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

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。NGC 2264分子云是一个有吸引力的恒星形成区域，在760 pc附近，具有低的前景消光和大量的前主序星，其年龄分散是连续星星形成的证据。孤立的星星形成发生在中心大质量恒星形成星团NGC 2264-C和NGC 2264-D向外辐射的丝状体中。丝状结构在分子云中普遍存在，我们的目标是了解团簇的演化序列，以及与丝状结构的关系。亚毫米连续辐射探测了星星形成的最早阶段：具有高柱密度和低温的核心。发射光很薄，直接追踪分子云的质量含量。随着SCUBA-2的出现，云的大尺度尘埃结构将首次在大于1-20'的尺度上被测量，而许多现有的研究对这一尺度不敏感。利用这一能力，我们将利用10小时的分配时间来测量大规模的细丝密度，并定位密集、紧凑的核心。利用我们现有的HARP-CO数据，我们获得了NGC 2264的温度场和速度场，因此我们可以将细丝的位置和物理参数与孤立核心和集群的位置，活动和演化进行比较。

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.