为早期eVolution探测器做准备：利用TESS和Swift的多波长耀斑观测表征年轻行星的光化学输入及凌星探测效率
Preparing for the Early eVolution Explorer: Characterizing the photochemical inputs and transit detection efficiencies of young planets using multiwavelength flare observations by TESS and Swift
AI总结：
本研究利用Swift和TESS多波段观测M矮星耀斑，发现9000K黑体低估NUV流量并存在时间滞后，提出预测方法，证明NUV去耀斑可提升20%凌星探测效率，并展示了EVE探测器的应用潜力。
摘要：
紫外耀斑辐射能够驱动系外行星大气中的光化学过程，甚至可能成为大气反演中不确定性的主要来源。此外，由于缺乏同时观测数据，耀斑能量收支尚未得到充分理解。我们展示了使用Swift和TESS以20秒 cadence获取的三颗M矮星耀斑的新近紫外（NUV）和光学观测数据，并对两颗M矮星的耀斑进行了重新分析，以探究NUV到光学波段的耀斑能量收支和时序特性。我们发现，对于54±14%的耀斑，9000 K黑体会将NUV流量低估≥2倍，而对其中一次耀斑的低估倍数达14.8倍。我们报告了各波段之间存在0.5至6.6分钟的时间滞后，并开发了一种方法来预测耀斑的定性形状和时间滞后，准确率达到36±30%。由于排除了$T_\mathrm{eff}\approx$5000 K的尾部，在比较FWHM持续时间内的总NUV能量与TESS能量时，光学-NUV关系中的离散度降低了2.0±0.6倍。我们表明，NUV光变曲线可用于从光学光变曲线中去除耀斑，并能一致地探测到比无耀斑去趋势时小20%的凌星行星。最后，我们展示了早期eVolution探测器（EVE）能够将文献中的多波长耀斑数量增加10倍，EVE是一个天体物理学小探测器概念，旨在通过同时观测NUV和光学波段来探测年轻行星，评估其光化学辐射环境，并观测吸积过程。
英文摘要：
Ultraviolet flare emission can drive photochemistry in exoplanet atmospheres and even serve as the primary source of uncertainty in atmospheric retrievals. Additionally, flare energy budgets are not well-understood due to a paucity of simultaneous observations. We present new near-UV (NUV) and optical observations of flares from three M dwarfs obtained at 20 s cadence with Swift and TESS, along with a re-analysis of flares from two M dwarfs in order to explore the energy budget and timing of flares at NUV--optical wavelengths. We find a 9000 K blackbody underestimates the NUV flux by $\geq$2$\times$ for 54$\pm$14% of flares and 14.8$\times$ for one flare. We report time lags between the bands of 0.5--6.6 min and develop a method to predict the qualitative flare shape and time lag to 36$\pm$30% accuracy. The scatter present in optical-NUV relations is reduced by a factor of 2.0$\pm$0.6 when comparing the total NUV energy with the TESS energy during the FWHM duration due to the exclusion of the $T_\mathrm{eff}\approx$5000 K tail. We show the NUV light curve can be used to remove flares from the optical light curve and consistently detect planets with 20% smaller transits than is possible without flare detrending. Finally, we demonstrate a 10$\times$ increase in the literature number of multi-wavelength flares with the Early eVolution Explorer (EVE), an astrophysics Small Explorer concept to observe young clusters with simultaneous NUV and optical bands in order to detect young planets, assess their photochemical radiation environments, and observe accretion.
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