论文标题
高质量簇形成区域中的多个流出，G25.82-0.17
Multiple outflows in the high-mass cluster forming region, G25.82-0.17
论文作者
论文摘要
我们使用KAVA和VERA朝着高质量星形的区域G25.82-0.17介绍了使用ALMA和22 GHz水（H $ _2 $ O）的连续性和光谱线观测结果。揭示了多个1.3毫米连续源，表明在不同的进化阶段存在年轻恒星物体（YSO），即超压缩的HII区域，G25.82-E，G25.82-E，一种高质量的年轻恒星物体（HM-YSO），G25.82-W1，G25.82-W1，以及G25.82-W2-W2-82-82-82-82-82-82-82-82-82-82-82-82-82-82-82-2-82-82-82-2-82-82-2-82-2-82-82-2-82-2-82-2-82-2-2-82-2-82-2。确定了两个SIO流出，N-S和SE-NW方向。 Ch $ _3 $ OH 8 $ _ { - 1} $ - 7 $ _ {0} $ e系，已知为I ch $ _3 $ _3 $ oh Maser在229 GHz也被检测到，显示了热力和maser排放的混合物。此外，h $ _2 $ o masers分布在〜0.25“从g25.82-w1的区域中分布。ch $ _3 $ _3 $ oh 22 $ _ {4} $ _ {4} $ -21 $ _ {5} $ e线显示在带有速度级别的g25.82-w1的位置上的紧凑型环的结构，指示了旋转的旋转，或者指示旋转的旋转器，以备旋转。 G25.82-W1的质量估计为$> $ 25 m $ _ {\ odot} $，总质量为20 m $ _ \ odot $ -84 m $ _ \ odot $，源自1.3 mm continumenuum continum conterflocy of g25.82-ww1。无质量的$/$ ProtoStellar核心和候选人没有低质量的核心，如果是湍流核心积聚模型的预测，HM-sos可以在单个高质量核心中形成。
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.
