We present a new near-infrared photometric system for detection of water ice and methane ice in the solar system. The system consists of two medium-band filters in the K-band region of the near-infrared, which are sensitive to water ice and methane ice, plus continuum observations in the J-band and Y-band. The primary purpose of this system is to distinguish between three basic types of Kuiper Belt Objects (KBOs) --- those rich in water ice, those rich in methane ice, and those with little absorbance. In this work, we present proof-of-concept observations of 51 KBOs using our filter system, 21 of which have never been observed in the near-IR spectroscopically. We show that our custom photometric system is consistent with previous spectroscopic observations while reducing telescope observing time by a factor of 3. We use our filters to identify Haumea collisional family members, which are thought to be collisional remnants of a much larger body and are characterized by large fractions of water ice on their surfaces. We add 2009 YE7 to the Haumea collisional family based on our water ice band observations(J-H2O = -1.03 +/- 0.27) which indicate a high amount of water ice absorption, our calculated proper orbital elements, and the neutral optical colors we measured, V-R = 0.38 +/- 0.04, which are all consistent with the rest of the Haumea family. We identify several objects dynamically similar to Haumea as being distinct from the Haumea family as they do not have water ice on their surfaces. In addition, we find that only the largest KBOs have methane ice, and we find that Haumea itself has significantly less water ice absorption than the smaller Haumea family members. We find no evidence for other families in the Kuiper Belt.
The surface composition of large Kuiper belt object 2007 OR10
我们提出的光度学和光谱的大型柯伊伯带对象2007 OR 10。这些数据显示了由于水冰而产生的显著的近红外吸收特征。虽然柯伊伯带中大多数吸收水冰的天体都具有水冰的光学中性颜色，但2007 OR 10是已知的最红的柯伊伯带天体之一。另一个大型柯伊伯带天体-夸欧尔-有类似的红色和水冰吸收，它的红色被假设是由于照射的少量甲烷能够保留在夸欧尔。2007 OR 10虽然比夸欧尔更温暖，但也有类似的挥发性保留，因为它足够大，其更强的重力仍然可以保留甲烷。因此，我们认为2007 OR 10上的红色也是由少量甲烷的保留引起的。阳性检测将需要2007年甲烷的光谱，或10将需要具有更高信噪比的光谱。柯伊伯带天体上的挥发物保留模型似乎继续在再现所有可用的观测结果方面做得很好。
Modification of icy planetesimals by early thermal evolution and collisions: Constraints for formation time and initial size of comets and small KBOs
彗星和小型柯伊伯带天体被认为是太阳系中最原始的天体之一，因为像C/1995 O 1 Hale-Bopp这样的彗星富含像CO这样的高度挥发性冰。在这里，我们采用二维有限差分数值模型来研究这些对象的内部热演化，在那里我们改变形成时间，半径和岩石冰质量分数。此外，我们执行不同的碰撞参量的三维SPH碰撞模型，从而考虑到陨石坑和灾难性的破坏事件。结合这两个数值模型的结果，我们估计在何种条件下，高挥发性的冰，如CO，CO2和NH3可以保留在现今的彗星和柯伊伯带物体。我们的研究结果表明，对于目前的对象来自最大的碰撞后残留物的内部热演化控制剩余的高度挥发性冰的量，而从未绑定的碰撞后材料形成的对象的影响加热是占主导地位的。最后，我们将我们的结果应用到今天的彗星和柯伊伯带天体，如67 P/Churyumov-Gerasimenko，C/1995 O 1 Hale-Bopp和（486958）Arrokoth。
JWST reveals anomalously enhanced methane outgassing from below Chiron's water ice and carbon dioxide bearing surface
Space Telescope Science Institute（太空望远镜科学研究所）；Southwest Research Institute（西南研究院）；Université Lyon 1（里昂第一大学）；NASA Goddard Space Flight Center（美国国家航空航天局戈达德太空飞行中心）；Université Paris-Saclay（巴黎萨克雷大学）；Northern Arizona University（北亚利桑那大学）；University of Oviedo（奥维耶多大学）；University of Central Florida（中佛罗里达大学）
An Enriched Methane D/H Ratio in the Interstellar Object 3I/ATLAS
NASA Goddard Space Flight Center（美国国家航空航天局戈达德太空飞行中心）；American University（美利坚大学）；Catholic University of America（天主教大学）；LIRA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université Paris Cité, CY Cergy Paris Université（巴黎天文台LIRA实验室，巴黎文理研究大学，法国国家科学研究中心，索邦大学，巴黎西岱大学，塞吉-蓬图瓦兹大学）；Auburn University（奥本大学）
1I/'Oumuamua as an N2 ice fragment of an exo-Pluto surface: I. size and compositional constraints
星际天体1I/'Oumuamua的起源一直无法解释。我们进行计算的非重力加速度，将经历由一系列不同的冰组成的机构，并证明，由N2冰组成的机构将满足现有的约束条件的非重力加速度，大小和体积，以及缺乏可检测的排放的CO或CO2或灰尘。我们发现'Oumuamua很小，在距离太阳1.42天文单位的观测时尺寸为45 m x 44 m x 7.5 m，具有0.64的高散射度。这与冥王星和海卫一等天体的N2表面一致。我们估计'Oumuamua'大约在0.4 - 0.5 Gyr前从一个年轻的恒星系统中喷出，可能在英仙座臂中。像'Oumuamua'这样的物体可能直接探测到一种迄今未观测到的系外行星类型的表面成分："外冥王星"。在一篇配套论文（Desch & Jackson，2021）中，我们证明了在其他恒星系统中，像柯伊伯带所经历的那样的动力学不稳定性可能会产生并喷射出大量的N2冰碎片。“Oumuamua可能是带给我们的第一个系外行星样本。
