arXiv 2005.050062020-05-11astro-ph.GAastro-ph.SR

高质量团簇形成区的多股外流，G25 .82-0.17

Multiple outflows in the high-mass cluster forming region, G25.82-0.17

Jungha Kim, Mi Kyoung Kim, Tomoya Hirota, Kee-Tae Kim, Koichiro Sugiyama, Mareki Honma, Do-young Byun, Chungsik Oh, Kazuhito Motogi, Jihyun Kang, Jeongsook Kim,… 展开作者

Jungha Kim, Mi Kyoung Kim, Tomoya Hirota, Kee-Tae Kim, Koichiro Sugiyama, Mareki Honma, Do-young Byun, Chungsik Oh, Kazuhito Motogi, Jihyun Kang, Jeongsook Kim, Tie Liu, Bo Hu, Ross A. Burns, James O. Chibueze, Naoko Matsumoto, Kazuyoshi Sunada

备注：: 28 pages, 9 figures, accepted to ApJ
DOI：: 10.3847/1538-4357/ab9100

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摘要：

我们目前的连续谱和光谱线观测的结果与ALMA和22 GHz的水（H $_2$ O）脉泽观测使用的KaVA和VERA对高质量恒星形成区，G25.82-0.17。多个1.3毫米的连续源被揭示，表明存在年轻恒星物体（YSO）在不同的演化阶段，即超紧凑的HII区域，G25.82-E，高质量的年轻恒星物体（HM-YSO），G25.82-W1，和无星的核心，G25.82-W2和G25.82-W3。两个SiO外流，在N-S和SE-NW方向的识别。CH $_3$ OH 8 $_{-1}$ -7 $_{0}$ E谱线是一个I类CH $_3$ OH脉泽，频率为229 GHz，同时也探测到热辐射和脉泽辐射。此外，H $_2$ O脉泽分布在距离G25.82-W1约0.25”的区域内。CH $_3$ OH 22 $_{4}$ -21 $_{5}$ E谱线在G25.82-W1位置显示了一个致密的环状结构，具有速度梯度，表明有一个旋转盘或包层。假设开普勒旋转，G25.82-W1的动力学质量估计为$>$ 25 M $_{\odot}$，20 M $_\odot$ -84 M $_\odot$的总质量由1.3 mm连续谱发射得出。南北向SiO外流的驱动源为G25.82-W1，东南-NW向SiO外流的驱动源不确定。探测到多个大质量无星的$/$原恒星核心和没有低质量核心的候选者意味着HM-YSO可以形成于湍流核心吸积模型预测的单个高质量核心。如果是这样的话，G25.82中的高质量恒星形成过程将与低质量恒星形成的放大版本相一致。

英文摘要：

We present results of continuum and spectral line observations with ALMA and 22 GHz water (H$_2$O) maser observations using KaVA and VERA toward a high-mass star-forming region, G25.82-0.17. Multiple 1.3 mm continuum sources are revealed, indicating the presence of young stellar objects (YSOs) at different evolutionary stages, namely an ultra-compact HII region, G25.82-E, a high-mass young stellar object (HM-YSO), G25.82-W1, and starless cores, G25.82-W2 and G25.82-W3. Two SiO outflows, at N-S and SE-NW orientations, are identified. The CH$_3$OH 8$_{-1}$-7$_{0}$ E line, known to be a class I CH$_3$OH maser at 229 GHz is also detected showing a mixture of thermal and maser emission. Moreover, the H$_2$O masers are distributed in a region ~0.25" shifted from G25.82-W1. The CH$_3$OH 22$_{4}$-21$_{5}$ E line shows a compact ring-like structure at the position of G25.82-W1 with a velocity gradient, indicating a rotating disk or envelope. Assuming Keplerian rotation, the dynamical mass of G25.82-W1 is estimated to be $>$25 M$_{\odot}$ and the total mass of 20 M$_\odot$-84 M$_\odot$ is derived from the 1.3 mm continuum emission. The driving source of the N-S SiO outflow is G25.82-W1 while that of the SE-NW SiO outflow is uncertain. Detection of multiple high-mass starless$/$protostellar cores and candidates without low-mass cores implies that HM-YSOs could form in individual high-mass cores as predicted by the turbulent core accretion model. If this is the case, the high-mass star formation process in G25.82 would be consistent with a scaled-up version of low-mass star formation.

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摘要：

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