每个数据点都很重要:恒星耀斑作为 LSST 时代大气辅助瞬变研究的案例研究

Riley W. Clarke, James R. A. Davenport, John Gizis, Melissa L. Graham, Xiaolong Li, Willow Fortino, Easton J. Honaker, Ian Sullivan, Yusra Alsayyad, James Bosch, Robert A. Knop, Federica B. Bianco
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摘要

由于时间尺度较短,恒星耀斑对于最现代的同步巡天观测来说是一个具有挑战性的目标。即将开展的维拉-C-鲁宾时空遗产巡天(LSST)是一个旨在收集比任何先导巡天更多数据的项目,但在其主要巡天中不太可能探测到一个以上数据点的耀斑。我们开发了一种方法,使 LSST 能够对恒星耀斑进行研究,重点是耀斑温度和温度演化,与耀斑形态相比,耀斑温度和温度演化的约束性仍然很差。通过利用鲁宾系统的预期灵敏度,差分色度折射(DCR)可用于通过单波段探测来约束耀斑温度,这将实现耀斑温度的统计研究,并利用鲁宾系统在10年LSST期间产生的前所未有的大量数据来约束耀斑发射背后的物理过程模型。我们将折射效应建模为大气柱密度、光度滤光片和耀斑温度的函数,并表明,考虑到对LSST单次观测相对天体测量精度的最低规定要求,在空气质量X ≳ 1.2的条件下,通过单次g波段观测就可以约束4000 K或以上的耀斑温度。由于未能在 LSST 前兆巡天中测量耀斑 DCR,我们对巡天设计和数据产品提出了建议,以便在 LSST 和其他未来的巡天中进行这些研究。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
Every Data Point Counts: Stellar Flares as a Case Study of Atmosphere-aided Studies of Transients in the LSST Era
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 (DCR) 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 yr 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 ∼4000 K can be constrained by a single g-band observation at air mass X ≳ 1.2, given the minimum specified requirement on the single-visit relative astrometric accuracy of LSST, and that a surprisingly large number of LSST observations are 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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