Jupiter's moon Io is the most volcanically active body in the Solar System with hundreds of active volcanoes varying in intensity on different timescales. Io has been observed during occultations by other Galilean moons and Jupiter since the 1980s, using high-cadence near infrared photometry. These observations encode a wealth of information about the volcanic features on its surface. We built a generative model for the observed occultations using the code starry which enables fast, analytic, and differentiable computation of occultation light curves in emitted and reflected light. Our probabilistic Bayesian model is able to recover known hotspots on the surface of Io using only two light curves and without any assumptions on the locations, shapes or the number of spots. The methods we have developed are also directly applicable to the problem of mapping the surfaces of stars and exoplanets.
Physical Characterization of Asteroid (16583) Oersted Combining Stellar Occultation and Photometric Data
Charles University, Faculty of Mathematics and Physics, Institute of Astronomy（查理大学数学物理学院天体物理研究所）；Université Côte d’Azur, CNRS-Lagrange, Observatoire de la Côte d’Azur（蔚蓝海岸大学法国国家科学研究中心拉格朗日实验室蔚蓝海岸天文台）；School of Physics and Astronomy, University of Leicester（莱斯特大学物理与天文学院）；Department of Physics, The Catholic University of America（美国天主教大学物理系）；Astrophysics Science Division, NASA Goddard Space Flight Center（NASA戈达德太空飞行中心天体物理学科学部）；Center for Research and Exploration in Space Science and Technology, NASA/GSFC（NASA/戈达德太空飞行中心空间科学与技术研究探索中心）；SETI Institute, Carl Sagan Center（SETI研究所卡尔·萨根中心）；Unistellar
背景：太阳系外行星的热辐射使得研究其大气层中的重要物理过程和获得更精确的轨道要素成为可能。目标：通过使用新的近红外和光学数据，我们研究这些数据如何约束轨道偏心率和行星大气的热特性。方法：TESS卫星从两个扇区获得的全光变曲线用于设定行星相位变化幅度的上限和估计掩星深度。两个，已经公布的和一个，尚未公布的后续观测在2 MASS K（Ks）波段，推导出更精确的掩星光变曲线在这个近红外波段。结果：Ks波段的合并掩星光变曲线包括4515个数据点。这些数据证实了早期偏心率估计的结果，表明轨道是圆形的：e=0.005+/-0.015。Ks波段的高通量下降值（2.70+/-0.14）ppt排除了10 sigma水平的简单黑体发射，也与（4-7）sigma水平的当前大气模型不一致。通过对TESS数据的分析，在可见波段，我们发现了一个接近噪音水平的二次日食探测的初步证据，并对行星相位变化的相关幅度进行了限制。一个正式的箱形拟合得到的掩星深度为（0.157+/-0.056）ppt。这意味着对于完全有效的大气环流，Ag=0.43+/-0.15和Ag=0.29+/-0.15的相对高的几何可达性。没有偏好可以看出，无论是氧增强，或碳增强大气模型。
Mid-Infrared Spectroscopy of Uranus from the Spitzer Infrared Spectrometer: 1. Determination of the Mean Temperature Structure of the Upper Troposphere and Stratosphere
The nature of ASASSN-24fw's occultation: modelling the event as dimming by optically thick rings around a sub-stellar companion
Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences（波兰科学院尼古拉·哥白尼天文学中心）；Inter-University Centre for Astronomy and Astrophysics（大学天文与天体物理联合中心）；Institute of Astronomy and Astrophysics, Academia Sinica（中央研究院天文及天文物理学研究所）；Instituto de Astrofísica de Canarias（加那利群岛天体物理学研究所）；Departamento de Astrofísica, Universidad de La Laguna（拉帕鲁纳大学天体物理学系）；European Space Agency (ESA)（欧洲空间局）；Division of Physics, Mathematics and Astronomy, California Institute of Technology（加州理工学院物理、数学与天文学部）
Inferring and Interpreting the Visual Geometric Albedo and Phase Function of Earth
Lunar & Planetary Laboratory, University of Arizona（亚利桑那大学月球与行星实验室）；Habitability, Atmospheres, and Biosignatures Laboratory, University of Arizona（亚利桑那大学宜居性、大气和生物标志物实验室）；NASA Nexus for Exoplanet System Science Virtual Planetary Laboratory, University of Washington（华盛顿大学NASA系外行星系统科学虚拟行星实验室）
