用JWST干涉测量探测水霜线附近的行星质量伴星
Detecting planetary mass companions near the water frost-line using JWST interferometry
摘要：
JWST有望成为未来二十年最多功能的红外天文台。近红外和无狭缝光谱仪在孔径掩蔽干涉测量法模式下使用时，与任何现有的中红外波长观测站相比，将提供无与伦比的角分辨率和灵敏度。使用模拟观测与进化模型相结合，我们提出了这种模式的能力，图像行星质量的同伴在附近的恒星周围的小轨道分离附近的拱星水霜线的年轻，运动的团体Beta Picture，TW长蛇座，以及金牛座御夫座协会的成员。我们发现，对于适当选择的恒星，JWST/NIRISS在AMI模式下运行可以成像亚木星同伴附近的水霜线与~68%的置信度。其中，M型星是最有希望的。我们还表明，这种JWST模式将提高最小的内部工作角高达~50%，在大多数情况下，从最好的地面系外行星直接成像设施（如VLT/SPHERE）的调查结果相比。我们还讨论了NIRISS/AMI模式将如何特别强大的中红外表征的众多系外行星预计将被盖亚揭示。当与来自盖亚的动力学质量相结合时，这样的测量将提供这些年轻行星的初始熵的更强大的表征，从而对它们的早期热历史施加强大的约束。
英文摘要：
JWST promises to be the most versatile infrared observatory for the next two decades. The Near Infrared and Slitless Spectrograph (NIRISS) instrument, when used in the Aperture Masking Interferometry (AMI) mode, will provide an unparalleled combination of angular resolution and sensitivity compared to any existing observatory at mid-infrared wavelengths. Using simulated observations in conjunction with evolutionary models, we present the capability of this mode to image planetary mass companions around nearby stars at small orbital separations near the circumstellar water frost-line for members of the young, kinematic moving groups Beta Pictoris, TW Hydrae, as well as the Taurus-Auriga association. We show that for appropriately chosen stars, JWST/NIRISS operating in the AMI mode can image sub-Jupiter companions near the water frost-lines with ~68% confidence. Among these, M-type stars are the most promising. We also show that this JWST mode will improve the minimum inner working angle by as much as ~50% in most cases when compared to the survey results from the best ground-based exoplanet direct imaging facilities (e.g. VLT/SPHERE). We also discuss how the NIRISS/AMI mode will be especially powerful for the mid-infrared characterization of the numerous exoplanets expected to be revealed by Gaia. When combined with dynamical masses from Gaia, such measurements will provide a much more robust characterization of the initial entropies of these young planets, thereby placing powerful constraints on their early thermal histories.
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