Support for Observing at CARMA

支持 CARMA 观察

• 批准号: ST/I005838/1
• 负责人: John Richer
• 金额: $ 0.12万
• 依托单位: University of Cambridge
• 依托单位国家: 英国
• 项目类别: Research Grant
• 财政年份: 2010
• 资助国家: 英国
• 起止时间: 2010 至 无数据
• 项目状态: 已结题
• 来源: https://gtr.ukri.org/projects?ref=ST%2FI005838%2F1
• 关键词: Support; Observing; CARMA

Understanding the physics of where and how stars form is a fundamental astrophysical question. The processes associated with star formation are important: on large scales, in the structure and evolution of galaxies, to small scales, in the formation of planets. The NGC2264 molecular cloud is an attractive massive star-forming region to study since at 760 pc it is nearby, and has low foreground extinction. There are two very young, massive star forming clusters that we will observe in several methanol lines at spatial and spectral high resolution. The methanol lines that we will observe cover excitation temperatures from 7 to 130 K, and can trace a range of physical conditions. Reaction on ice grain surfaces is the only viable formation route to methanol, and since it can survive only 10,000 yr in the gas phase, this molecule traces very recent interactions. We can therefore use methanol to probe changes in the physical environment of the clusters induced by recent star formation activity.

了解恒星在哪里以及如何形成的物理学是一个基本的天体物理学问题。与星星形成有关的过程是重要的：从大尺度上的星系结构和演化，到小尺度上的行星形成。NGC2264分子云是一个有吸引力的大质量恒星形成区域，因为它在760 pc附近，并且具有低前景消光。有两个非常年轻，大质量的星星形成的集群，我们将观察在几个甲醇线在空间和光谱的高分辨率。我们将观察到的甲醇谱线涵盖了从7到130 K的激发温度，并且可以跟踪一系列物理条件。在冰粒表面的反应是甲醇唯一可行的形成途径，由于它在气相中只能存活10，000年，这种分子追踪最近的相互作用。因此，我们可以用甲醇来探测由最近的星星形成活动引起的星系团物理环境的变化。