Support for observing at the JCMT: SCUBA-2 shared risks observing

对 JCMT 观测的支持：SCUBA-2 共担风险观测

• 批准号: ST/I000534/1
• 负责人: John Richer
• 金额: $ 0.19万
• 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%2FI000534%2F1
• 关键词: Support; observing; JCMT; SCUBA; shared

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 star-forming region to study; at 760 pc it is nearby, has low foreground extinction and a large population of pre-main sequence stars, whose age dispersion is evidence of sequential star formation. Isolated star formation is taking place in filaments radiating away from the central massive star-forming clusters NGC2264-C and NGC2264-D. Filamentary structure is ubiquitous in molecular clouds, and we aim to understand the evolutionary sequence of clusters, and the relation to filamentary structure. Submm continuum emission probes the earliest stages of star formation: cores with high column density and low temperatures. The emission is optically thin, directly tracing the mass content of molecular clouds. With the advent of SCUBA-2 the large-scale dust structure of clouds will be for the first time measurable on size scales larger than 1-20' to which many existing studies are insensitive. Using this capability, we will use our 10 hours of allocated time to measure the large-scale density of the filaments and locate the dense, compact cores. With our existing HARP-CO data, we have the temperature and velocity field across NGC2264, and so we can compare the location and physical parameters of the filaments with the location, activity and evolution of both the isolated cores and the clusters.

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恒星形成区域。在760 PC上它在附近，前景灭绝低，并且大量的预梅因序列星，其年龄分散是顺序形成的证据。孤立的恒星形成发生在从中央大型恒星形成簇NGC2264-C和NGC2264-D辐射的细丝中进行。丝状结构在分子云中无处不在，我们旨在了解簇的进化序列以及与丝状结构的关系。 Obsm Continuum发射探测恒星形成的最早阶段：圆柱密度高和低温的核心。发射是光学薄的，直接追踪分子云的质量含量。随着Scuba-2的出现，云的大规模尘埃结构将首次在大于1-20'的尺寸尺度上进行测量，许多现有研究不敏感。使用此功能，我们将使用10小时的分配时间来测量细丝的大规模密度并找到密集的紧凑核。使用现有的HARP-CO数据，我们在NGC2264上具有温度和速度场，因此我们可以将细丝的位置和物理参数与隔离核心和簇的位置，活动和演变进行比较。

项目成果

The JCMT Legacy Survey of the Gould Belt: a first look at Orion B with HARP

• DOI: 10.1111/j.1365-2966.2009.15619.x
• 发表时间: 2009-08
• 期刊: Monthly Notices of the Royal Astronomical Society
• 影响因子: 4.8
• 作者: J. Buckle;E. Curtis;J. Roberts;G. White;G. White;J. Hatchell;C. Brunt;H. Butner;B. Cavanagh-B.-Cav