Collaborative Research: Making a Habitable Planet - The Evolution of the Volatile Inventory in Gas-Rich Planet-Forming Disks

现在很明显，有大量的行星围绕着与我们的太阳相似的恒星运行。这个项目试图了解这些行星是如何诞生的，以及培育生命所需的关键元素，如碳、氧、氮和氢，是否可能在它们出生时存在。重点将放在通过研究组成这些元素的分子如何结合到小型岩石天体中来形成类似地球的行星的早期步骤。该计划将把世界级天文望远镜的观测与最先进的详细计算模型结合起来。这个项目将帮助我们更好地理解像我们这样的行星是如何诞生的。这一努力的一个核心部分是培训具有不同背景的下一代科学家，他们代表着研究和教学的未来。合作努力融合了布莱克和伯金团队的工作。这使得使用Keck和ALMA对少于几个AU的气体排放进行观测探索成为可能，这可以使用详细的理论模型来解释。他们将产生数千个跨越参数空间的物理/时间相关的化学模型，他们将开发/实施关于小行星形成和冰固存的处方。这个网格的丰度和排放预测将阐明C、H、O和N元素池的关键载体/示踪剂的命运。这将使得能够确定可观测的、与质量无关的小行星形成的特征。观测工作将以采样年龄范围内的来源为目标。这将在两个方面完成：(1)使用Keck档案、ALMA档案、新的Keck光谱天体测量数据、团队接受的ALMA周期1和2计划，以及关于ALMA周期3的新建议。他们将把这些数据与他们的理论网格进行比较，以表征关键挥发物的整体空间分布及其与行星形成的联系。手头已有的数据集适合于从两个来源研究磁盘化学。(2)第二种是基于氰化物可能是热气体的关键有机示踪剂的证据，热气体的条件与年轻恒星预期的1AU条件相当。他们将使用ALMA第2周期的数据来表征这些有机物在热核中的起源，并提供在附近的磁盘系统中寻找这种进化示踪剂的证据。

It is now clear that there is an abundance of planets in orbit around stars similar to our own Sun. This program seeks to understand how these planets are born and whether key elements needed to foster life, such as carbon, oxygen, nitrogen, and hydrogen, are likely to be present at their birth. The focus will be on the early steps in the formation of an Earth-like planet by studying how molecules comprising these elements are incorporated into small, rocky bodies. This program will combine observations from world-class astronomical telescopes with state-of-the-art detailed computational models. This program will foster a greater understanding of how planets like our own are born. A central part of this effort is the training of the next generation of scientists with diverse backgrounds that represent the future of research and teaching.The collaborative effort merges the work of the Blake and Bergin groups. This enables observational explorations of gas emission from less than a few AU using Keck and beyond with ALMA, which can be interpreted using detailed theoretical models. They will generate several thousand physical/time-dependent chemical models spanning parameter space, and they will develop/implement prescriptions for planetesimal formation and ice sequestration. The abundance and emission predictions from this grid will elucidate the fate of key carriers/tracers of the C, H, O, and N elemental pools. This will enable the determination of observable, mass independent, signatures of planetesimal formation. The observational efforts will target sources sampling a range in age. This will be done in two tracks: (1) Using the Keck archive, the ALMA archive, new Keck spectro-astrometric data, the team's accepted ALMA Cycle 1 and 2 programs, plus new proposals for ALMA Cycle 3. They will compare these data to their theoretical grid to characterize the overall spatial distribution of key volatiles and their links to planet formation. Data sets already in hand are suitable to study disk chemistry in two sources. (2) The second is based on evidence that nitriles might be key organic tracers of hot gas that has conditions comparable to those expected 1 AU from a young star. They will use ALMA Cycle 2 data to characterize the origin of these organics in hot cores and provide to search for evidence of this evolutionary tracer in nearby disk systems.