Stellar Atmospheres in the era of Big Data

在未来的十年里，天文学调查将监测我们银河系内外数十亿颗恒星的光谱。天文学家将从这些光谱中描述恒星的特性，包括它们的表面温度，重力和原子组成，以探索银河系的形成和演变历史;我们宇宙中元素的演变和创造;以及恒星的结构和演变。但是，这些大型调查依赖于我们对恒星大气层的理解以及锚定这些模型的物理学。以同样的方式，我们采用模型恒星大气探测和表征高角分辨率的系外行星凌日和光学干涉观测的恒星是敏感的强度在整个恒星盘。 在未来十年中，大型光谱测量，如大型综合巡天望远镜（LSST），Maunakea光谱探测器（MSE）和SpecTel，与光学干涉测量设施和行星凌日任务（如凌日系外行星巡天卫星（TESS））相结合，将为恒星大气的精确物理学提供新的联合测试。这种方法是一种新颖的方法，可以连接恒星大气物理学的两个测试，并以前所未有的细节引导恒星。这两种方法的观测结果，光谱和高角分辨率，都依赖于恒星大气的模型来物理和精确地解释它们。目前还没有开源的建模程序套件可以高精度地探测观测结果。我将利用即将到来的大量测量，使用最先进的恒星大气代码SAtlas创建一个开源环境，用于拟合来自调查的恒星光谱和拟合行星过境和光学干涉测量。这使我们能够测量基本的恒星参数，如质量，半径和温度沿着的组成;通过作为波长函数的过境测量更精确地描述系外行星大气;测量我们银河系中恒星的化学历史;并在局部尺度上探索宇宙学。 这些进步将允许恒星大气的动态和自动化建模，以构建跨越许多参数的网格，例如恒星表面温度，质量和半径，以及每种元素的丰度，沿着测试恒星大气中的其他物理特性，例如恒星对流，旋转，化学分层。 加拿大的天文学界在建造大型光谱巡天（如LSST和MSE）以及通过MOST卫星飞行任务和即将进行的CASTOR和JWST飞行任务进行行星凌日观测方面发挥了领导作用，沿着。这项工作旨在创建计算资源，以获得对银河考古学的新见解，并表征恒星表面和系外行星大气。

In the coming decade astronomy surveys will monitor the spectra from billions of stars in our Galaxy and beyond. From these spectra, astronomers will characterize the properties of stars, including their surface temperatures, gravities and atomic composition to probe the formation and evolution history of the Galaxy; the evolution and creation of elements in our Universe; and the structure and evolution of stars. But, these big surveys rely on our understanding stellar atmospheres and the physics anchoring those models. In the same way, we employ model stellar atmospheres to probe and characterize high-angular resolution exoplanetary transits and optical interferometric observations of stars that are sensitive to the intensity across the stellar disk. The combination of of big spectral surveys in the next decade, such as the Large Synoptic Survey Telescope (LSST), the Maunakea Spectroscopic Explorer (MSE), and SpecTel, with optical interferometric facilities and with planetary transit missions such as Transiting Exoplanet Survey Satellite (TESS)  will offer novel joint tests of the precise physics of stellar atmospheres. This approach is a novel methodology to bridge two tests of the physics of stellar atmospheres and lead about stars in unprecedented detail. The observations from both methods, spectroscopic and high-angular resolution, rely on models of stellar atmospheres to physically and precisely interpret them. There are currently no open source suites of modelling programs that can probe observations with the high precision. I will take advantage of the abundance of forthcoming measurements by using the state-of-the-art stellar atmospheres code SAtlas to create an open source environment for both fitting stellar spectra from surveys and fitting planet transit and optical interferometric measurements. This allows us to measure fundamental stellar parameters such as mass, radius and temperature along with composition; to more precisely characterize exoplanet atmospheres via transit measurements as function of wavelength; to measure the chemical history of stars across our Galaxy; and probe the cosmology at the local scale. These advancements will allow for dynamic and automated modelling of stellar atmospheres to construct grids across numerous parameters such as stellar surface temperature, mass and radius, and abundance of each element, along with testing additional physics in stellar atmospheres such as stellar convection, rotation, chemical stratification. The astronomy community in Canada has demonstrated leadership in constructing large spectral surveys such as LSST and MSE along with planetary transit observations through the MOST satellite missions and upcoming CASTOR and JWST missions. This work aims to create computational resources for gaining new insights into Galactic Archaeology and for characterizing stellar surfaces and exoplanetary atmospheres.