JWST Reveals Varied Origins Between Jupiter's Irregular Satellites
University of Maryland（马里兰大学）；Johns Hopkins University Applied Physics Laboratory（约翰斯·霍普金斯大学应用物理实验室）；Space Telescope Science Institute（太空望远镜科学研究所）；Northern Arizona University（北亚利桑那大学）
Benjamin N. L. Sharkey, Andrew S. Rivkin, Richard J. Cartwright, Bryan J. Holler, Joshua P. Emery, Cristina Thomas
备注：
Revised: 22 Pages, 11 Figures, 2 Tables. Accepted to PSJ
We report observations of eight Jovian irregular satellites with JWST's NIRSpec instrument: Himalia, Elara, Pasiphae, Sinope, Lysithea, Carme, Ananke, and Themisto. Irregular satellite families, which are presumed to have formed via collisions, contain various Trojan-like and C-type-asteroid-like surfaces. We sample the three largest members of the Himalia satellite family, detecting the presence of complexed CO$_2$ and a unique absorption band from $\sim2.7-3.6\ μm$ whose character correlates with satellite size. The two largest irregular satellites, Himalia family members Himalia and Elara, contain ammoniated phyllosilicates that are not seen in the meteorite inventory. We propose that the Himalia parent body was heterogeneous and formed with materials similar to Ceres-like ammonium-bearing asteroids. Several small ($D\sim 10km$) irregular satellites closely track the colors and absorption bands of ``red'' Jovian Trojans, demonstrating that these compositions are retained amongst the products of collisions that occurred after Jovian capture. We report the first detection of aqueous alteration products in the retrograde satellite swarm, finding Ananke's 3 micron band to closely match phyllosilicates seen in C2 chondrites. Notably, objects with OH absorption features similar to the Trojan asteroid Eurybates are found in both the retrograde Pasiphae family and the prograde Himalia family, confounding a simple link between such materials and a single surface type. The irregular satellites appear consistent with some materials that experienced alteration from liquid water and others that did not. Consequently, Jupiter may have captured bodies that formed from different initial compositions, or bodies that experienced different levels of heating, driving differential alteration processes.
A JWST Transit of a Jupiter Analog I: Constraints on the Oblateness of Kepler-167e
Columbia University（哥伦比亚大学）；University of Groningen（格罗宁根大学）；Flatiron Institute（平顿研究所）；University of California, Santa Cruz（加州大学圣克鲁兹分校）；SRON Netherlands Institute for Space Research（荷兰空间研究所）；Academia Sinica Institute of Astronomy and Astrophysics（中央研究院天文及天文物理研究所）
Simultaneous retrieval of orbital phase resolved JWST/MIRI emission spectra of the hot Jupiter WASP-43b: evidence of water, ammonia and carbon monoxide
NIRCam yells at cloud: JWST MIRI imaging can directly detect exoplanets of the same temperature, mass, age, and orbital separation as Saturn and Jupiter
A JWST Transit of a Jupiter Analog: II. A Search for Exomoons
Columbia University（哥伦比亚大学）；Kapteyn Institute, University of Groningen（格罗宁根大学卡普坦研究所）；Department of Physics and Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology（麻省理工学院物理系与卡弗里天体物理学与空间研究研究所）；Academia Sinica Institute of Astronomy & Astrophysics（中央研究院天文及天文物理研究所）；SRON, Netherlands Institute for Space Research（荷兰空间研究所）
Molecular mapping of an exoplanet with JWST: detection of NH$_3$ and HCN in the temperate super-Jupiter Epsilon Indi Ab
Institut de Recherche en Astrophysique et Planétologie（天体物理学与行星学研究所在）；École polytechnique, Institut Polytechnique de Paris（巴黎综合理工学院，巴黎理工学院）；Observatoire de Paris（巴黎天文台）
利用JWST红外光谱和交叉相关技术，对直接成像的温带超级木星Epsilon Indi Ab进行分子测绘，可靠探测到NH3、H2O、CH4，并边缘性探测到CO2，验证了该方法在强恒星污染下的有效性。
A second visit to Eps Ind Ab with JWST: new photometry confirms ammonia and suggests thick clouds in the exoplanet atmosphere of the closest super-Jupiter
Max Planck Institute for Astronomy（马克斯·普朗克天文学研究所）；University of Texas at Austin（德克萨斯大学奥斯汀分校）；Space Telescope Science Institute（太空望远镜科学研究所）；Heidelberg University（海德堡大学）；Leiden University（莱顿大学）
Investing in the Unrivaled Potential of Wide-Separation Sub-Jupiter Exoplanet Detection and Characterisation with JWST -- Strategic Exoplanet Initiatives with HST and JWST White Paper
ExoEcho: Exoplanet Ephemerides Change Observations. III. A JWST Survey for Transit Timing Variations of 37 Exoplanets
School of Physics and Astronomy, Sun Yat-sen University（中山大学物理学院）；CSST Science Center for the Guangdong-Hong Kong-Macau Great Bay Area, Sun Yat-sen University（中山大学粤港澳大湾区空间望远镜科学中心）
JWST and HST Confirm Transit Timing Variations for the Ultra-Hot Jupiter TOI-2109 b
Carnegie Institution for Science（卡内基科学机构）；University of California San Diego（加州大学圣迭戈分校）；Carnegie Science Observatories（卡内基科学天文台）；Space Telescope Science Institute（太空望远镜科学研究所）；University of Oxford（牛津大学）；University of California, Santa Cruz（加州大学圣克鲁兹分校）；University of Hawai‘i（夏威夷大学）
A Binary Flux Calibrator Reveals the Scientific Potential of Short-integration JWST MIRI Imaging to Directly Detect sub-Jupiter Exoplanets
Eureka Scientific Inc.（Eureka科学公司）；University of Michigan（密歇根大学）；Max Planck Institute for Astronomy（马克斯·普朗克天文学研究所）；University of California Santa Cruz（加州大学圣克鲁兹分校）；Massachusetts Institute of Technology（麻省理工学院）；Johns Hopkins APL（约翰斯·霍普金斯大学应用物理实验室）
On the Detectability of Volcanic Exo-Ios That May Fuel Auroras on Super-Jupiters
University of Michigan（密歇根大学）；American Museum of Natural History（美国自然历史博物馆）；Trinity College Dublin, The University of Dublin（都柏林三一学院，都柏林大学）；Lowell Observatory（洛厄尔天文台）；University of California, Santa Cruz（加州大学圣克鲁兹分校）；Johns Hopkins APL（约翰斯·霍普金斯大学应用物理实验室）
The JWST Sub-Jupiters Survey: Direct Imaging Discovery of a Giant Planet and a Debris Disk Around the Young M-dwarf RX J0534.0-0221
Northwestern University（西北大学）；University of Arizona（亚利桑那大学）；University of Maryland, Baltimore County（马里兰大学巴尔的摩分校）；NASA-GSFC（美国宇航局戈达德太空飞行中心）；Space Telescope Science Institute (STScI)（空间望远镜科学研究所）
Precise Constraints on the Energy Budget of WASP-121 b from its JWST NIRISS/SOSS Phase Curve
McGill University（麦吉尔大学）；University of Michigan（密歇根大学）；University of Waterloo（滑铁卢大学）；University of Chicago（芝加哥大学）；University of British Columbia（不列颠哥伦比亚大学）；University of California, Los Angeles（加州大学洛杉矶分校）；Johns Hopkins University（约翰斯·霍普金斯大学）；University of Victoria（维多利亚大学）；Cornell University（康奈尔大学）；University of Oxford（牛津大学）
Horizontal and vertical exoplanet thermal structure from a JWST spectroscopic eclipse map
Cornell University（康奈尔大学）；University of Michigan（密歇根大学）；Arizona State University（亚利桑那州立大学）；University of Maryland, College Park（马里兰大学帕克分校）；Space Research Institute, Austrian Academy of Sciences（奥地利科学院空间研究所）；INAF - Turin Astrophysical Observatory（意大利国家天体物理研究所都灵天文台）；Carnegie Institution for Science（卡内基科学机构）；New York University Abu Dhabi（阿布扎比纽约大学）；University of Chicago（芝加哥大学）；University of California, Los Angeles（加州大学洛杉矶分校）；University of Central Florida（中佛罗里达大学）；German Aerospace Center (DLR)（德国航空航天中心）；University of Rome “Tor Vergata”（罗马托维加塔大学）；Max Planck Institute for Astronomy（马克斯·普朗克天文学研究所）；Department of Astronomy & Astrophysics, University of California Santa Cruz（加州大学圣克鲁兹分校天文与天体物理系）；Universidad Andres Bello（安德斯·贝略大学）；University of Kansas（堪萨斯大学）；Rijksuniversiteit Groningen（格罗宁根大学）；University of Amsterdam（阿姆斯特丹大学）；Space Telescope Science Institute（太空望远镜科学研究所）；Massachusetts Institute of Technology（麻省理工学院）；Steward Observatory, University of Arizona（亚利桑那大学斯图尔德天文台）；Johns Hopkins University（约翰斯·霍普金斯大学）
Flow-Driven Limb-Asymmetry of Haze Distribution Part I: An Analytical Framework for Predicting the Size Distribution of Photochemical Hazes Across the Two Limbs of hot-Jupiters
University of Oxford（牛津大学）；University of Exeter（埃克塞特大学）；Johns Hopkins University（约翰斯·霍普金斯大学）
Worlds Next Door. III. Indirect Evidence for Enhanced Atmospheric Metallicity and/or the Presence of Water Clouds in the Nearest Jupiter-analog $ε$ Eri b
Cahill Center for Astronomy and Astrophysics, California Institute of Technology（加州理工学院卡希尔天文与天体物理中心）；Department of Astronomy, University of Texas at Austin（德克萨斯大学奥斯汀分校天文学系）；Jet Propulsion Laboratory, California Institute of Technology（加州理工学院喷气推进实验室）；NRC Herzberg Astronomy and Astrophysics（国家研究委员会赫尔茨伯格天文学与天体物理学研究所）；Department of Earth, Planetary, and Space Sciences, University of California Los Angeles（加州大学洛杉矶分校地球、行星与空间科学系）
Jupiter-like uniform metal enrichment in a system of multiple giant exoplanets
University of California San Diego（加州大学圣迭戈分校）；California Institute of Technology（加州理工学院）；University of California, Santa Cruz（加州大学圣克鲁兹分校）；IPAC, Caltech（加州理工学院IPAC）；University of Hawaii, Institute for Astronomy（夏威夷大学天文学研究所）；Johns Hopkins University（约翰斯·霍普金斯大学）；Space Telescope Science Institute（太空望远镜科学研究所）；Jet Propulsion Laboratory, California Institute of Technology（加州理工学院喷气推进实验室）；Division of Geological and Planetary Sciences, California Institute of Technology（加州理工学院地质与行星科学系）
A Sulfur-Rich Atmosphere for the Young Jupiter Analog AF Lep b Reveals Significant Solid Accretion
University of California, Los Angeles（加州大学洛杉矶分校）；Northwestern University（西北大学）；University of California, Santa Cruz（加州大学圣克鲁兹分校）；University of California, San Diego（加州大学圣迭戈分校）；National Astronomical Observatory of Japan（日本国立天文台）；European Southern Observatory（欧洲南方天文台）；New Mexico State University（新墨西哥州立大学）
A Clearer View of HAT-P-1 b: JWST NIRSpec G395H Reveals Water, Carbon Dioxide, and Possibly Hydrogen Sulfide
Johns Hopkins University Applied Physics Laboratory（约翰斯·霍普金斯大学应用物理实验室）；William H. Miller III Department of Physics and Astronomy, Johns Hopkins University（约翰斯·霍普金斯大学威廉·H·米勒三世物理与天文学系）；School of Earth & Planetary Sciences, National Institute of Science Education and Research (NISER)（国家科学教育与研究研究所地球与行星科学学院）；Homi Bhabha National Institute（霍米·巴巴国立研究所）；Morton K. Blaustein Department of Earth & Planetary Sciences, Johns Hopkins University（约翰斯·霍普金斯大学莫顿·K·布拉斯坦地球与行星科学学院）；Space Telescope Science Institute（太空望远镜科学研究所）；School of Earth and Space Exploration, Arizona State University（亚利桑那州立大学地球与空间探索学院）；Department of Astrophysical Sciences, Princeton University（普林斯顿大学天体物理科学系）；Atmospheric, Oceanic, and Planetary Physics, University of Oxford（牛津大学大气、海洋与行星物理系）；Department of Physics and Astronomy, University of Exeter（埃克塞特大学物理与天文学系）
本研究结合 JWST、HST 的多波段光谱数据，证实热木星 HAT-P-1 b 大气富含水、二氧化碳，可能含硫化氢，金属丰度约为太阳的 10 倍，是热木星大气研究的基准天体。
