KMT-2017-BLG-0165Lb: A Super-Neptune mass planet Orbiting a Sun-like Host Star
Youn Kil Jung, Andrew Gould, Weicheng Zang, Kyu-Ha Hwang, Yoon-Hyun Ryu, Cheongho Han, Jennifer C. Yee, Michael D. Albrow, Sun-Ju Chung, In-Gu Shin, Yossi Shvar… 展开作者
Youn Kil Jung, Andrew Gould, Weicheng Zang, Kyu-Ha Hwang, Yoon-Hyun Ryu, Cheongho Han, Jennifer C. Yee, Michael D. Albrow, Sun-Ju Chung, In-Gu Shin, Yossi Shvartzvald, Wei Zhu, Sang-Mok Cha, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Matthew T. Penny, Shude Mao, Pascal Fouqué, Tianshu Wang
备注：
27 pages, 3 tables, 9 figures, accepted for publication in AJ
We report the discovery of a low mass-ratio planet $(q = 1.3\times10^{-4})$, i.e., 2.5 times higher than the Neptune/Sun ratio. The planetary system was discovered from the analysis of the KMT-2017-BLG-0165 microlensing event, which has an obvious short-term deviation from the underlying light curve produced by the host of the planet. Although the fit improvement with the microlens parallax effect is relatively low, one component of the parallax vector is strongly constrained from the light curve, making it possible to narrow down the uncertainties of the lens physical properties. A Bayesian analysis yields that the planet has a super-Neptune mass $(M_{2}=34_{-12}^{+15}~M_{\oplus})$ orbiting a Sun-like star $(M_{1}=0.76_{-0.27}^{+0.34}~M_{\odot})$ located at $4.5~{\rm kpc}$. The blended light is consistent with these host properties. The projected planet-host separation is $a_{\bot}={3.45_{-0.95}^{+0.98}}~{\rm AU}$, implying that the planet is located outside the snowline of the host, i.e., $a_{sl}\sim2.1~{\rm AU}$. KMT-2017-BLG-0165Lb is the sixteenth microlensing planet with mass ratio $q<3\times10^{-4}$. Using the fifteen of these planets with unambiguous mass-ratio measurements, we apply a likelihood analysis to investigate the form of the mass-ratio function in this regime. If we adopt a broken power law for the form of this function, then the break is at $q_{\rm br}\simeq0.55\times10^{-4}$, which is much lower than previously estimated. Moreover, the change of the power law slope, $ζ>3.3$ is quite severe. Alternatively, the distribution is also suggestive of a "pile-up" of planets at Neptune-like mass ratios, below which there is a dramatic drop in frequency.
KMT-2025-BLG-0975Lb and KMT-2025-BLG-1160Lb: Two Uranus-Mass Planets Beyond the Snow Line Discovered by Microlensing
Chungbuk National University（忠北国立大学）；Korea Astronomy and Space Science Institute（韩国天体宇宙科学研究所）；University of Warsaw（华沙大学）；Ohio State University（俄亥俄州立大学）；University of Canterbury（坎特伯雷大学）；University of Science and Technology（科学技术大学）
Testing KMTNet--PRIME Optical--Near-Infrared Source-Color Constraints in KMT-2024-BLG-0211 and KMT-2024-BLG-1522
The University of Osaka（大阪大学）；Massey University（梅西大学）；Ohio State University（俄亥俄州立大学）；Westlake University（西湖大学）；NASA Goddard Space Flight Center（美国宇航局戈达德太空飞行中心）；University of Maryland, College Park（马里兰大学帕克分校）
KMT-2025-BLG-1314 and KMT-2025-BLG-1392: two microlensing planetary/brown-dwarf candidates analyzed with differentiable code
Tsinghua University（清华大学）；Westlake University（西湖大学）；Korea Astronomy and Space Science Institute（韩国天文与空间科学研究院）；University of Canterbury（坎特伯雷大学）；Max-Planck-Institute for Astronomy（马克斯·普朗克天文学研究所）；Ohio State University（俄亥俄州立大学）；Chungbuk National University（忠北国立大学）；National University of Science and Technology (UST)（韩国科学技术院）
KMT-2024-BLG-0816/OGLE-2024-BLG-0519 -- A Microlensing Event with Candidate Free-Floating Planet Lens and Blended Light
University of Warsaw（华沙大学）；Korea Astronomy and Space Science Institute（韩国天文学与空间科学研究所）；Westlake University（西湖大学）；University of Canterbury（坎特伯雷大学）；Max-Planck-Institute for Astronomy（马克斯·普朗克天体物理学研究所）；Ohio State University（俄亥俄州立大学）；Chungbuk National University（忠北国立大学）；National University of Science and Technology (UST)（国立科学技术大学）；Weizmann Institute of Science（魏茨曼科学研究所）
Four Giant Planets from 2024 KMTNet Microlensing Campaign
Chungbuk National University（忠北国立大学）；University of Warsaw（华沙大学）；Massey University（梅西大学）；Korea Astronomy and Space Science Institute（韩国天体与空间科学研究所）；Tsinghua University（清华大学）；University of Canterbury（坎特伯雷大学）；Ohio State University（俄亥俄州立大学）；University of Science and Technology（科学技术大学）；Weizmann Institute of Science（魏茨曼科学研究所）；Westlake University（西湖大学）；University of Warwick（华威大学）；Villanova University（维拉诺瓦大学）；Nagoya University（名古屋大学）；NASA Goddard Space Flight Center（美国宇航局戈达德太空飞行中心）；University of Maryland, College Park（马里兰大学帕克分校）；Osaka University（大阪大学）；The Catholic University of America（美国天主教大学）；The University of Tokyo（东京大学）；Japan Aerospace Exploration Agency（日本宇宙航空研究开发机构）；Institut d'Astrophysique de Paris（巴黎天体物理研究所）；University of Auckland（奥克兰大学）；Kanto Gakuin University（关东学院大学）；Tel-Aviv University（特拉维夫大学）
Systematic KMTNet Planetary Anomaly Search. VI. Complete Sample of 2018 Sub-Prime-Field Planets
我们完成了对KMTNet Anomalysis确定的所有2018次主场微透镜行星的分析。在9个先前未发表的行星事件中，有6个明显是行星事件（KMT-2018-BLG-0030，KMT-2018-BLG-0087，KMT-2018-BLG-0247，OGLE-2018-BLG-0298，KMT-2018-BLG-2602和OGLE-2018-BLG-1119），而其余3个在性质上是模糊的。此外，有8个先前公布的次主场行星是由Anomalysts算法选出的。连同一篇关于2018年素场行星的配套论文（Gould et al. 2022），这项工作为基于KMTNet数据中识别的行星的行星质量比函数的首次统计分析奠定了基础。正如预期的那样（Zhu et al. 2014），2018年可能进入质量比分析的行星中有一半（17/33）具有非焦散交叉异常。然而，在5个具有行星-宿主质量比$q<10^{-3}$的非焦散异常中，只有1个是通过肉眼发现的（相比之下，12个具有$q>10^{-3}$的异常中有7个是通过肉眼发现的），这表明了半自动异常搜索的重要性。
Candidate Microlensing Brown Dwarfs in Binary Lens Systems from the 2023--2025 Observing Seasons
Chungbuk National University（忠北国立大学）；University of Warsaw（华沙大学）；Massey University（梅西大学）；Korea Astronomy and Space Science Institute（韩国天文学与空间科学研究所）；University of Canterbury（坎特伯雷大学）；Ohio State University（俄亥俄州立大学）；University of Science and Technology（科学技术大学）
Mass Production of 2023 KMTNet Microlensing Planets I: Low Mass Ratio
Korea Astronomy and Space Science Institute（韩国天文与空间科学研究所）；Astronomical Observatory, University of Warsaw（华沙大学天文台）；Westlake University（西湖大学）；Tsinghua University（清华大学）；University of Chinese Academy of Sciences（中国科学院大学）；Ohio State University（俄亥俄州立大学）；University of Canterbury（坎特伯雷大学）
Mass Production of 2023 KMTNet Microlensing Planets. II: Two Planets and A Brown Dwarf
Westlake University（西湖大学）；Tsinghua University（清华大学）；Korea Astronomy and Space Science Institute（韩国天体宇宙科学研究所）；Astronomical Observatory, University of Warsaw（华沙大学天文台）；Department of Earth and Space Science, Graduate School of Science, Osaka University（大阪大学理学研究科地球・宇宙科学系）；University of Canterbury, School of Physical and Chemical Sciences（坎特伯雷大学物理与化学科学学院）
Limits on a Host Star around a Saturn-mass Free-floating Planet Candidate KMT-2024-BLG-0792/OGLE-2024-BLG-0516
University of Warsaw（华沙大学）；École Normale Supérieure, Paris（巴黎高等师范学院）；European Southern Observatory（欧洲南方天文台）；Peking University（北京大学）；National Astronomical Observatories, Chinese Academy of Science（中国科学院国家天文台）
KMT-2025-BLG-2093: Free-Floating Planet Candidate Near the Shore of the Einstein Desert
Korea Astronomy and Space Science Institute（韩国天体宇宙科学研究所）；Ohio State University（俄亥俄州立大学）；Westlake University（西湖大学）；Tsinghua University（清华大学）；University of Canterbury（坎特伯雷大学）；Chungbuk National University（忠北国立大学）；National University of Science and Technology (UST)（韩国科学技术院）；Weizmann Institute of Science（魏茨曼科学研究所）
KMT-2025-BLG-1616Lb: First Microlensing Bound Planet From DREAMS
Westlake Institute for Advanced Study（西湖高等研究院）；Westlake University（西湖大学）；Korea Astronomy and Space Science Institute（韩国天文与空间科学研究所）；The University of Osaka（大阪大学）；Tsinghua University（清华大学）；Chungbuk National University（忠北国立大学）
