最近的、最亮的碎片盘宿主恒星：具有饱和2MASS测光恒星的最新光球模型与尘埃性质
The Nearest, Brightest Debris Disk Host Stars: Updated Photosphere Models and Dust Properties for Stars with Saturated 2MASS Photometry
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中文总结 AI 辅助
针对2MASS饱和的最亮碎片盘宿主星，用替代测光构建新光球模型，拟合红外数据估计尘埃温度与距离，识别可成像候选盘，并发现Tri星暖尘或可被JWST分辨。
中文摘要 AI 辅助
为了发现并表征碎片盘，必须获得高质量的光度数据，以便精确拟合宿主恒星的光球模型。由于$K$波段总是落在恒星光谱能量分布（SED）的瑞利-金斯一侧，其可靠性对于揭示来自尘埃的中红外过量辐射尤为重要。虽然两微米全天巡天（2MASS）测光是大多数由斯皮策和广域红外巡天探测器（WISE）发现的碎片盘宿主恒星的红外基准，但最亮的恒星（$K_s < 5$）使2MASS探测器饱和。为了精确建模围绕最近、最亮恒星的碎片盘，我们通过用来自NASA红外观测目录的$JHK$测光、档案$R_C I_C$测光以及饱和校正的WISE W1测光替换饱和的2MASS数据，构建了新的光球模型。我们通过将黑体和修正黑体模型拟合到来自WISE、斯皮策和赫歇尔的红外测光，估算尘埃温度和距恒星的最小距离。我们的模型使我们能够识别在天空中张角较大的盘；这些盘是地面角差分成像、哈勃空间望远镜（HST）上的空间望远镜成像光谱仪（STIS）以及JWST上的NIRCam进行后续观测的候选目标。最后，我们发现围绕$\gamma$~Tri的盘可能具有暖尘埃，这些尘埃可能通过JWST的MIRI仪器在$23$或$25.5 \micron$处可分辨。多波长观测为碰撞级联模型提供了基准，并可能揭示行星-盘相互作用。
英文摘要
To discover and characterize debris disks, one must obtain high-quality photometry in order to accurately fit photosphere models for the host stars. Since the $K$ band always falls on the Rayleigh-Jeans side of a star's spectral energy distribution (SED), its reliability is particularly important for uncovering mid-infrared excess emission from dust. While Two Micron All Sky Survey (2MASS) photometry is the near-infrared benchmark for most stars that host debris disks discovered by Spitzer and the Wide Field Infrared Survey Explorer (WISE), the brightest stars ($K_s < 5$) saturated the 2MASS detectors. To accurately model debris disks that orbit the nearest, brightest stars, we construct new photosphere models by replacing saturated 2MASS data with $JHK$ photometry from the NASA Catalog of Infrared Observations, archival $R_C I_C$ photometry, and saturation-corrected WISE W1 photometry. We estimate the dust temperature and minimum distance from the star by fitting blackbody and modified blackbody models to infrared photometry from WISE, Spitzer, and Herschel. Our models allow us to identify disks that subtend large angles on the sky; these disks are candidates for follow-up with ground-based angular differential imaging, the Space Telescope Imaging Spectrograph (STIS) on the Hubble Space Telescope (HST), and NIRCam on JWST. Finally, we find that the disk surrounding $γ$~Tri likely has warm dust that could be resolvable with JWST's MIRI instrument at $23$ or $25.5 \micron$. Multiwavelength observations provide benchmarks for collisional cascade models and may reveal planet--disk interactions.
发表机构
- University of Delaware（特拉华大学）
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