每一个数据点都至关重要：恒星耀斑作为LSST时代大气辅助瞬变源研究的案例研究
Every Datapoint Counts: Stellar Flares as a Case Study of Atmosphere Aided Studies of Transients in the LSST Era
AI总结：
针对LSST难以多历元探测恒星耀斑的问题，提出利用差分色散折射从单次观测约束耀斑温度的方法，并给出巡天设计建议，以利用海量数据开展统计研究。
摘要：
由于恒星耀斑的时间尺度很短，它们对最现代的全天巡天项目而言是一个具有挑战性的目标。即将开展的薇拉·鲁宾遗产时空巡天（LSST）是一个旨在收集比任何前期巡天项目更多数据的项目，但其主巡天不太可能探测到具有多于一个数据点的耀斑。我们开发了一种方法，使LSST能够研究恒星耀斑，重点关注耀斑温度及其演化，这些方面与耀斑形态相比仍受到较差的约束。通过利用鲁宾系统预期的灵敏度，差分色散折射（Differential Chromatic Refraction）可用于从单历元探测中约束耀斑温度，这将使得对耀斑温度的统计研究成为可能，并利用鲁宾在10年LSST期间产生的空前高数据量来约束耀斑发射背后物理过程的模型。我们将折射效应建模为大气柱密度、测光滤波器和耀斑温度的函数，并表明在LSST单次访问相对天体测量精度的最低规定要求下，当大气质量X > 1.2时，单次g波段观测即可约束约4,000K及以上温度的耀斑；并且尽管图像质量要求推动巡天优先选择低大气质量X，但事实上LSST很可能有数量惊人的观测在X > 1.2条件下进行。由于未能在LSST前期巡天中测量到耀斑的DCR，我们对巡天设计和数据产品提出了建议，以便在LSST及其他未来巡天中实现这些研究。
英文摘要：
Due to their short timescale, stellar flares are a challenging target for the most modern synoptic sky surveys. The upcoming Vera C. Rubin Legacy Survey of Space and Time (LSST), a project designed to collect more data than any precursor survey, is unlikely to detect flares with more than one data point in its main survey. We developed a methodology to enable LSST studies of stellar flares, with a focus on flare temperature and temperature evolution, which remain poorly constrained compared to flare morphology. By leveraging the sensitivity expected from the Rubin system, Differential Chromatic Refraction can be used to constrain flare temperature from a single-epoch detection, which will enable statistical studies of flare temperatures and constrain models of the physical processes behind flare emission using the unprecedentedly high volume of data produced by Rubin over the 10-year LSST. We model the refraction effect as a function of the atmospheric column density, photometric filter, and temperature of the flare, and show that flare temperatures at or above ~4,000K can be constrained by a single g-band observation at airmass X > 1.2, given the minimum specified requirement on single-visit relative astrometric accuracy of LSST, and that a surprisingly large number of LSST observations is in fact likely be conducted at X > 1.2, in spite of image quality requirements pushing the survey to preferentially low X. Having failed to measure flare DCR in LSST precursor surveys, we make recommendations on survey design and data products that enable these studies in LSST and other future surveys.
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