The Interstellar Gas in Star Forming Regions

了解大质量恒星的形成和控制它的星际气体的特性之间的相互作用对于理解宇宙的演化是至关重要的。研究计划的一个要素是通过观察附近星系分子的毫米线来研究这种相互作用，这些分子是星际气体条件的示踪剂。此外，正在进行理论计算，以模拟大质量恒星形成时产生的激波对周围介质的激发作用。通过这种方式，它旨在将初始气体条件与恒星形成的结果分开，特别是在经历大质量恒星形成爆发的星系中。此外，一些关于大星团中新生的大质量恒星的风的星际气体的集体效应的新想法将被测试，这被认为是星暴星系中恒星形成的主要途径。特别是，这些星系中众多致密射电辐射源的性质将是这些想法的重点，因为它们目前被认为是超新星的残留物，即结束大质量恒星生命的爆炸。如果得到证实，这些想法将表明它们是星团风的集体效应，这反过来可能会大大改变我们对大质量恒星形成对周围气体影响的理解。最后，我们将对银河系中心气体的恒星形成潜力进行分子线研究，以了解这个过程是如何发生的，尽管有强烈的紫外线辐射和与中心区域相关的重力潮汐应力的抑制作用。重点放在某些分子示踪剂上，这些示踪剂将对潜在的恒星形成团块中分子气体的解离和蒸发进行取样，并揭示星际尘埃颗粒地幔的蒸发。这项研究将与宇宙早期星系和类星体的形成有关。

An understanding of the interplay between massive star formation and the properties of the interstellar gas which control it is crucial to comprehending the evolution of the universe. An element of the research plan is to investigate this interaction by observations of nearby galaxies in the millimetre lines of molecules which are tracers of conditions in the interstellar gas. In addition, theoretical computations are being undertaken to simulate the excitation effects of the shock waves produced by the formation of massive stars on the surrounding medium. In this way, it is intended to separate initial gas conditions from those that are the consequences of star formation, especially in galaxies undergoing bursts of massive star formation.   In addition, some new ideas will be tested concerning the collective effects on the interstellar gas of the winds of newly born massive stars in large star clusters which are known to be a primary route of star formation in starburst galaxies. In particular, the nature of the numerous compact sources of radio radiation in such galaxies will be the focus of these ideas, since they are currently thought to be the remnants of supernovae, the explosions which end the life of massive stars. If borne out, these ideas will show that they are instead the collective effects of cluster winds, which in turn may considerably modify our understanding of the impact of massive star formation on the surrounding gas.   Finally, we will conduct a molecular line study of the star forming potential of gas at the very centre of our own Galaxy in order to understand how this process occurs despite the inhibiting effects of intense ultravioletradiation and gravitational tidal stresses associated with the central region. Emphasis is being placed on certain molecular tracers which will sample the dissociation and evaporation of molecular gas from potential star forming clumps, and reveal the evaporation of the mantles of interstellar dust grains. The study will have relevance to the formation of galaxies and quasars at an early stage of the universe.