论文标题
太空中的生命种子。 ix。 $ \ rm so_2 $的化学隔离，因此朝着低质量的ProtoStellar震惊区域的L1157区域
Seeds of Life in Space SOLIS. IX. Chemical segregation of $\rm SO_2$ and SO toward the low-mass protostellar shocked region of L1157
论文作者
论文摘要
我们介绍了SO和$ \ rm SO_2 $线的观察结果，沿L1157化学丰富的流出区域，这是在太空中生命种子的背景下拍摄的IRAM-Northern扩展毫米阵列大型程序，并得到了亚毫升阵列和IRAM-30 M望远镜的数据支持，在1.1-3.6 mmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmmm的范围内。我们首次同时分析了蓝光叶中的所有最明亮的冲击，即B0，B1和B2。我们找到了以下内容。 （1）SO和$ \ rm SO_2 $可能会追踪不同的气体，鉴于大（ - 尺度）速度梯度分析表示$ \ rm so_2 $ so_2 $ a量密度（$ \ rm 10^5 \ text { - } 10^6 \，cm^{ - 3} $）固定的订单，即订单的命令。 （2）研究0.1 PC量表视野，我们注意到沿进取射流路径的暂定梯度。更具体地说，$ \rmχ（{so/so_2}）$从B0-B1冲击减少到较旧的B2。 （3）在线性分辨率为500--1400 AU的情况下，检测到两个发射分子之间的暂定空间位移，SO峰更近（相对于$ \ rm so_2 $），到最近的喷气机在B1腔壁上撞击的位置。我们的天体化学建模表明，SO和$ \ rm SO_2 $丰度在时间标准上不到1000年。此外，该建模需要$ \ rm H_2S/H $和S/H的高丰度（$ 2 \ times10^{ - 6} $），并且由于冲击发生而在气相注射了S/H。因此，前烟叶的OCS仅足以再现我们的新观察结果。
We present observations of SO and $\rm SO_2$ lines toward the shocked regions along the L1157 chemically rich outflow, taken in the context of the Seeds Of Life In Space IRAM-NOrthern Extended Millimeter Array Large Program, and supported by data from Submillimeter Array and IRAM-30 m telescope at 1.1--3.6 mm wavelengths. We simultaneously analyze, for the first time, all of the brightest shocks in the blueshifted lobe, namely, B0, B1, and B2. We found the following. (1) SO and $\rm SO_2$ may trace different gas, given that the large(-scale) velocity gradient analysis indicates for $\rm SO_2$ a volume density ($\rm 10^5\text{--}10^6\,cm^{-3}$) denser than that of the gas emitting in SO by a factor up to an order of magnitude. (2) Investigating the 0.1 pc scale field of view, we note a tentative gradient along the path of the precessing jet. More specifically, $\rm χ({SO/SO_2})$ decreases from the B0-B1 shocks to the older B2. (3) At a linear resolution of 500--1400 au, a tentative spatial displacement between the two emitting molecules is detected, with the SO peak closer (with respect to $\rm SO_2$) to the position where the recent jet is impinging on the B1 cavity wall. Our astrochemical modeling shows that the SO and $\rm SO_2$ abundances evolve on timescales less than about 1000 years. Furthermore, the modeling requires high abundances ($2\times10^{-6}$) of both $\rm H_2S/H$ and S/H injected in the gas phase due to the shock occurrence, so pre-frozen OCS only is not enough to reproduce our new observations.
