论文标题
CO（J = 1-0）在银河系区域内对丝状云的观察，$ 153.60^{\ Circ} \ leqslant l \ leqslant 156.50^{\ circ} $和$ 1.85^{\ circ} \ circ}
CO(J = 1-0) Observations toward the Filamentary Cloud in the Galactic Region of $153.60^{\circ} \leqslant l \leqslant 156.50^{\circ}$ and $1.85^{\circ} \leqslant b \leqslant 3.50^{\circ}$
论文作者
论文摘要
我们提出了$ j $ = 1-0的$ {}^{}^{12} \ mathrm {co} $，$ {}^{}^{13} \ Mathrm {Co} $的观察结果\ leqslant l \ leqslant 156.50^{\ circ} $和$ 1.85^{\ circ} \ leqslant b \ leqslant 3.50^{\ circ} $，使用紫色山脉（PMO）13.7毫米毫米望远镜。基于\ tht数据，在$ [-42.5，-30.0] \，\ Mathrm {km} \ Mathrm {\ \，s}^{ - 1} $的速度间隔中一起找到一个主要细丝和五个子丝作为网络结构。该分子云（MC）的运动距离估计为$ \ sim4.5 \ mathrm {\，kpc} $。这些细丝的中间长度，宽度，激发温度，线质量为$ \ sim49 \ mathrm {\，pc} $，$ \ sim2.9 \ mathrm {\，pc} $，$ \ sim8.9 \ sim8.9 \ mathrm \ Mathrm {PC}^{ - 1} $。沿这些细丝的速度结构表现出振荡模式，这可能是由于这些细丝的碎裂或吸积过程引起的。估计最大积聚率高达$ \ sim700 \，m _ {\ odot} \ mathrm {pc}^{ - 1} $。在该区域中确定了总共$ \ sim162 $ \ tht团块和$ \ sim 103 $ Young Stellar对象（YSO）。大多数团块处于重力结合状态。发现三个\ HII区域（G154.359+2.606，SH2-211，SH2-212）位于细丝的顶点。在整个丝状云中都发现了激烈的星形形成活动。观察到的结果可能有助于我们更好地了解细丝与大量恒星形成之间的联系。
We present observations of $J$=1-0 transition lines of ${ }^{12} \mathrm{CO}$, ${ }^{13} \mathrm{CO}$, and $\mathrm{C}^{18} \mathrm{O}$ towards the Galactic region of $153.60^{\circ} \leqslant l \leqslant 156.50^{\circ}$ and $1.85^{\circ} \leqslant b \leqslant 3.50^{\circ}$, using the Purple Mountain Observatory (PMO) 13.7 m millimeter telescope. Based on the \tht data, one main filament and five sub-filaments are found together as a network structure in the velocity interval of $[-42.5, -30.0] \,\mathrm{km} \mathrm{\,s}^{-1}$. The kinematic distance of this molecular cloud (MC) is estimated to be $\sim4.5 \mathrm{\,kpc}$. The median length, width, excitation temperature, line mass of these filaments are $\sim49 \mathrm{\,pc}$, $\sim2.9 \mathrm{\,pc}$, $\sim8.9 \mathrm{\,K}$, and $\sim39 \,M_{\odot} \mathrm{pc}^{-1}$, respectively. The velocity structures along these filaments exhibit oscillatory patterns, which are likely caused by the fragmentation or accretion process along these filaments. The maximum accretion rate is estimated to be as high as $\sim700 \,M_{\odot} \mathrm{pc}^{-1}$. A total of $\sim162$ \tht clumps and $\sim 103$ young stellar objects (YSOs) are identified in this region. Most of the clumps are in gravitationally bound states. Three \hii regions (G154.359+2.606, SH2-211, SH2-212) are found to be located in the apexes of the filaments. Intense star forming activities are found along the entire filamentary cloud. The observed results may help us to better understand the link between filaments and massive star formation.
