论文标题
猎户座星云群中的原星盘：Alma可以看到的气盘形态和运动学
Protoplanetary Disks in the Orion Nebula Cluster: Gas Disk Morphologies and Kinematics as seen with ALMA
论文作者
论文摘要
我们介绍了Atacama大毫米阵列公司（3 $ - $ 2）和HCO $^+$（4 $ - $ 3）观察值涵盖了中央$ 1 \ rlap {。}'5 $$ \ times $$ $$ 1 \ rlap {。}'5 $ of Orion nebula cluster（ONC）。 The unprecedented level of sensitivity ($\sim$0.1 mJy beam$^{-1}$) and angular resolution ($\sim$$0\rlap{.}''09 \approx 35$ AU) of these line observations enable us to search for gas-disk detections towards the known positions of submillimeter-detected dust disks in this region.我们在CO中检测到23个气体：17个磁盘（3 $ - $ 2），HCO $^+$（4 $ - $ 3）中的17个磁盘，两行中的11个。根据源位于ONC中的位置，我们可以看到发射中的线检测，吸收温暖的背景或发射和吸收。我们通过$ 0.5 $ km s $^{ - 1} $ CHANNELS解决气体，并发现大多数来源的运动学与开普勒旋转一致。我们测量气盘尺寸的分布，并找到$ \ sim $ 50-200 au的典型半径。因此，与低密度恒星形成区域中看到的气盘相比，ONC中的气盘是紧凑的。气体尺寸比灰尘尺寸大。但是，气体和灰尘尺寸并不密切相关。我们发现气体尺寸与距大型恒星$θ^1 $ ori c之间的正相关，表明ONC中的磁盘受光离子化的影响。最后，我们使用观察到的检测到气体线的运动学来对开普勒旋转进行建模，并推断中央前序列恒星的质量。我们动态衍生的恒星质量与光谱衍生的质量不一致，我们讨论了这种差异的可能原因。
We present Atacama Large Millimeter Array CO(3$-$2) and HCO$^+$(4$-$3) observations covering the central $1\rlap{.}'5$$\times$$1\rlap{.}'5$ region of the Orion Nebula Cluster (ONC). The unprecedented level of sensitivity ($\sim$0.1 mJy beam$^{-1}$) and angular resolution ($\sim$$0\rlap{.}''09 \approx 35$ AU) of these line observations enable us to search for gas-disk detections towards the known positions of submillimeter-detected dust disks in this region. We detect 23 disks in gas: 17 in CO(3$-$2), 17 in HCO$^+$(4$-$3), and 11 in both lines. Depending on where the sources are located in the ONC, we see the line detections in emission, in absorption against the warm background, or in both emission and absorption. We spectrally resolve the gas with $0.5$ km s$^{-1}$ channels, and find that the kinematics of most sources are consistent with Keplerian rotation. We measure the distribution of gas-disk sizes and find typical radii of $\sim$50-200 AU. As such, gas disks in the ONC are compact in comparison with the gas disks seen in low-density star-forming regions. Gas sizes are universally larger than the dust sizes. However, the gas and dust sizes are not strongly correlated. We find a positive correlation between gas size and distance from the massive star $θ^1$ Ori C, indicating that disks in the ONC are influenced by photoionization. Finally, we use the observed kinematics of the detected gas lines to model Keplerian rotation and infer the masses of the central pre-main-sequence stars. Our dynamically-derived stellar masses are not consistent with the spectroscopically-derived masses, and we discuss possible reasons for this discrepancy.
