deviate more from the plane are more dispersion-dominated due to turbulence. Much of the scatter in $M_*-j_*$ that is not explained by variations in the bulge-to-total ratio or evolution with redshift may be driven by increased turbulence due to star formation, or by treating mergers as rotating disks.
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