Deciphering the interstellar medium around the Scorpius-Centarus OB association

我们提出研究天蝎座-半人马座OB星协附近星际介质（ISM）的复杂结构和演化。由于这是最近大质量恒星形成的区域，多波长观测可以提供一个独特的机会，详细研究scoc - cen中众所周知的大质量恒星群如何向ISM提供动能、电离辐射和核合成抛射物，以及这种反馈如何在关联周围产生可观察到的超级气泡系统，并破坏母体分子云。我们还将测试这样一个场景，即这种恒星反馈席卷了新的密集分子云，并引发了这些云中新一代恒星的形成。我们将把MPE种群合成代码与流体动力学模拟结合起来，以跟踪放射性示踪剂，这些示踪剂从大质量恒星中喷射出来，作为星际环境演化和不同气相混合的独立标志。数值模拟的理论预测将与观测数据进行比较，以检验模型。在这个项目开始的两年中，我们收集了大量的ScoCen复合体的观测数据，从无线电到伽马射线，我们现在可以用这些观测数据来描述ScoCen及其周围的ISM。我们利用来自普朗克、赫歇尔的数据，以及APEX亚毫米望远镜的新观测数据，研究了冷致密云的结构和物理参数，特别是狼疮1号分子云，它可能是由两个碰撞气泡相互作用产生的。我们最近被允许在APEX望远镜上有更多的时间来观察狼座云的选定部分的CO线发射；这将以前所未有的分辨率揭示分子气体的运动学。为了追踪更温暖和更扩散的气体，我们分析了来自帕克斯星系全天空巡天的21厘米HI无线电数据，这些数据提供了关于膨胀气泡结构和运动学的非常详细的信息。我们对用INTEGRAL测量的放射性伽马射线和漫射x射线发射的分析将追踪大质量恒星的超新星和风输出。在第二个资助期，我们将整合所有这些数据集，以全面了解上海合作组织ISM的结构和动态。面对这些数据的数值模拟应该最终导致一个自洽的模式的起源，演化，和co- cen复合体的命运。

We propose to study the complex structure and evolution of the interstellar medium (ISM) in the vicinity of the Scorpius-Centaurus OB association. As this is the nearest region of recent massive star formation, multi-wavelength observations can provide a unique opportunity to investigate in detail how the well known population of massive stars in Sco-Cen feeds the ISM with kinetic energy, ionizing radiation, and nucleosynthesis ejecta, and how this feedback created the observed systems of superbubbles surrounding the association and destroyed the parental molecular cloud. We will also test the scenario that this stellar feedback swept up new dense molecular clouds and triggered the formation of new generations of stars in these clouds. We will couple the MPE population synthesis code with hydrodynamical simulations in order to follow radioactive tracers, ejected from the massive stars as an independent signature of the evolution of the interstellar environment and the mixing of different gas phases. The theoretical predictions from the numerical simulations will be compared with the observational data to test the models.In the two years since the start of this project, we have collected numerous observations of the ScoCen complex across a wide range of wavelengths, from the radio to the gamma-ray regime, that we can now use to characterize the ISM in and around ScoCen.We use data from Planck, Herschel, and our new observations with the APEX sub-mm telescope to study the structure and the physical parameters of the cold dense clouds, in particular the Lupus I molecular cloud, that was probably created by the interaction of two colliding bubbles. We have been recently granted further time at the APEX telescope to observe the CO line emission in selected parts of the Lupus clouds; this will reveal the kinematics of the molecular gas in unprecedented resolution. In order to trace the warmer and more diffuse gas, we analyze new 21 cm HI radio data from the Parkes Galactic All Sky Survey, which provide very detailed information about the structure and kinematics of the expanding bubbles. Our analysis of the radioactivity gamma-rays as measured with INTEGRAL and the diffuse X-ray emission will trace the supernova- and wind-outputs of the massive stars. In the second funding period, we will combine all these data sets to obtain a comprehensive picture of the structure and dynamics of the ISM in Sco-Cen. Confronting the numerical simulations to these data should finally lead to a self-consistent model of the origin, evolution, and fate of the Sco-Cen complex.