CHEMISTRY AND FEEDBACK IN MASSIVE STAR FORMING REGIONS

形成高质量恒星（> 8个太阳质量）的区域表现出惊人的化学多样性，从富含复杂有机分子的“热核”到几乎没有分子线发射的冷而致密的核心。该项目的目的是描述和量化这种化学多样性，首先使用亚毫米阵列（SMA;莫纳克亚山上的毫米波长干涉仪）对高质量星星形成区域进行调查。利用这次调查提供的大量统一观测样本，该项目将包括为大型干涉测量数据立方体开发有效的（半）自动分析方法，并探索源分类的统计方法。天体化学分析的结果将与其他对大质量星星形成很重要的现象的示踪剂相互关联，包括外流、电离和辐射反馈。

Regions forming high mass stars (> 8 solar masses) exhibit a striking chemical diversity, from "hot cores" rich in complex organic molecules to cold, dense cores with little or no molecular line emission. The aim of this project is to characterize and quantify this chemical diversity using, in the first instance, a survey of high mass star forming regions conducted with the Submillimeter Array (SMA; the millimetre-wavelength interferometer on Mauna Kea). Using the large sample of uniform observations provided by this survey, the project will include developing efficient (semi)automated analysis methods for large interferometric datacubes and exploring statistical approaches to source classification. The results of the astrochemical analysis will be cross-correlated with tracers of other phenomena important to high-mass star formation, including outflow, ionizing, and radiative feedback.