CHEMISTRY AND FEEDBACK IN MASSIVE STAR FORMING REGIONS

形成高质量恒星(8个太阳质量)的区域显示出惊人的化学多样性，从富含复杂有机分子的“热核心”到冷、致密的核心，分子谱线发射很少或根本没有。该项目的目的是首先利用亚毫米阵列对高质量恒星形成区进行的调查来确定和量化这种化学多样性。利用本次调查提供的统一观测的大样本，该项目将包括为大型干涉数据立方体开发有效的(半自动)分析方法，并探索来源分类的统计方法。天体化学分析的结果将与其他对高质量恒星形成重要的现象的示踪物相互关联，包括流出、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.