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.

了解恒星形成的地点和方式的物理学是一个基本的天体物理问题。与恒星形成相关的过程很重要：在星系的结构和演变中，在行星的形成中，在小尺度上。 NGC2264分子云是一个有吸引力的巨大恒星形成区域，因为在760 PC上它在附近，并且前景灭绝较低。有两个非常年轻的巨大恒星形成簇，我们将在空间和光谱高分辨率的几个甲醇线中观察到它们。我们将观察到的甲醇线覆盖了7至130 K的激发温度，并且可以追踪一系列物理条件。在冰粒表面上的反应是通往甲醇的唯一可行的地层途径，并且由于气相只能生存10,000年，因此该分子痕迹很近的相互作用。因此，我们可以使用甲醇来探测最近恒星形成活性引起的簇的物理环境的变化。