论文标题
对九个恒星形成区域的化学研究，并具有插入运动的证据
A Chemical Study of Nine Star-forming Regions with Evidence of Infall Motion
论文作者
论文摘要
对分子团块中气体中心运动的物理和化学特性的研究有助于我们了解恒星形成的初始阶段。我们使用IRAM 30米望远镜的FTS宽边模式观察9个具有显着双峰蓝线剖面的九个中心源。观察频率范围为83.7-91.5 GHz和99.4-107.2 GHz。我们获得了分子线数据的数量。使用XCLASS，在这9个来源中已经确定了总共7至27种不同的分子和同位素过渡线，包括CCH，C-C3H2和HC3N等碳链分子。根据辐射转移模型，我们估计了这些来源的旋转温度和色谱柱密度。采用HMSFR的物理模型的化学模拟用于拟合观察到的分子丰度。比较表明，大多数来源处于HMPO早期阶段，内部温度约为十个。
The study of the physical and chemical properties of gas infall motion in the molecular clumps helps us understand the initial stages of star formation. We used the FTS wide-sideband mode of the IRAM 30-m telescope to observe nine infall sources with significant double peaked blue line profile. The observation frequency range are 83.7 - 91.5 GHz and 99.4 - 107.2 GHz. We have obtained numbers of molecular line data. Using XCLASS, a total of 7 to 27 different molecules and isotopic transition lines have been identified in these nine sources, including carbon chain molecules such as CCH, c-C3H2 and HC3N. According to the radiation transfer model, we estimated the rotation temperatures and column densities of these sources. Chemical simulations adopting a physical model of HMSFRs are used to fit the observed molecular abundances. The comparison shows that most sources are in the early HMPO stage, with the inner temperature around several ten K.
