Collaborative Research: High Resolution Spectroscopy and Spectro-Astrometry of Warm Gas in Herbig Ae/Be Stars: A Search for Forming Gas Giant Planets

该团队将使用地面望远镜和计算机模型来探测和描述其他恒星周围圆盘中的系外行星。该团队将应用新技术来探测仍在形成过程中的气态巨行星。如果成功，这些结果将使我们能够将行星形成环境的初始条件与形成的行星类型联系起来。对我们自己的星球是如何形成的固有好奇心吸引了来自各种背景的学生进入STEM学科。参与这个项目的学生将有机会利用最先进的天文台和计算模型提供的数据，在现代天体物理学的前沿之一进行研究。之前参与这一群体的学生将他们的经验应用于K-12教育、工业、国防等职业，以及更传统的研究职业。该项目还将为南卡罗来纳州立大学-克莱姆森大学桥梁项目的学生提供基于研究的学习机会，积极扩大未被充分代表的群体对天文学的参与。该项目有三个主要科学目标。(1)搜索围绕赫比格Ae/Be恒星运行的伴星周围的行星盘：生成赫比格Ae/Be的所有存档高分辨率M波段观测的统一图集，搜索指示轨道伴星的可变CO排放，并获得额外的观测结果。(2)寻找大质量星下伴星的动力学标志。(3)将该小组的热化学模型应用于观测到的氢氧化物和一氧化碳排放源，以检验氢氧化物主要来自恒星周盘内缘的假设。

This team will use ground-based telescopes and computer models to detect and characterize exoplanets in disks around other stars. The team will apply novel techniques to detect gas giant planets that are still in the process of forming. If successful, these results would allow us to connect the initial conditions of the planet-forming environment to the kinds of planets that form. Inherent curiosity about how our own planet came to be attracts students from all backgrounds into STEM disciplines. The students involved with this project will have the opportunity to carry out research at one of the frontiers of modern astrophysics by exploiting data available from state of the art observatories and computational modeling. Previous students involved in this group have applied their experiences to careers in K-12 education, industry, national defense, in addition to more traditional research careers. This project will also provide research-based learning opportunities for students in the South Carolina State University - Clemson University bridge program, actively broadening participation of underrepresented groups in astronomy.This program has three principal science goals. (1) Search for circumplanetary disks around companions orbiting Herbig Ae/Be stars: generate a uniform atlas of all archival high resolution M-band observations of Herbig Ae/Be, search for variable CO emission indicative of an orbiting companion, and obtain additional observations. (2) Search for dynamical markers of massive substellar companions. (3) Apply this group's thermochemical model to sources with observed OH and CO emission to test the hypothesis that OH primarily arises from the inner rim of circumstellar disks.