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href="/search/?searchtype=author&query=Shin%2C+I&start=200" class="pagination-link " aria-label="Page 5" aria-current="page">5 </a> </li> </ul> </nav> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2501.06293">arXiv:2501.06293</a> <span> [<a href="https://arxiv.org/pdf/2501.06293">pdf</a>, <a href="https://arxiv.org/format/2501.06293">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Artificial Intelligence">cs.AI</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/ada4b5">10.3847/1538-3881/ada4b5 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> LensNet: Enhancing Real-time Microlensing Event Discovery with Recurrent Neural Networks in the Korea Microlensing Telescope Network </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Via%C3%B1a%2C+J">Javier Via帽a</a>, <a href="/search/astro-ph?searchtype=author&query=Hwang%2C+K">Kyu-Ha Hwang</a>, <a href="/search/astro-ph?searchtype=author&query=de+Beurs%2C+Z">Zo毛 de Beurs</a>, <a href="/search/astro-ph?searchtype=author&query=Yee%2C+J+C">Jennifer C. Yee</a>, <a href="/search/astro-ph?searchtype=author&query=Vanderburg%2C+A">Andrew Vanderburg</a>, <a href="/search/astro-ph?searchtype=author&query=Albrow%2C+M+D">Michael D. Albrow</a>, <a href="/search/astro-ph?searchtype=author&query=Chung%2C+S">Sun-Ju Chung</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">Andrew Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Han%2C+C">Cheongho Han</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+Y+K">Youn Kil Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Ryu%2C+Y">Yoon-Hyun Ryu</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+I">In-Gu Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Shvartzvald%2C+Y">Yossi Shvartzvald</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+H">Hongjing Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Zang%2C+W">Weicheng Zang</a>, <a href="/search/astro-ph?searchtype=author&query=Cha%2C+S">Sang-Mok Cha</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Dong-Jin Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+S">Seung-Lee Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+C">Chung-Uk Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+D">Dong-Joo Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+Y">Yongseok Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Park%2C+B">Byeong-Gon Park</a>, <a href="/search/astro-ph?searchtype=author&query=Pogge%2C+R+W">Richard W. Pogge</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2501.06293v1-abstract-short" style="display: inline;"> Traditional microlensing event vetting methods require highly trained human experts, and the process is both complex and time-consuming. This reliance on manual inspection often leads to inefficiencies and constrains the ability to scale for widespread exoplanet detection, ultimately hindering discovery rates. To address the limits of traditional microlensing event vetting, we have developed LensN… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.06293v1-abstract-full').style.display = 'inline'; document.getElementById('2501.06293v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.06293v1-abstract-full" style="display: none;"> Traditional microlensing event vetting methods require highly trained human experts, and the process is both complex and time-consuming. This reliance on manual inspection often leads to inefficiencies and constrains the ability to scale for widespread exoplanet detection, ultimately hindering discovery rates. To address the limits of traditional microlensing event vetting, we have developed LensNet, a machine learning pipeline specifically designed to distinguish legitimate microlensing events from false positives caused by instrumental artifacts, such as pixel bleed trails and diffraction spikes. Our system operates in conjunction with a preliminary algorithm that detects increasing trends in flux. These flagged instances are then passed to LensNet for further classification, allowing for timely alerts and follow-up observations. Tailored for the multi-observatory setup of the Korea Microlensing Telescope Network (KMTNet) and trained on a rich dataset of manually classified events, LensNet is optimized for early detection and warning of microlensing occurrences, enabling astronomers to organize follow-up observations promptly. The internal model of the pipeline employs a multi-branch Recurrent Neural Network (RNN) architecture that evaluates time-series flux data with contextual information, including sky background, the full width at half maximum of the target star, flux errors, PSF quality flags, and air mass for each observation. We demonstrate a classification accuracy above 87.5%, and anticipate further improvements as we expand our training set and continue to refine the algorithm. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.06293v1-abstract-full').style.display = 'none'; document.getElementById('2501.06293v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2025. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">23 pages, 13 figures, Accepted for publication in the The Astronomical Journal</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">MSC Class:</span> 85-08 <span class="has-text-black-bis has-text-weight-semibold">ACM Class:</span> J.2 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> 2025 AJ </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2501.02193">arXiv:2501.02193</a> <span> [<a href="https://arxiv.org/pdf/2501.02193">pdf</a>, <a href="https://arxiv.org/ps/2501.02193">ps</a>, <a href="https://arxiv.org/format/2501.02193">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> MOA-2022-BLG-033Lb, KMT-2023-BLG-0119Lb, and KMT-2023-BLG-1896Lb: Three low mass-ratio microlensing planets detected through dip signals </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Han%2C+C">Cheongho Han</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+I+A">Ian A. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+Y+K">Youn Kil Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Albrow%2C+M+D">Michael D. Albrow</a>, <a href="/search/astro-ph?searchtype=author&query=Chung%2C+S">Sun-Ju Chung</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">Andrew Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Hwang%2C+K">Kyu-Ha Hwang</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+C">Chung-Uk Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Ryu%2C+Y">Yoon-Hyun Ryu</a>, <a href="/search/astro-ph?searchtype=author&query=Shvartzvald%2C+Y">Yossi Shvartzvald</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+I">In-Gu Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Yee%2C+J+C">Jennifer C. Yee</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+H">Hongjing Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Zang%2C+W">Weicheng Zang</a>, <a href="/search/astro-ph?searchtype=author&query=Cha%2C+S">Sang-Mok Cha</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Doeon Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Dong-Jin Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+S">Seung-Lee Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+D">Dong-Joo Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+Y">Yongseok Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Park%2C+B">Byeong-Gon Park</a>, <a href="/search/astro-ph?searchtype=author&query=Pogge%2C+R+W">Richard W. Pogge</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+F">Fumio Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Barry%2C+R">Richard Barry</a>, <a href="/search/astro-ph?searchtype=author&query=Bennett%2C+D+P">David P. Bennett</a> , et al. (23 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2501.02193v1-abstract-short" style="display: inline;"> We examined the anomalies in the light curves of the lensing events MOA-2022-BLG-033, KMT-2023-BLG-0119, and KMT-2023-BLG-1896. We conducted detailed modeling of the light curves to uncover the nature of the anomalies. This modeling revealed that all signals originated from planetary companions to the primary lens. The planet-to-host mass ratios are very low: $q\sim 7.5\times 10^{-5}$ for MOA-2022… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.02193v1-abstract-full').style.display = 'inline'; document.getElementById('2501.02193v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.02193v1-abstract-full" style="display: none;"> We examined the anomalies in the light curves of the lensing events MOA-2022-BLG-033, KMT-2023-BLG-0119, and KMT-2023-BLG-1896. We conducted detailed modeling of the light curves to uncover the nature of the anomalies. This modeling revealed that all signals originated from planetary companions to the primary lens. The planet-to-host mass ratios are very low: $q\sim 7.5\times 10^{-5}$ for MOA-2022-BLG-033, $q\sim 3.6\times 10^{-4}$ for KMT-2023-BLG-0119, and $q\sim 6.9\times 10^{-5}$ for KMT-2023-BLG-1896. The anomalies occurred as the source passed through the negative deviation region behind the central caustic along the planet-host axis. The solutions are subject to a common inner-outer degeneracy, resulting in variations in estimating the projected planet-host separation. For KMT-2023-BLG-1896, although the planetary scenario provides the best explanation of the anomaly, the binary companion scenario is marginally possible. We estimate the physical parameters of the planetary systems through Bayesian analyses based on the lensing observables. The analysis identifies MOA-2022-BLG-033L as a planetary system with an ice giant, approximately 12 times the mass of Earth, orbiting an early M dwarf star. The companion of KMT-2023-BLG-1896L is also an ice giant, with a mass around 16 Earth masses, orbiting a mid-K-type main-sequence star. The companion of KMT-2023-BLG-0119L, which has a mass about the mass of Saturn, orbits a mid-K-type dwarf star. The lens for MOA-2022-BLG-033 is highly likely to be located in the disk, whereas for the other events, the probabilities of the lens being in the disk or the bulge are roughly comparable. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.02193v1-abstract-full').style.display = 'none'; document.getElementById('2501.02193v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2025. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 pages, 10 figures, 6 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.09096">arXiv:2411.09096</a> <span> [<a href="https://arxiv.org/pdf/2411.09096">pdf</a>, <a href="https://arxiv.org/ps/2411.09096">ps</a>, <a href="https://arxiv.org/format/2411.09096">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> KMT-2021-BLG-0284, KMT-2022-BLG-2480, and KMT-2024-BLG-0412: Three microlensing events involving two lens masses and two source stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Han%2C+C">Cheongho Han</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">Andrzej Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+I+A">Ian A. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+C">Chung-Uk Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">Andrew Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Albrow%2C+M+D">Michael D. Albrow</a>, <a href="/search/astro-ph?searchtype=author&query=Chung%2C+S">Sun-Ju Chung</a>, <a href="/search/astro-ph?searchtype=author&query=Hwang%2C+K">Kyu-Ha Hwang</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+Y+K">Youn Kil Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Ryu%2C+Y">Yoon-Hyun Ryu</a>, <a href="/search/astro-ph?searchtype=author&query=Shvartzvald%2C+Y">Yossi Shvartzvald</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+I">In-Gu Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Yee%2C+J+C">Jennifer C. Yee</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+H">Hongjing Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Zang%2C+W">Weicheng Zang</a>, <a href="/search/astro-ph?searchtype=author&query=Cha%2C+S">Sang-Mok Cha</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Doeon Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Dong-Jin Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+S">Seung-Lee Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+D">Dong-Joo Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+Y">Yongseok Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Park%2C+B">Byeong-Gon Park</a>, <a href="/search/astro-ph?searchtype=author&query=Pogge%2C+R+W">Richard W. Pogge</a>, <a href="/search/astro-ph?searchtype=author&query=Mr%C3%B3z%2C+P">Przemek Mr贸z</a>, <a href="/search/astro-ph?searchtype=author&query=Szyma%C5%84ski%2C+M+K">Micha艂 K. Szyma艅ski</a> , et al. (37 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2411.09096v1-abstract-short" style="display: inline;"> We carried out a project involving the systematic analysis of microlensing data from the Korea Microlensing Telescope Network survey. The aim of this project is to identify lensing events with complex anomaly features that are difficult to explain using standard binary-lens or binary-source models. Our investigation reveals that the light curves of microlensing events KMT-2021-BLG-0284, KMT-2022-B… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.09096v1-abstract-full').style.display = 'inline'; document.getElementById('2411.09096v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.09096v1-abstract-full" style="display: none;"> We carried out a project involving the systematic analysis of microlensing data from the Korea Microlensing Telescope Network survey. The aim of this project is to identify lensing events with complex anomaly features that are difficult to explain using standard binary-lens or binary-source models. Our investigation reveals that the light curves of microlensing events KMT-2021-BLG-0284, KMT-2022-BLG-2480, and KMT-2024-BLG-0412 display highly complex patterns with three or more anomaly features. These features cannot be adequately explained by a binary-lens (2L1S) model alone. However, the 2L1S model can effectively describe certain segments of the light curve. By incorporating an additional source into the modeling, we identified a comprehensive model that accounts for all the observed anomaly features. Bayesian analysis, based on constraints provided by lensing observables, indicates that the lenses of KMT-2021-BLG-0284 and KMT-2024-BLG-0412 are binary systems composed of M dwarfs. For KMT-2022-BLG-2480, the primary lens is an early K-type main-sequence star with an M dwarf companion. The lenses of KMT-2021-BLG-0284 and KMT-2024-BLG-0412 are likely located in the bulge, whereas the lens of KMT-2022-BLG-2480 is more likely situated in the disk. In all events, the binary stars of the sources have similar magnitudes due to a detection bias favoring binary source events with a relatively bright secondary source star, which increases detection efficiency. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.09096v1-abstract-full').style.display = 'none'; document.getElementById('2411.09096v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 pages, 9 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.05268">arXiv:2411.05268</a> <span> [<a href="https://arxiv.org/pdf/2411.05268">pdf</a>, <a href="https://arxiv.org/ps/2411.05268">ps</a>, <a href="https://arxiv.org/format/2411.05268">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> KMT-2024-BLG-1044L: A sub-Uranus microlensing planet around a host at the star-brown dwarf mass boundary </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Han%2C+C">Cheongho Han</a>, <a href="/search/astro-ph?searchtype=author&query=Ryu%2C+Y">Yoon-Hyun Ryu</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+C">Chung-Uk Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">Andrew Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Albrow%2C+M+D">Michael D. Albrow</a>, <a href="/search/astro-ph?searchtype=author&query=Chung%2C+S">Sun-Ju Chung</a>, <a href="/search/astro-ph?searchtype=author&query=Hwang%2C+K">Kyu-Ha Hwang</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+Y+K">Youn Kil Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Shvartzvald%2C+Y">Yossi Shvartzvald</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+I">In-Gu Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Yee%2C+J+C">Jennifer C. Yee</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+H">Hongjing Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Zang%2C+W">Weicheng Zang</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Doeon Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Dong-Jin Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Park%2C+B">Byeong-Gon Park</a>, <a href="/search/astro-ph?searchtype=author&query=Pogge%2C+R+W">Richard W. Pogge</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2411.05268v1-abstract-short" style="display: inline;"> We analysed microlensing data to uncover the nature of the anomaly that appeared near the peak of the short-timescale microlensing event KMT-2024-BLG-1044. Despite the anomaly's brief duration of less than a day, it was densely observed through high-cadence monitoring conducted by the KMTNet survey. Detailed modelling of the light curve confirmed the planetary origin of the anomaly and revealed tw… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.05268v1-abstract-full').style.display = 'inline'; document.getElementById('2411.05268v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.05268v1-abstract-full" style="display: none;"> We analysed microlensing data to uncover the nature of the anomaly that appeared near the peak of the short-timescale microlensing event KMT-2024-BLG-1044. Despite the anomaly's brief duration of less than a day, it was densely observed through high-cadence monitoring conducted by the KMTNet survey. Detailed modelling of the light curve confirmed the planetary origin of the anomaly and revealed two possible solutions, due to an inner--outer degeneracy. The two solutions provide different measured planet parameters: $(s, q)_{\rm inner} = [1.0883 \pm 0.0027, (3.125 \pm 0.248)\times 10^{-4}]$ for the inner solutions and $(s, q)_{\rm outer} = [1.0327 \pm 0.0054, (3.350 \pm 0.316)\times 10^{-4}]$ for the outer solutions. Using Bayesian analysis with constraints provided by the short event timescale ($t_{\rm E} \sim 9.1$~day) and the small angular Einstein radius ($胃_{\rm E}\sim 0.16$~mas for the inner solution and $\sim 0.10$~mas for the outer solutio), we determined that the lens is a planetary system consisting of a host near the boundary between a star and a brown dwarf and a planet with a mass lower than that of Uranus. The discovery of the planetary system highlights the crucial role of the microlensing technique in detecting planets that orbit substellar brown dwarfs or very low-mass stars. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.05268v1-abstract-full').style.display = 'none'; document.getElementById('2411.05268v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 10 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.12227">arXiv:2409.12227</a> <span> [<a href="https://arxiv.org/pdf/2409.12227">pdf</a>, <a href="https://arxiv.org/format/2409.12227">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> Observations of Microlensed Images with Dual-field Interferometry: On-sky Demonstration and Prospects </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mroz%2C+P">P. Mroz</a>, <a href="/search/astro-ph?searchtype=author&query=Dong%2C+S">S. Dong</a>, <a href="/search/astro-ph?searchtype=author&query=Merand%2C+A">A. Merand</a>, <a href="/search/astro-ph?searchtype=author&query=Shangguan%2C+J">J. Shangguan</a>, <a href="/search/astro-ph?searchtype=author&query=Woillez%2C+J">J. Woillez</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">A. Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">A. Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Eisenhauer%2C+F">F. Eisenhauer</a>, <a href="/search/astro-ph?searchtype=author&query=Ryu%2C+Y+-">Y. -H. Ryu</a>, <a href="/search/astro-ph?searchtype=author&query=Wu%2C+Z">Z. Wu</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+Z">Z. Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+H">H. Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Bourdarot%2C+G">G. Bourdarot</a>, <a href="/search/astro-ph?searchtype=author&query=Defrere%2C+D">D. Defrere</a>, <a href="/search/astro-ph?searchtype=author&query=Drescher%2C+A">A. Drescher</a>, <a href="/search/astro-ph?searchtype=author&query=Fabricius%2C+M">M. Fabricius</a>, <a href="/search/astro-ph?searchtype=author&query=Garcia%2C+P">P. Garcia</a>, <a href="/search/astro-ph?searchtype=author&query=Genzel%2C+R">R. Genzel</a>, <a href="/search/astro-ph?searchtype=author&query=Gillessen%2C+S">S. Gillessen</a>, <a href="/search/astro-ph?searchtype=author&query=Honig%2C+S+F">S. F. Honig</a>, <a href="/search/astro-ph?searchtype=author&query=Kreidberg%2C+L">L. Kreidberg</a>, <a href="/search/astro-ph?searchtype=author&query=Bouquin%2C+J+-+L">J. -B. Le Bouquin</a>, <a href="/search/astro-ph?searchtype=author&query=Lutz%2C+D">D. Lutz</a>, <a href="/search/astro-ph?searchtype=author&query=Millour%2C+F">F. Millour</a>, <a href="/search/astro-ph?searchtype=author&query=Ott%2C+T">T. Ott</a> , et al. (35 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2409.12227v2-abstract-short" style="display: inline;"> Interferometric observations of gravitational microlensing events offer an opportunity for precise, efficient, and direct mass and distance measurements of lensing objects, especially those of isolated neutron stars and black holes. However, such observations have previously been possible for only a handful of extremely bright events. The recent development of a dual-field interferometer, GRAVITY… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.12227v2-abstract-full').style.display = 'inline'; document.getElementById('2409.12227v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.12227v2-abstract-full" style="display: none;"> Interferometric observations of gravitational microlensing events offer an opportunity for precise, efficient, and direct mass and distance measurements of lensing objects, especially those of isolated neutron stars and black holes. However, such observations have previously been possible for only a handful of extremely bright events. The recent development of a dual-field interferometer, GRAVITY Wide, has made it possible to reach out to significantly fainter objects and increase the pool of microlensing events amenable to interferometric observations by two orders of magnitude. Here, we present the first successful observation of a microlensing event with GRAVITY Wide and the resolution of microlensed images in the event OGLE-2023-BLG-0061/KMT-2023-BLG-0496. We measure the angular Einstein radius of the lens with subpercent precision, $胃_{\rm E} = 1.280 \pm 0.009$ mas. Combined with the microlensing parallax detected from the event light curve, the mass and distance to the lens are found to be $0.472 \pm 0.012\,M_{\odot}$ and $1.81 \pm 0.05$ kpc, respectively. We present the procedure for the selection of targets for interferometric observations and discuss possible systematic effects affecting GRAVITY Wide data. This detection demonstrates the capabilities of the new instrument, and it opens up completely new possibilities for the follow-up of microlensing events and future routine discoveries of isolated neutron stars and black holes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.12227v2-abstract-full').style.display = 'none'; document.getElementById('2409.12227v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2408.11248">arXiv:2408.11248</a> <span> [<a href="https://arxiv.org/pdf/2408.11248">pdf</a>, <a href="https://arxiv.org/ps/2408.11248">ps</a>, <a href="https://arxiv.org/format/2408.11248">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> Microlensing brown-dwarf companions in binaries detected during the 2022 and 2023 seasons </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Han%2C+C">Cheongho Han</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+I+A">Ian A. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">Andrzej Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+C">Chung-Uk Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">Andrew Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Albrow%2C+M+D">Michael D. Albrow</a>, <a href="/search/astro-ph?searchtype=author&query=Chung%2C+S">Sun-Ju Chung</a>, <a href="/search/astro-ph?searchtype=author&query=Hwang%2C+K">Kyu-Ha Hwang</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+Y+K">Youn Kil Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Ryu%2C+Y">Yoon-Hyun Ryu</a>, <a href="/search/astro-ph?searchtype=author&query=Shvartzvald%2C+Y">Yossi Shvartzvald</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+I">In-Gu Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Yee%2C+J+C">Jennifer C. Yee</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+H">Hongjing Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Zang%2C+W">Weicheng Zang</a>, <a href="/search/astro-ph?searchtype=author&query=Cha%2C+S">Sang-Mok Cha</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Doeon Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Dong-Jin Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+S">Seung-Lee Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+D">Dong-Joo Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+Y">Yongseok Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Park%2C+B">Byeong-Gon Park</a>, <a href="/search/astro-ph?searchtype=author&query=Pogge%2C+R+W">Richard W. Pogge</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+F">Fumio Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Bando%2C+K">Ken Bando</a> , et al. (41 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2408.11248v1-abstract-short" style="display: inline;"> Building on previous works to construct a homogeneous sample of brown dwarfs in binary systems, we investigate microlensing events detected by the Korea Microlensing Telescope Network (KMTNet) survey during the 2022 and 2023 seasons. Given the difficulty in distinguishing brown-dwarf events from those produced by binary lenses with nearly equal-mass components, we analyze all lensing events detect… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.11248v1-abstract-full').style.display = 'inline'; document.getElementById('2408.11248v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.11248v1-abstract-full" style="display: none;"> Building on previous works to construct a homogeneous sample of brown dwarfs in binary systems, we investigate microlensing events detected by the Korea Microlensing Telescope Network (KMTNet) survey during the 2022 and 2023 seasons. Given the difficulty in distinguishing brown-dwarf events from those produced by binary lenses with nearly equal-mass components, we analyze all lensing events detected during the seasons that exhibit anomalies characteristic of binary-lens systems. Using the same criteria consistently applied in previous studies, we identify six additional brown dwarf candidates through the analysis of lensing events KMT-2022-BLG-0412, KMT-2022-BLG-2286, KMT-2023-BLG-0201, KMT-2023-BLG-0601, KMT-2023-BLG-1684, and KMT-2023-BLG-1743. An examination of the mass posteriors shows that the median mass of the lens companions ranges from 0.02 $M_\odot$ to 0.05 $M_\odot$, indicating that these companions fall within the brown-dwarf mass range. The mass of the primary lenses ranges from 0.11 $M_\odot$ to 0.68 $M_\odot$, indicating that they are low-mass stars with substantially lower masses compared to the Sun. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.11248v1-abstract-full').style.display = 'none'; document.getElementById('2408.11248v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 17 figures, 12 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.17002">arXiv:2407.17002</a> <span> [<a href="https://arxiv.org/pdf/2407.17002">pdf</a>, <a href="https://arxiv.org/ps/2407.17002">ps</a>, <a href="https://arxiv.org/format/2407.17002">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> KMT-2021-BLG-2609Lb and KMT-2022-BLG-0303Lb: Microlensing planets identified through signals produced by major-image perturbations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Han%2C+C">Cheongho Han</a>, <a href="/search/astro-ph?searchtype=author&query=Albrow%2C+M+D">Michael D. Albrow</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+C">Chung-Uk Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Chung%2C+S">Sun-Ju Chung</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">Andrew Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Hwang%2C+K">Kyu-Ha Hwang</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+Y+K">Youn Kil Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+C">Chung-Uk Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Ryu%2C+Y">Yoon-Hyun Ryu</a>, <a href="/search/astro-ph?searchtype=author&query=Shvartzvald%2C+Y">Yossi Shvartzvald</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+I">In-Gu Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Yee%2C+J+C">Jennifer C. Yee</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+H">Hongjing Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Zang%2C+W">Weicheng Zang</a>, <a href="/search/astro-ph?searchtype=author&query=Cha%2C+S">Sang-Mok Cha</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Doeon Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Dong-Jin Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+S">Seung-Lee Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+D">Dong-Joo Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+Y">Yongseok Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Park%2C+B">Byeong-Gon Park</a>, <a href="/search/astro-ph?searchtype=author&query=Pogge%2C+R+W">Richard W. Pogge</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2407.17002v1-abstract-short" style="display: inline;"> We investigate microlensing data collected by the Korea Microlensing Telescope Network (KMTNet) survey. Our investigation reveals that the light curves of two lensing events, KMT-2021-BLG-2609 and KMT-2022-BLG-0303, exhibit a similar anomaly, in which short-term positive deviations appear on the sides of the low-magnification lensing light curves. To unravel the nature of these anomalies, we metic… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.17002v1-abstract-full').style.display = 'inline'; document.getElementById('2407.17002v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.17002v1-abstract-full" style="display: none;"> We investigate microlensing data collected by the Korea Microlensing Telescope Network (KMTNet) survey. Our investigation reveals that the light curves of two lensing events, KMT-2021-BLG-2609 and KMT-2022-BLG-0303, exhibit a similar anomaly, in which short-term positive deviations appear on the sides of the low-magnification lensing light curves. To unravel the nature of these anomalies, we meticulously analyze each of the lensing events. Our investigations reveal that these anomalies stem from a shared channel, wherein the source passed near the planetary caustic induced by a planet with projected separations from the host star exceeding the Einstein radius. We find that interpreting the anomaly of KMT-2021-BLG-2609 is complicated by the "inner--outer" degeneracy, whereas for KMT-2022-BLG-0303, there is no such issue despite similar lens-system configurations. In addition to this degeneracy, interpreting the anomaly in KMT-2021-BLG-2609 involves an additional degeneracy between a pair of solutions, in which the source partially envelops the caustic and the other three solutions in which the source fully envelopes the caustic. As in an earlier case of this so-called von Schlieffen--Cannae degeneracy, the former solutions have substantially higher mass ratio. Through Bayesian analyses conducted based on the measured lensing observables of the event time scale and angular Einstein radius, the host of KMT-2021-BLG-2609L is determined to be a low-mass star with a mass $\sim 0.2~M_\odot$ in terms of a median posterior value, while the planet's mass ranges from approximately 0.032 to 0.112 times that of Jupiter, depending on the solutions. For the planetary system KMT-2022-BLG-0303L, it features a planet with a mass of approximately $0.51~M_{\rm J}$ and a host star with a mass of about $0.37~M_\odot$. In both cases, the lenses are most likely situated in the bulge. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.17002v1-abstract-full').style.display = 'none'; document.getElementById('2407.17002v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 11 figures, 6 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.13740">arXiv:2407.13740</a> <span> [<a href="https://arxiv.org/pdf/2407.13740">pdf</a>, <a href="https://arxiv.org/format/2407.13740">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> Analysis of the full Spitzer microlensing sample I: Dark remnant candidates and Gaia predictions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Rybicki%2C+K+A">Krzysztof A. Rybicki</a>, <a href="/search/astro-ph?searchtype=author&query=Shvartzvald%2C+Y">Yossi Shvartzvald</a>, <a href="/search/astro-ph?searchtype=author&query=Yee%2C+J+C">Jennifer C. Yee</a>, <a href="/search/astro-ph?searchtype=author&query=Novati%2C+S+C">Sebastiano Calchi Novati</a>, <a href="/search/astro-ph?searchtype=author&query=Ofek%2C+E+O">Eran O. Ofek</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+I+A">Ian A. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Beichman%2C+C">Charles Beichman</a>, <a href="/search/astro-ph?searchtype=author&query=Bryden%2C+G">Geoff Bryden</a>, <a href="/search/astro-ph?searchtype=author&query=Carey%2C+S">Sean Carey</a>, <a href="/search/astro-ph?searchtype=author&query=Henderson%2C+C">Calen Henderson</a>, <a href="/search/astro-ph?searchtype=author&query=Zhu%2C+W">Wei Zhu</a>, <a href="/search/astro-ph?searchtype=author&query=Fausnaugh%2C+M+M">Michael M. Fausnaugh</a>, <a href="/search/astro-ph?searchtype=author&query=Wibking%2C+B">Benjamin Wibking</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">Andrzej Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Poleski%2C+R">Radek Poleski</a>, <a href="/search/astro-ph?searchtype=author&query=Mr%C3%B3z%2C+P">Przemek Mr贸z</a>, <a href="/search/astro-ph?searchtype=author&query=Szyma%C5%84ski%2C+M+K">Michal K. Szyma艅ski</a>, <a href="/search/astro-ph?searchtype=author&query=Soszy%C5%84ski%2C+I">Igor Soszy艅ski</a>, <a href="/search/astro-ph?searchtype=author&query=Pietrukowicz%2C+P">Pawe艂 Pietrukowicz</a>, <a href="/search/astro-ph?searchtype=author&query=Koz%C5%82owski%2C+S">Szymon Koz艂owski</a>, <a href="/search/astro-ph?searchtype=author&query=Skowron%2C+J">Jan Skowron</a>, <a href="/search/astro-ph?searchtype=author&query=Ulaczyk%2C+K">Krzysztof Ulaczyk</a>, <a href="/search/astro-ph?searchtype=author&query=Iwanek%2C+P">Patryk Iwanek</a>, <a href="/search/astro-ph?searchtype=author&query=Wrona%2C+M">Marcin Wrona</a>, <a href="/search/astro-ph?searchtype=author&query=Ryu%2C+Y">Yoon-Hyun Ryu</a> , et al. (48 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2407.13740v1-abstract-short" style="display: inline;"> In the pursuit of understanding the population of stellar remnants within the Milky Way, we analyze the sample of $\sim 950$ microlensing events observed by the Spitzer Space Telescope between 2014 and 2019. In this study we focus on a sub-sample of nine microlensing events, selected based on their long timescales, small microlensing parallaxes and joint observations by the Gaia mission, to increa… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.13740v1-abstract-full').style.display = 'inline'; document.getElementById('2407.13740v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.13740v1-abstract-full" style="display: none;"> In the pursuit of understanding the population of stellar remnants within the Milky Way, we analyze the sample of $\sim 950$ microlensing events observed by the Spitzer Space Telescope between 2014 and 2019. In this study we focus on a sub-sample of nine microlensing events, selected based on their long timescales, small microlensing parallaxes and joint observations by the Gaia mission, to increase the probability that the chosen lenses are massive and the mass is measurable. Among the selected events we identify lensing black holes and neutron star candidates, with potential confirmation through forthcoming release of the Gaia time-series astrometry in 2026. Utilizing Bayesian analysis and Galactic models, along with the Gaia Data Release 3 proper motion data, four good candidates for dark remnants were identified: OGLE-2016-BLG-0293, OGLE-2018-BLG-0483, OGLE-2018-BLG-0662, and OGLE-2015-BLG-0149, with lens masses of $2.98^{+1.75}_{-1.28}~M_{\odot}$, $4.65^{+3.12}_{-2.08}~M_{\odot}$, $3.15^{+0.66}_{-0.64}~M_{\odot}$ and $1.4^{+0.75}_{-0.55}~M_{\odot}$, respectively. Notably, the first two candidates are expected to exhibit astrometric microlensing signals detectable by Gaia, offering the prospect of validating the lens masses. The methodologies developed in this work will be applied to the full Spitzer microlensing sample, populating and analyzing the time-scale ($t_{\rm E}$) vs. parallax ($蟺_{\rm E}$) diagram to derive constraints on the population of lenses in general and massive remnants in particular. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.13740v1-abstract-full').style.display = 'none'; document.getElementById('2407.13740v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">submitted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.10547">arXiv:2406.10547</a> <span> [<a href="https://arxiv.org/pdf/2406.10547">pdf</a>, <a href="https://arxiv.org/ps/2406.10547">ps</a>, <a href="https://arxiv.org/format/2406.10547">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> Four microlensing giant planets detected through signals produced by minor-image perturbations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Han%2C+C">Cheongho Han</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+I+A">Ian A. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+C">Chung-Uk Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">Andrew Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Albrow%2C+M+D">Michael D. Albrow</a>, <a href="/search/astro-ph?searchtype=author&query=Chung%2C+S">Sun-Ju Chung</a>, <a href="/search/astro-ph?searchtype=author&query=Hwang%2C+K">Kyu-Ha Hwang</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+Y+K">Youn Kil Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Ryu%2C+Y">Yoon-Hyun Ryu</a>, <a href="/search/astro-ph?searchtype=author&query=Shvartzvald%2C+Y">Yossi Shvartzvald</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+I">In-Gu Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Yee%2C+J+C">Jennifer C. Yee</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+H">Hongjing Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Zang%2C+W">Weicheng Zang</a>, <a href="/search/astro-ph?searchtype=author&query=Cha%2C+S">Sang-Mok Cha</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Doeon Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Dong-Jin Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+S">Seung-Lee Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+D">Dong-Joo Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+Y">Yongseok Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Park%2C+B">Byeong-Gon Park</a>, <a href="/search/astro-ph?searchtype=author&query=Pogge%2C+R+W">Richard W. Pogge</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+F">Fumio Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Bando%2C+K">Ken Bando</a>, <a href="/search/astro-ph?searchtype=author&query=Barry%2C+R">Richard Barry</a> , et al. (41 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2406.10547v1-abstract-short" style="display: inline;"> We investigated the nature of the anomalies appearing in four microlensing events KMT-2020-BLG-0757, KMT-2022-BLG-0732, KMT-2022-BLG-1787, and KMT-2022-BLG-1852. The light curves of these events commonly exhibit initial bumps followed by subsequent troughs that extend across a substantial portion of the light curves. We performed thorough modeling of the anomalies to elucidate their characteristic… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.10547v1-abstract-full').style.display = 'inline'; document.getElementById('2406.10547v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.10547v1-abstract-full" style="display: none;"> We investigated the nature of the anomalies appearing in four microlensing events KMT-2020-BLG-0757, KMT-2022-BLG-0732, KMT-2022-BLG-1787, and KMT-2022-BLG-1852. The light curves of these events commonly exhibit initial bumps followed by subsequent troughs that extend across a substantial portion of the light curves. We performed thorough modeling of the anomalies to elucidate their characteristics. Despite their prolonged durations, which differ from the usual brief anomalies observed in typical planetary events, our analysis revealed that each anomaly in these events originated from a planetary companion located within the Einstein ring of the primary star. It was found that the initial bump arouse when the source star crossed one of the planetary caustics, while the subsequent trough feature occurred as the source traversed the region of minor image perturbations lying between the pair of planetary caustics. The estimated masses of the host and planet, their mass ratios, and the distance to the discovered planetary systems are $(M_{\rm host}/M_\odot, M_{\rm planet}/M_{\rm J}, q/10^{-3}, \dl/{\rm kpc}) = (0.58^{+0.33}_{-0.30}, 10.71^{+6.17}_{-5.61}, 17.61\pm 2.25,6.67^{+0.93}_{-1.30})$ for KMT-2020-BLG-0757, $(0.53^{+0.31}_{-0.31}, 1.12^{+0.65}_{-0.65}, 2.01 \pm 0.07, 6.66^{+1.19}_{-1.84})$ for KMT-2022-BLG-0732, $(0.42^{+0.32}_{-0.23}, 6.64^{+4.98}_{-3.64}, 15.07\pm 0.86, 7.55^{+0.89}_{-1.30})$ for KMT-2022-BLG-1787, and $(0.32^{+0.34}_{-0.19}, 4.98^{+5.42}_{-2.94}, 8.74\pm 0.49, 6.27^{+0.90}_{-1.15})$ for KMT-2022-BLG-1852. These parameters indicate that all the planets are giants with masses exceeding the mass of Jupiter in our solar system and the hosts are low-mass stars with masses substantially less massive than the Sun. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.10547v1-abstract-full').style.display = 'none'; document.getElementById('2406.10547v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 12 figures, 7 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.16857">arXiv:2405.16857</a> <span> [<a href="https://arxiv.org/pdf/2405.16857">pdf</a>, <a href="https://arxiv.org/ps/2405.16857">ps</a>, <a href="https://arxiv.org/format/2405.16857">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> KMT-2023-BLG-2669: Ninth Free-floating Planet Candidate with $胃_{\rm E}$ measurements </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Jung%2C+Y+K">Youn Kil Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Hwang%2C+K">Kyu-Ha Hwang</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+H">Hongjing Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">Andrew Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Yee%2C+J+C">Jennifer C. Yee</a>, <a href="/search/astro-ph?searchtype=author&query=Han%2C+C">Cheongho Han</a>, <a href="/search/astro-ph?searchtype=author&query=Albrow%2C+M+D">Michael D. Albrow</a>, <a href="/search/astro-ph?searchtype=author&query=Chung%2C+S">Sun-Ju Chung</a>, <a href="/search/astro-ph?searchtype=author&query=Ryu%2C+Y">Yoon-Hyun Ryu</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+I">In-Gu Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Shvartzvald%2C+Y">Yossi Shvartzvald</a>, <a href="/search/astro-ph?searchtype=author&query=Zang%2C+W">Weicheng Zang</a>, <a href="/search/astro-ph?searchtype=author&query=Cha%2C+S">Sang-Mok Cha</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Dong-Jin Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+S">Seung-Lee Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+C">Chung-Uk Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+D">Dong-Joo Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+Y">Yongseok Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Park%2C+B">Byeong-Gon Park</a>, <a href="/search/astro-ph?searchtype=author&query=Pogge%2C+R+W">Richard W. Pogge</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.16857v2-abstract-short" style="display: inline;"> We report a free-floating planet (FFP) candidate identified from the analysis of the microlensing event KMT-2023-BLG-2669. The lensing light curve is characterized by a short duration $(\lesssim 3\,{\rm days})$ and a small amplitude $(\lesssim 0.7\,{\rm mag})$. From the analysis, we find the Einstein timescale of $t_{\rm E} \backsimeq 0.33\,{\rm days}$ and the Einstein radius of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.16857v2-abstract-full').style.display = 'inline'; document.getElementById('2405.16857v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.16857v2-abstract-full" style="display: none;"> We report a free-floating planet (FFP) candidate identified from the analysis of the microlensing event KMT-2023-BLG-2669. The lensing light curve is characterized by a short duration $(\lesssim 3\,{\rm days})$ and a small amplitude $(\lesssim 0.7\,{\rm mag})$. From the analysis, we find the Einstein timescale of $t_{\rm E} \backsimeq 0.33\,{\rm days}$ and the Einstein radius of $胃_{\rm E} \backsimeq 4.41\,渭{\rm as}$. These measurements enable us to infer the lens mass as $M = 8\,M_{\oplus} (蟺_{\rm rel} / 0.1\,{\rm mas})^{-1}$, where $蟺_{\rm rel}$ is the relative lens-source parallax. The inference implies that the lens is a sub-Neptune- to Saturn-mass object depending on its unknown distance. This is the ninth isolated planetary-mass microlens with $胃_{\rm E} < 10\,渭{\rm as}$, which (as shown by \citealt{gould22}) is a useful threshold for a FFP candidate. We conduct extensive searches for possible signals of a host star in the light curve, but find no strong evidence for the host. We investigate the possibility of using late-time high-resolution imaging to probe for possible hosts. In particular, we discuss that for the case of finite-source point-lens FFP candidates, it would be possible to search for very wide separation hosts immediately, although such searches are "high-risk, high-reward". <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.16857v2-abstract-full').style.display = 'none'; document.getElementById('2405.16857v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">26 pages, 6 figures, accepted in publication in AJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.07514">arXiv:2405.07514</a> <span> [<a href="https://arxiv.org/pdf/2405.07514">pdf</a>, <a href="https://arxiv.org/ps/2405.07514">ps</a>, <a href="https://arxiv.org/format/2405.07514">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> KMT-2023-BLG-1866Lb: Microlensing super-Earth around an M dwarf host </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Han%2C+C">Cheongho Han</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+I+A">Ian A. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">Andrzej Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+C">Chung-Uk Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">Andrew Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Albrow%2C+M+D">Michael D. Albrow</a>, <a href="/search/astro-ph?searchtype=author&query=Chung%2C+S">Sun-Ju Chung</a>, <a href="/search/astro-ph?searchtype=author&query=Hwang%2C+K">Kyu-Ha Hwang</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+Y+K">Youn Kil Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Ryu%2C+Y">Yoon-Hyun Ryu</a>, <a href="/search/astro-ph?searchtype=author&query=Shvartzvald%2C+Y">Yossi Shvartzvald</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+I">In-Gu Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Yee%2C+J+C">Jennifer C. Yee</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+H">Hongjing Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Zang%2C+W">Weicheng Zang</a>, <a href="/search/astro-ph?searchtype=author&query=Cha%2C+S">Sang-Mok Cha</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Doeon Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Dong-Jin Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+S">Seung-Lee Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+D">Dong-Joo Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+Y">Yongseok Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Park%2C+B">Byeong-Gon Park</a>, <a href="/search/astro-ph?searchtype=author&query=Pogge%2C+R+W">Richard W. Pogge</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+F">Fumio Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Bando%2C+K">Ken Bando</a> , et al. (42 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.07514v1-abstract-short" style="display: inline;"> We investigate the nature of the short-term anomaly that appears in the lensing light curve of KMT-2023-BLG-1866. The anomaly was only partly covered due to its short duration, less than a day, coupled with cloudy weather conditions and restricted nighttime duration. Considering intricacy of interpreting partially covered signals, we thoroughly explore all potential degenerate solutions. Through t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.07514v1-abstract-full').style.display = 'inline'; document.getElementById('2405.07514v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.07514v1-abstract-full" style="display: none;"> We investigate the nature of the short-term anomaly that appears in the lensing light curve of KMT-2023-BLG-1866. The anomaly was only partly covered due to its short duration, less than a day, coupled with cloudy weather conditions and restricted nighttime duration. Considering intricacy of interpreting partially covered signals, we thoroughly explore all potential degenerate solutions. Through this process, we identify three planetary scenarios that equally well account for the observed anomaly. These scenarios are characterized by the specific planetary parameters: $(s, q)_{\rm inner} = [0.9740 \pm 0.0083, (2.46 \pm 1.07) \times 10^{-5}]$, $(s, q)_{\rm intermediate} = [0.9779 \pm 0.0017, (1.56 \pm 0.25)\times 10^{-5}]$, and $(s, q)_{\rm outer} = [0.9894 \pm 0.0107, (2.31 \pm 1.29)\times 10^{-5}]$, where $s$ and $q$ denote the projected separation (scaled to the Einstein radius) and mass ratio between the planet and its host, respectively. We identify that the ambiguity between the inner and outer solutions stems from the inner-outer degeneracy, while the similarity between the intermediate solution and the others is due to an accidental degeneracy caused by incomplete anomaly coverage. Through Bayesian analysis utilizing the constraints derived from measured lensing observables and blending flux, our estimation indicates that the lens system comprises a very low-mass planet orbiting an early M-type star situated approximately (6.2 -- 6.5)~kpc from Earth in terms of median posterior values for the different solutions. The median mass of the planet host is in the range of (0.48 -- 0.51)~$M_\odot$, and that of the planet's mass spans a range of (2.6 -- 4.0)~$M_{\rm E}$, varying across different solutions. The detection of KMT-2023-BLG-1866Lb signifies the extension of the lensing surveys to very low-mass planets that have been difficult to be detected from earlier surveys. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.07514v1-abstract-full').style.display = 'none'; document.getElementById('2405.07514v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 pages, 8 figures, 4 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.15502">arXiv:2404.15502</a> <span> [<a href="https://arxiv.org/pdf/2404.15502">pdf</a>, <a href="https://arxiv.org/format/2404.15502">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1538-3873/ad70d7">10.1088/1538-3873/ad70d7 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A New Parameterization for Finding Solutions for Microlensing Exoplanet Light Curves </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hall%2C+K+E">Kylie E. Hall</a>, <a href="/search/astro-ph?searchtype=author&query=Yee%2C+J+C">Jennifer C. Yee</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+I">In-Gu Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+H">Hongjing Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+J">Jiyuan Zhang</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2404.15502v2-abstract-short" style="display: inline;"> The gravitational microlensing method of discovering exoplanets and multi-star systems can produce degenerate solutions, some of which require in-depth analysis to uncover. We propose a new parameter space that can be used to sample potential solutions more efficiently and is more robust at finding all degenerate solutions. We identified two new parameters, k and h, that can be sampled in place of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.15502v2-abstract-full').style.display = 'inline'; document.getElementById('2404.15502v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.15502v2-abstract-full" style="display: none;"> The gravitational microlensing method of discovering exoplanets and multi-star systems can produce degenerate solutions, some of which require in-depth analysis to uncover. We propose a new parameter space that can be used to sample potential solutions more efficiently and is more robust at finding all degenerate solutions. We identified two new parameters, k and h, that can be sampled in place of the mass ratios and separations of the systems under analysis to identify degenerate solutions. The parameter k is related to the size of the central caustic, $螖尉_c$, while h is related to the distance of a point along the k contour from log(s)=0, where s is the projected planet-host separation. In this work, we present the characteristics of these parameters and the tests we conducted to prove their efficacy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.15502v2-abstract-full').style.display = 'none'; document.getElementById('2404.15502v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, updated with version accepted to PASP</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> PASP 136 094401 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.05912">arXiv:2404.05912</a> <span> [<a href="https://arxiv.org/pdf/2404.05912">pdf</a>, <a href="https://arxiv.org/ps/2404.05912">ps</a>, <a href="https://arxiv.org/format/2404.05912">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> OGLE-2018-BLG-0971, MOA-2023-BLG-065, and OGLE-2023-BLG-0136: Microlensing events with prominent orbital effects </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Han%2C+C">Cheongho Han</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">Andrzej Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+I+A">Ian A. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+C">Chung-Uk Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">Andrew Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Albrow%2C+M+D">Michael D. Albrow</a>, <a href="/search/astro-ph?searchtype=author&query=Chung%2C+S">Sun-Ju Chung</a>, <a href="/search/astro-ph?searchtype=author&query=Hwang%2C+K">Kyu-Ha Hwang</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+Y+K">Youn Kil Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+H">Hyoun-Woo Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Ryu%2C+Y">Yoon-Hyun Ryu</a>, <a href="/search/astro-ph?searchtype=author&query=Shvartzvald%2C+Y">Yossi Shvartzvald</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+I">In-Gu Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Yee%2C+J+C">Jennifer C. Yee</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+H">Hongjing Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Zang%2C+W">Weicheng Zang</a>, <a href="/search/astro-ph?searchtype=author&query=Cha%2C+S">Sang-Mok Cha</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Doeon Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Dong-Jin Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+S">Seung-Lee Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+D">Dong-Joo Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+Y">Yongseok Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Park%2C+B">Byeong-Gon Park</a>, <a href="/search/astro-ph?searchtype=author&query=Pogge%2C+R+W">Richard W. Pogge</a>, <a href="/search/astro-ph?searchtype=author&query=Mr%C3%B3z%2C+P">Przemek Mr贸z</a> , et al. (38 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2404.05912v1-abstract-short" style="display: inline;"> We undertake a project to reexamine microlensing data gathered from high-cadence surveys. The aim of the project is to reinvestigate lensing events with light curves exhibiting intricate anomaly features associated with caustics, yet lacking prior proposed models to explain these features. Through detailed reanalyses considering higher-order effects, we identify that accounting for orbital motions… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.05912v1-abstract-full').style.display = 'inline'; document.getElementById('2404.05912v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.05912v1-abstract-full" style="display: none;"> We undertake a project to reexamine microlensing data gathered from high-cadence surveys. The aim of the project is to reinvestigate lensing events with light curves exhibiting intricate anomaly features associated with caustics, yet lacking prior proposed models to explain these features. Through detailed reanalyses considering higher-order effects, we identify that accounting for orbital motions of lenses is vital in accurately explaining the anomaly features observed in the light curves of the lensing events OGLE-2018-BLG-0971, MOA-2023-BLG-065, and OGLE-2023-BLG-0136. We estimate the masses and distances to the lenses by conducting Bayesian analyses using the lensing parameters of the newly found lensing solutions. From these analyses, we identify that the lenses of the events OGLE-2018-BLG-0971 and MOA-2023-BLG-065 are binaries composed of M dwarfs, while the lens of OGLE-2023-BLG-0136 is likely to be a binary composed of an early K-dwarf primary and a late M-dwarf companion. For all lensing events, the probability of the lens residing in the bulge is considerably higher than that of it being located in the disk. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.05912v1-abstract-full').style.display = 'none'; document.getElementById('2404.05912v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 13 figures, 6 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2402.08116">arXiv:2402.08116</a> <span> [<a href="https://arxiv.org/pdf/2402.08116">pdf</a>, <a href="https://arxiv.org/ps/2402.08116">ps</a>, <a href="https://arxiv.org/format/2402.08116">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> OGLE-2023-BLG-0836L: The sixth microlensing planet in a binary stellar system </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Han%2C+C">Cheongho Han</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">Andrzej Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+Y+K">Youn Kil Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">Andrew Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Doeon Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Albrow%2C+M+D">Michael D. Albrow</a>, <a href="/search/astro-ph?searchtype=author&query=Chung%2C+S">Sun-Ju Chung</a>, <a href="/search/astro-ph?searchtype=author&query=Hwang%2C+K">Kyu-Ha Hwang</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+C">Chung-Uk Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Ryu%2C+Y">Yoon-Hyun Ryu</a>, <a href="/search/astro-ph?searchtype=author&query=Shvartzvald%2C+Y">Yossi Shvartzvald</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+I">In-Gu Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Yee%2C+J+C">Jennifer C. Yee</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+H">Hongjing Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Zang%2C+W">Weicheng Zang</a>, <a href="/search/astro-ph?searchtype=author&query=Cha%2C+S">Sang-Mok Cha</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Dong-Jin Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+S">Seung-Lee Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+D">Dong-Joo Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+Y">Yongseok Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Park%2C+B">Byeong-Gon Park</a>, <a href="/search/astro-ph?searchtype=author&query=Pogge%2C+R+W">Richard W. Pogge</a>, <a href="/search/astro-ph?searchtype=author&query=Mr%C3%B3z%2C+P">Przemek Mr贸z</a>, <a href="/search/astro-ph?searchtype=author&query=Mr%C3%B3z%2C+M+J">Mateusz J. Mr贸z</a>, <a href="/search/astro-ph?searchtype=author&query=Szyma%C5%84ski%2C+M+K">Micha艂 K. Szyma艅ski</a> , et al. (10 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2402.08116v2-abstract-short" style="display: inline;"> Light curves of microlensing events occasionally deviate from the smooth and symmetric form of a single-lens single-source event. While most of these anomalous events can be accounted for by employing a binary-lens single-source (2L1S) or a single-lens binary-source (1L2S) framework, it is established that a small fraction of events remain unexplained by either of these interpretations. We carry o… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.08116v2-abstract-full').style.display = 'inline'; document.getElementById('2402.08116v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.08116v2-abstract-full" style="display: none;"> Light curves of microlensing events occasionally deviate from the smooth and symmetric form of a single-lens single-source event. While most of these anomalous events can be accounted for by employing a binary-lens single-source (2L1S) or a single-lens binary-source (1L2S) framework, it is established that a small fraction of events remain unexplained by either of these interpretations. We carry out a project in which data collected by high-cadence microlensing surveys were reinvestigated with the aim of uncovering the nature of anomalous lensing events with no proposed 2L1S or 1L2S models. From the project, we find that the anomaly appearing in the lensing event OGLE-2023-BLG-0836 cannot be explained by the usual interpretations and conduct a comprehensive analysis of the event. From thorough modeling of the light curve under sophisticated lens-system configurations, we have arrived at the conclusion that a triple-mass lens system is imperative to account for the anomaly features observed in the lensing light curve. From the Bayesian analysis using the measured observables of the event time scale and angular Einstein radius, we determine that the least massive component of the lens has a planetary mass of $4.36^{+2.35}_{-2.18}~M_{\rm J}$. This planet orbits within a stellar binary system composed of two stars with masses $0.71^{+0.38}_{-0.36}~M_\odot$ and $0.56^{+0.30}_{-0.28}~M_\odot$. This lensing event signifies the sixth occurrence of a planetary microlensing system in which a planet belongs to a stellar binary system. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.08116v2-abstract-full').style.display = 'none'; document.getElementById('2402.08116v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 12 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 12 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.11329">arXiv:2401.11329</a> <span> [<a href="https://arxiv.org/pdf/2401.11329">pdf</a>, <a href="https://arxiv.org/ps/2401.11329">ps</a>, <a href="https://arxiv.org/format/2401.11329">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> MOA-2022-BLG-563Lb, KMT-2023-BLG-0469Lb, and KMT-2023-BLG-0735Lb: Three sub-Jovian-mass microlensing planets </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Han%2C+C">Cheongho Han</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+Y+K">Youn Kil Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+I+A">Ian A. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">Andrew Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Albrow%2C+M+D">Michael D. Albrow</a>, <a href="/search/astro-ph?searchtype=author&query=Chung%2C+S">Sun-Ju Chung</a>, <a href="/search/astro-ph?searchtype=author&query=Hwang%2C+K">Kyu-Ha Hwang</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+C">Chung-Uk Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Ryu%2C+Y">Yoon-Hyun Ryu</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+I">In-Gu Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Shvartzvald%2C+Y">Yossi Shvartzvald</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+H">Hongjing Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Yee%2C+J+C">Jennifer C. Yee</a>, <a href="/search/astro-ph?searchtype=author&query=Zang%2C+W">Weicheng Zang</a>, <a href="/search/astro-ph?searchtype=author&query=Cha%2C+S">Sang-Mok Cha</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Doeon Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Dong-Jin Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+S">Seung-Lee Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+D">Dong-Joo Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+Y">Yongseok Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Park%2C+B">Byeong-Gon Park</a>, <a href="/search/astro-ph?searchtype=author&query=Pogge%2C+R+W">Richard W. Pogge</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+F">Fumio Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Barry%2C+R">Richard Barry</a>, <a href="/search/astro-ph?searchtype=author&query=Bennett%2C+D+P">David P. Bennett</a> , et al. (23 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2401.11329v1-abstract-short" style="display: inline;"> We analyze the anomalies appearing in the light curves of the three microlensing events MOA-2022-BLG-563, KMT-2023-BLG-0469, and KMT-2023-BLG-0735. The anomalies exhibit common short-term dip features that appear near the peak. From the detailed analyses of the light curves, we find that the anomalies were produced by planets accompanied by the lenses of the events. For all three events, the estim… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.11329v1-abstract-full').style.display = 'inline'; document.getElementById('2401.11329v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.11329v1-abstract-full" style="display: none;"> We analyze the anomalies appearing in the light curves of the three microlensing events MOA-2022-BLG-563, KMT-2023-BLG-0469, and KMT-2023-BLG-0735. The anomalies exhibit common short-term dip features that appear near the peak. From the detailed analyses of the light curves, we find that the anomalies were produced by planets accompanied by the lenses of the events. For all three events, the estimated mass ratios between the planet and host are on the order of $10^{-4}$: $q\sim 8 \times 10^{-4}$ for MOA-2022-BLG-563L, $q\sim 2.5\times 10^{-4}$ for KMT-2023-BLG-0469L, and $q\sim 1.9\times 10^{-4}$ for KMT-2023-BLG-0735L. The interpretations of the anomalies are subject to a common inner-outer degeneracy, which causes ambiguity when estimating the projected planet-host separation. We estimated the planet mass, $M_{\rm p}$, host mass, $M_{\rm h}$, and distance, $D_{\rm L}$, to the planetary system by conducting Bayesian analyses using the observables of the events. The estimated physical parameters of the planetary systems are $(M_{\rm h}/M_\odot, M_{\rm p}/M_{\rm J}, D_{\rm L}/{\rm kpc}) = (0.48^{+0.36}_{-0.30}, 0.40^{+0.31}_{-0.25}, 6.53^{+1.12}_{-1.57})$ for MOA-2022-BLG-563L, $(0.47^{+0.35}_{-0.26}, 0.124^{+0.092}_{-0.067}, 7.07^{+1.03}_{-1.19})$ for KMT-2023-BLG-0469L, and $(0.62^{+0.34}_{-0.35}, 0.125^{+0.068}_{-0.070}, 6.26^{+1.27}_{-1.67})$ for KMT-2023-BLG-0735L. According to the estimated parameters, all planets are cold planets with projected separations that are greater than the snow lines of the planetary systems, they have masses that lie between the masses of Uranus and Jupiter of the Solar System, and the hosts of the planets are main-sequence stars that are less massive than the Sun. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.11329v1-abstract-full').style.display = 'none'; document.getElementById('2401.11329v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 7 tables, 10 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.08904">arXiv:2401.08904</a> <span> [<a href="https://arxiv.org/pdf/2401.08904">pdf</a>, <a href="https://arxiv.org/ps/2401.08904">ps</a>, <a href="https://arxiv.org/format/2401.08904">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> KMT-2023-BLG-0416, KMT-2023-BLG-1454, KMT-2023-BLG-1642: Microlensing planets identified from partially covered signals </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Han%2C+C">Cheongho Han</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">Andrzej Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+C">Chung-Uk Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Zang%2C+W">Weicheng Zang</a>, <a href="/search/astro-ph?searchtype=author&query=Albrow%2C+M+D">Michael D. Albrow</a>, <a href="/search/astro-ph?searchtype=author&query=Chung%2C+S">Sun-Ju Chung</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">Andrew Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Hwang%2C+K">Kyu-Ha Hwang</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+Y+K">Youn Kil Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Ryu%2C+Y">Yoon-Hyun Ryu</a>, <a href="/search/astro-ph?searchtype=author&query=Shvartzvald%2C+Y">Yossi Shvartzvald</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+I">In-Gu Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Yee%2C+J+C">Jennifer C. Yee</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+H">Hongjing Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Cha%2C+S">Sang-Mok Cha</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Doeon Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Dong-Jin Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+S">Seung-Lee Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+D">Dong-Joo Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+Y">Yongseok Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Park%2C+B">Byeong-Gon Park</a>, <a href="/search/astro-ph?searchtype=author&query=Pogge%2C+R+W">Richard W. Pogge</a>, <a href="/search/astro-ph?searchtype=author&query=Mr%C3%B3z%2C+P">Przemek Mr贸z</a>, <a href="/search/astro-ph?searchtype=author&query=Szyma%C5%84ski%2C+M+K">Micha艂 K. Szyma艅ski</a>, <a href="/search/astro-ph?searchtype=author&query=Skowron%2C+J">Jan Skowron</a> , et al. (10 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2401.08904v1-abstract-short" style="display: inline;"> We investigate the 2023 season data from high-cadence microlensing surveys with the aim of detecting partially covered short-term signals and revealing their underlying astrophysical origins. Through this analysis, we ascertain that the signals observed in the lensing events KMT-2023-BLG-0416, KMT-2023-BLG-1454, and KMT-2023-BLG-1642 are of planetary origin. Considering the potential degeneracy ca… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.08904v1-abstract-full').style.display = 'inline'; document.getElementById('2401.08904v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.08904v1-abstract-full" style="display: none;"> We investigate the 2023 season data from high-cadence microlensing surveys with the aim of detecting partially covered short-term signals and revealing their underlying astrophysical origins. Through this analysis, we ascertain that the signals observed in the lensing events KMT-2023-BLG-0416, KMT-2023-BLG-1454, and KMT-2023-BLG-1642 are of planetary origin. Considering the potential degeneracy caused by the partial coverage of signals, we thoroughly investigate the lensing-parameter plane. In the case of KMT-2023-BLG-0416, we have identified two solution sets, one with a planet-to-host mass ratio of $q\sim 10^{-2}$ and the other with $q\sim 6\times 10^{-5}$, within each of which there are two local solutions emerging due to the inner-outer degeneracy. For KMT-2023-BLG-1454, we discern four local solutions featuring mass ratios of $q\sim (1.7-4.3)\times 10^{-3}$. When it comes to KMT-2023-BLG-1642, we identified two locals with $q\sim (6-10)\times 10^{-3}$ resulting from the inner-outer degeneracy. We estimate the physical lens parameters by conducting Bayesian analyses based on the event time scale and Einstein radius. For KMT-2023-BLG-0416L, the host mass is $\sim 0.6~M_\odot$, and the planet mass is $\sim (6.1-6.7)~M_{\rm J}$ according to one set of solutions and $\sim 0.04~M_{\rm J}$ according to the other set of solutions. KMT-2023-BLG-1454Lb has a mass roughly half that of Jupiter, while KMT-2023-BLG-1646Lb has a mass in the range of between 1.1 to 1.3 times that of Jupiter, classifying them both as giant planets orbiting mid M-dwarf host stars with masses ranging from 0.13 to 0.17 solar masses. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.08904v1-abstract-full').style.display = 'none'; document.getElementById('2401.08904v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 16 figures, 6 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.04256">arXiv:2401.04256</a> <span> [<a href="https://arxiv.org/pdf/2401.04256">pdf</a>, <a href="https://arxiv.org/ps/2401.04256">ps</a>, <a href="https://arxiv.org/format/2401.04256">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> Systematic KMTNet Planetary Anomaly Search. XI. Complete Sample of 2016 Sub-Prime Field Planets </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Shin%2C+I">In-Gu Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Yee%2C+J+C">Jennifer C. Yee</a>, <a href="/search/astro-ph?searchtype=author&query=Zang%2C+W">Weicheng Zang</a>, <a href="/search/astro-ph?searchtype=author&query=Han%2C+C">Cheongho Han</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+H">Hongjing Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">Andrew Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+C">Chung-Uk Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">Andrzej Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Sumi%2C+T">Takahiro Sumi</a>, <a href="/search/astro-ph?searchtype=author&query=Albrow%2C+M+D">Michael D. Albrow</a>, <a href="/search/astro-ph?searchtype=author&query=Chung%2C+S">Sun-Ju Chung</a>, <a href="/search/astro-ph?searchtype=author&query=Hwang%2C+K">Kyu-Ha Hwang</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+Y+K">Youn Kil Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Ryu%2C+Y">Yoon-Hyun Ryu</a>, <a href="/search/astro-ph?searchtype=author&query=Shvartzvald%2C+Y">Yossi Shvartzvald</a>, <a href="/search/astro-ph?searchtype=author&query=Cha%2C+S">Sang-Mok Cha</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Dong-Jin Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+H">Hyoun-Woo Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+S">Seung-Lee Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+D">Dong-Joo Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+Y">Yongseok Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Park%2C+B">Byeong-Gon Park</a>, <a href="/search/astro-ph?searchtype=author&query=Pogge%2C+R+W">Richard W. Pogge</a>, <a href="/search/astro-ph?searchtype=author&query=Mr%C3%B3z%2C+P">Przemek Mr贸z</a>, <a href="/search/astro-ph?searchtype=author&query=Szyma%C5%84ski%2C+M+K">Micha艂 K. Szyma艅ski</a> , et al. (41 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2401.04256v1-abstract-short" style="display: inline;"> Following Shin et al. (2023b), which is a part of the Systematic KMTNet Planetary Anomaly Search series (i.e., a search for planets in the 2016 KMTNet prime fields), we conduct a systematic search of the 2016 KMTNet sub-prime fields using a semi-machine-based algorithm to identify hidden anomalous events missed by the conventional by-eye search. We find four new planets and seven planet candidates… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.04256v1-abstract-full').style.display = 'inline'; document.getElementById('2401.04256v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.04256v1-abstract-full" style="display: none;"> Following Shin et al. (2023b), which is a part of the Systematic KMTNet Planetary Anomaly Search series (i.e., a search for planets in the 2016 KMTNet prime fields), we conduct a systematic search of the 2016 KMTNet sub-prime fields using a semi-machine-based algorithm to identify hidden anomalous events missed by the conventional by-eye search. We find four new planets and seven planet candidates that were buried in the KMTNet archive. The new planets are OGLE-2016-BLG-1598Lb, OGLE-2016-BLG-1800Lb, MOA-2016-BLG-526Lb, and KMT-2016-BLG-2321Lb, which show typical properties of microlensing planets, i.e., giant planets orbit M dwarf host stars beyond their snow lines. For the planet candidates, we find planet/binary or 2L1S/1L2S degeneracies, which are an obstacle to firmly claiming planet detections. By combining the results of Shin et al. (2023b) and this work, we find a total of nine hidden planets, which is about half the number of planets discovered by eye in 2016. With this work, we have met the goal of the systematic search series for 2016, which is to build a complete microlensing planet sample. We also show that our systematic searches significantly contribute to completing the planet sample, especially for planet/host mass ratios smaller than $10^{-3}$, which were incomplete in previous by-eye searches of the KMTNet archive. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.04256v1-abstract-full').style.display = 'none'; document.getElementById('2401.04256v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">63 pages, 16 Tables, 19 Figures, Submitted in the AAS journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.08635">arXiv:2312.08635</a> <span> [<a href="https://arxiv.org/pdf/2312.08635">pdf</a>, <a href="https://arxiv.org/format/2312.08635">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> OGLE-2017-BLG-0448Lb: A Low Mass-Ratio Wide-Orbit Microlensing Planet? </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zhai%2C+R">Ruocheng Zhai</a>, <a href="/search/astro-ph?searchtype=author&query=Poleski%2C+R">Rados艂aw Poleski</a>, <a href="/search/astro-ph?searchtype=author&query=Zang%2C+W">Weicheng Zang</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+Y+K">Youn Kil Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">Andrzej Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Kuang%2C+R">Renkun Kuang</a>, <a href="/search/astro-ph?searchtype=author&query=Albrow%2C+M+D">Michael D. Albrow</a>, <a href="/search/astro-ph?searchtype=author&query=Chung%2C+S">Sun-Ju Chung</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">Andrew Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Han%2C+C">Cheongho Han</a>, <a href="/search/astro-ph?searchtype=author&query=Hwang%2C+K">Kyu-Ha Hwang</a>, <a href="/search/astro-ph?searchtype=author&query=Ryu%2C+Y">Yoon-Hyun Ryu</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+I">In-Gu Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Shvartzvald%2C+Y">Yossi Shvartzvald</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+H">Hongjing Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Yee%2C+J+C">Jennifer C. Yee</a>, <a href="/search/astro-ph?searchtype=author&query=Cha%2C+S">Sang-Mok Cha</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Dong-Jin Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+H">Hyoun-Woo Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+S">Seung-Lee Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+C">Chung-Uk Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+D">Dong-Joo Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+Y">Yongseok Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Park%2C+B">Byeong-Gon Park</a>, <a href="/search/astro-ph?searchtype=author&query=Pogge%2C+R+W">Richard W. Pogge</a> , et al. (16 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2312.08635v1-abstract-short" style="display: inline;"> The gravitational microlensing technique is most sensitive to planets in a Jupiter-like orbit and has detected more than 200 planets. However, only a few wide-orbit ($s > 2$) microlensing planets have been discovered, where $s$ is the planet-to-host separation normalized to the angular Einstein ring radius, $胃_{\rm E}$. Here we present the discovery and analysis of a strong candidate wide-orbit mi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.08635v1-abstract-full').style.display = 'inline'; document.getElementById('2312.08635v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.08635v1-abstract-full" style="display: none;"> The gravitational microlensing technique is most sensitive to planets in a Jupiter-like orbit and has detected more than 200 planets. However, only a few wide-orbit ($s > 2$) microlensing planets have been discovered, where $s$ is the planet-to-host separation normalized to the angular Einstein ring radius, $胃_{\rm E}$. Here we present the discovery and analysis of a strong candidate wide-orbit microlensing planet in the event, OGLE-2017-BLG-0448. The whole light curve exhibits long-term residuals to the static binary-lens single-source model, so we investigate the residuals by adding the microlensing parallax, microlensing xallarap, an additional lens, or an additional source. For the first time, we observe a complex degeneracy between all four effects. The wide-orbit models with $s \sim 2.5$ and a planet-to-host mass-ratio of $q \sim 10^{-4}$ are significantly preferred, but we cannot rule out the close models with $s \sim 0.35$ and $q \sim 10^{-3}$. A Bayesian analysis based on a Galactic model indicates that, despite the complicated degeneracy, the surviving wide-orbit models all contain a super-Earth-mass to Neptune-mass planet at a projected planet-host separation of $\sim 6$ au and the surviving close-orbit models all consist of a Jovian-mass planet at $\sim 1$ au. The host star is probably an M or K dwarf. We discuss the implications of this dimension-degeneracy disaster on microlensing light-curve analysis and its potential impact on statistical studies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.08635v1-abstract-full').style.display = 'none'; document.getElementById('2312.08635v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">submitted to AJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.01278">arXiv:2312.01278</a> <span> [<a href="https://arxiv.org/pdf/2312.01278">pdf</a>, <a href="https://arxiv.org/ps/2312.01278">ps</a>, <a href="https://arxiv.org/format/2312.01278">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> </div> <p class="title is-5 mathjax"> OGLE-2019-BLG-1180Lb: Discovery of a Wide-orbit Jupiter-mass Planet around a Late-type Star </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Chung%2C+S">Sun-Ju Chung</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">Andrzej Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Yee%2C+J+C">Jennifer C. Yee</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">Andrew Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Albrow%2C+M+D">Michael D. Albrow</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+Y+K">Youn Kil Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Hwang%2C+K">Kyu-Ha Hwang</a>, <a href="/search/astro-ph?searchtype=author&query=Han%2C+C">Cheongho Han</a>, <a href="/search/astro-ph?searchtype=author&query=Ryu%2C+Y">Yoon-Hyun Ryu</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+I">In-Gu Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Shvartzvald%2C+Y">Yossi Shvartzvald</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+H">Hongjing Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Zang%2C+W">Weicheng Zang</a>, <a href="/search/astro-ph?searchtype=author&query=Cha%2C+S">Sang-Mok Cha</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Dong-Jin Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+S">Seung-Lee Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+C">Chung-Uk Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+D">Dong-Joo Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+Y">Yongseok Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Park%2C+B">Byeong-Gon Park</a>, <a href="/search/astro-ph?searchtype=author&query=Pogge%2C+R+W">Richard W. Pogge</a>, <a href="/search/astro-ph?searchtype=author&query=Poleski%2C+R">Radek Poleski</a>, <a href="/search/astro-ph?searchtype=author&query=Mr%C3%B3z%2C+P">Przemek Mr贸z</a>, <a href="/search/astro-ph?searchtype=author&query=Skowron%2C+J">Jan Skowron</a>, <a href="/search/astro-ph?searchtype=author&query=Szyma%C5%84ski%2C+M+K">Micha艂 K. Szyma艅ski</a> , et al. (8 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2312.01278v1-abstract-short" style="display: inline;"> We report on the discovery and analysis of the planetary microlensing event OGLE-2019-BLG-1180 with a planet-to-star mass ratio $q \sim 0.003$. The event OGLE-2019-BLG-1180 has unambiguous cusp-passing and caustic-crossing anomalies, which were caused by a wide planetary caustic with $s \simeq 2$, where $s$ is the star-planet separation in units of the angular Einstein radius $胃_{E}$. Thanks to we… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.01278v1-abstract-full').style.display = 'inline'; document.getElementById('2312.01278v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.01278v1-abstract-full" style="display: none;"> We report on the discovery and analysis of the planetary microlensing event OGLE-2019-BLG-1180 with a planet-to-star mass ratio $q \sim 0.003$. The event OGLE-2019-BLG-1180 has unambiguous cusp-passing and caustic-crossing anomalies, which were caused by a wide planetary caustic with $s \simeq 2$, where $s$ is the star-planet separation in units of the angular Einstein radius $胃_{E}$. Thanks to well-covered anomalies by the Korea Micorolensing Telescope Network (KMTNet), we measure both the angular Einstein radius and the microlens parallax in spite of a relatively short event timescale of $t_{E} = 28$ days. However, because of a weak constraint on the parallax, we conduct a Bayesian analysis to estimate the physical lens parameters. We find that the lens system is a super-Jupiter-mass planet of $M_{p} = 1.75^{+0.54}_{-0.51} M_{J}$ orbiting a late-type star of $M_{h}=0.55^{+0.27}_{-0.26} M_\odot$ at a distance of $D_{L} = 6.1^{+0.9}_{-1.3}$ kpc. The projected star-planet separation is $a_{\perp} = 5.19^{+0.90}_{-1.23}$ au, which means that the planet orbits at about four times the snow line of the host star. Considering the relative lens-source proper motion of $渭_{rel} = 6$ mas/yr, the lens will be separated from the source by 60 mas in 2029. At that time one can measure the lens flux from adaptive optics imaging of Kec or a next-generation 30 m class telescope. OGLE-2019-BLG-1180Lb represents a growing population of wide-orbit planets detected by KMTNet, so we also present a general investigation into prospects for further expanding the sample of such planets. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.01278v1-abstract-full').style.display = 'none'; document.getElementById('2312.01278v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 12 figures, 5 tables, published in AJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.13097">arXiv:2311.13097</a> <span> [<a href="https://arxiv.org/pdf/2311.13097">pdf</a>, <a href="https://arxiv.org/format/2311.13097">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> KMT-2023-BLG-1431Lb: A New $q < 10^{-4}$ Microlensing Planet from a Subtle Signature </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bell%2C+A">Aislyn Bell</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+J">Jiyuan Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+Y+K">Youn Kil Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Yee%2C+J+C">Jennifer C. Yee</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+H">Hongjing Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Sumi%2C+T">Takahiro Sumi</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">Andrzej Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Albrow%2C+M+D">Michael D. Albrow</a>, <a href="/search/astro-ph?searchtype=author&query=Chung%2C+S">Sun-Ju Chung</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">Andrew Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Han%2C+C">Cheongho Han</a>, <a href="/search/astro-ph?searchtype=author&query=Hwang%2C+K">Kyu-Ha Hwang</a>, <a href="/search/astro-ph?searchtype=author&query=Ryu%2C+Y">Yoon-Hyun Ryu</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+I">In-Gu Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Shvartzvald%2C+Y">Yossi Shvartzvald</a>, <a href="/search/astro-ph?searchtype=author&query=Zang%2C+W">Weicheng Zang</a>, <a href="/search/astro-ph?searchtype=author&query=Cha%2C+S">Sang-Mok Cha</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Dong-Jin Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+S">Seung-Lee Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+C">Chung-Uk Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+D">Dong-Joo Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+Y">Yongseok Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Park%2C+B">Byeong-Gon Park</a>, <a href="/search/astro-ph?searchtype=author&query=Pogge%2C+R+W">Richard W. Pogge</a>, <a href="/search/astro-ph?searchtype=author&query=Tang%2C+Y">Yunyi Tang</a> , et al. (48 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2311.13097v1-abstract-short" style="display: inline;"> The current studies of microlensing planets are limited by small number statistics. Follow-up observations of high-magnification microlensing events can efficiently form a statistical planetary sample. Since 2020, the Korea Microlensing Telescope Network (KMTNet) and the Las Cumbres Observatory (LCO) global network have been conducting a follow-up program for high-magnification KMTNet events. Here… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.13097v1-abstract-full').style.display = 'inline'; document.getElementById('2311.13097v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.13097v1-abstract-full" style="display: none;"> The current studies of microlensing planets are limited by small number statistics. Follow-up observations of high-magnification microlensing events can efficiently form a statistical planetary sample. Since 2020, the Korea Microlensing Telescope Network (KMTNet) and the Las Cumbres Observatory (LCO) global network have been conducting a follow-up program for high-magnification KMTNet events. Here, we report the detection and analysis of a microlensing planetary event, KMT-2023-BLG-1431, for which the subtle (0.05 magnitude) and short-lived (5 hours) planetary signature was characterized by the follow-up from KMTNet and LCO. A binary-lens single-source (2L1S) analysis reveals a planet/host mass ratio of $q = (0.72 \pm 0.07) \times 10^{-4}$, and the single-lens binary-source (1L2S) model is excluded by $螖蠂^2 = 80$. A Bayesian analysis using a Galactic model yields estimates of the host star mass of $M_{\rm host} = 0.57^{+0.33}_{-0.29}~M_\odot$, the planetary mass of $M_{\rm planet} = 13.5_{-6.8}^{+8.1}~M_{\oplus}$, and the lens distance of $D_{\rm L} = 6.9_{-1.7}^{+0.8}$ kpc. The projected planet-host separation of $a_\perp = 2.3_{-0.5}^{+0.5}$ au or $a_\perp = 3.2_{-0.8}^{+0.7}$, subject to the close/wide degeneracy. We also find that without the follow-up data, the survey-only data cannot break the degeneracy of central/resonant caustics and the degeneracy of 2L1S/1L2S models, showing the importance of follow-up observations for current microlensing surveys. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.13097v1-abstract-full').style.display = 'none'; document.getElementById('2311.13097v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">PASP submitted. arXiv admin note: text overlap with arXiv:2301.06779</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.04876">arXiv:2311.04876</a> <span> [<a href="https://arxiv.org/pdf/2311.04876">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> Systematic Reanalysis of KMTNet microlensing events, Paper I: Updates of the Photometry Pipeline and a New Planet Candidate </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Yang%2C+H">Hongjing Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Yee%2C+J+C">Jennifer C. Yee</a>, <a href="/search/astro-ph?searchtype=author&query=Hwang%2C+K">Kyu-Ha Hwang</a>, <a href="/search/astro-ph?searchtype=author&query=Qian%2C+Q">Qiyue Qian</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+I+A">Ian A. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">Andrew Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Hu%2C+Z">Zhecheng Hu</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+J">Jiyuan Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Mao%2C+S">Shude Mao</a>, <a href="/search/astro-ph?searchtype=author&query=Zhu%2C+W">Wei Zhu</a>, <a href="/search/astro-ph?searchtype=author&query=Albrow%2C+M+D">Michael D. Albrow</a>, <a href="/search/astro-ph?searchtype=author&query=Chung%2C+S">Sun-Ju Chung</a>, <a href="/search/astro-ph?searchtype=author&query=Han%2C+C">Cheongho Han</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+Y+K">Youn Kil Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Ryu%2C+Y">Yoon-Hyun Ryu</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+I">In-Gu Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Shvartzvald%2C+Y">Yossi Shvartzvald</a>, <a href="/search/astro-ph?searchtype=author&query=Cha%2C+S">Sang-Mok Cha</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Dong-Jin Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+H">Hyoun-Woo Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+S">Seung-Lee Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+C">Chung-Uk Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+D">Dong-Joo Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+Y">Yongseok Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Park%2C+B">Byeong-Gon Park</a> , et al. (30 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2311.04876v1-abstract-short" style="display: inline;"> In this work, we update and develop algorithms for KMTNet tender-love care (TLC) photometry in order to create an new, mostly automated, TLC pipeline. We then start a project to systematically apply the new TLC pipeline to the historic KMTNet microlensing events, and search for buried planetary signals. We report the discovery of such a planet candidate in the microlensing event MOA-2019-BLG-421/K… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.04876v1-abstract-full').style.display = 'inline'; document.getElementById('2311.04876v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.04876v1-abstract-full" style="display: none;"> In this work, we update and develop algorithms for KMTNet tender-love care (TLC) photometry in order to create an new, mostly automated, TLC pipeline. We then start a project to systematically apply the new TLC pipeline to the historic KMTNet microlensing events, and search for buried planetary signals. We report the discovery of such a planet candidate in the microlensing event MOA-2019-BLG-421/KMT-2019-BLG-2991. The anomalous signal can be explained by either a planet around the lens star or the orbital motion of the source star. For the planetary interpretation, despite many degenerate solutions, the planet is most likely to be a Jovian planet orbiting an M or K dwarf, which is a typical microlensing planet. The discovery proves that the project can indeed increase the sensitivity of historic events and find previously undiscovered signals. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.04876v1-abstract-full').style.display = 'none'; document.getElementById('2311.04876v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 13 figures, 7 tables. Submitted to MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.01280">arXiv:2309.01280</a> <span> [<a href="https://arxiv.org/pdf/2309.01280">pdf</a>, <a href="https://arxiv.org/ps/2309.01280">ps</a>, <a href="https://arxiv.org/format/2309.01280">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> KMT-2021-BLG-1547Lb: Giant microlensing planet detected through a signal deformed by source binarity </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Han%2C+C">Cheongho Han</a>, <a href="/search/astro-ph?searchtype=author&query=Zang%2C+W">Weicheng Zang</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+Y+K">Youn Kil Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+I+A">Ian A. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Chung%2C+S">Sun-Ju Chung</a>, <a href="/search/astro-ph?searchtype=author&query=Albrow%2C+M+D">Michael D. Albrow</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">Andrew Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Hwang%2C+K">Kyu-Ha Hwang</a>, <a href="/search/astro-ph?searchtype=author&query=Ryu%2C+Y">Yoon-Hyun Ryu</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+I">In-Gu Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Shvartzvald%2C+Y">Yossi Shvartzvald</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+H">Hongjing Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Yee%2C+J+C">Jennifer C. Yee</a>, <a href="/search/astro-ph?searchtype=author&query=Cha%2C+S">Sang-Mok Cha</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Doeon Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Dong-Jin Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+S">Seung-Lee Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+C">Chung-Uk Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+D">Dong-Joo Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+Y">Yongseok Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Park%2C+B">Byeong-Gon Park</a>, <a href="/search/astro-ph?searchtype=author&query=Pogge%2C+R+W">Richard W. Pogge</a>, <a href="/search/astro-ph?searchtype=author&query=Monard%2C+L+A+G">L. A. G. Monard</a>, <a href="/search/astro-ph?searchtype=author&query=Qian%2C+Q">Qiyue Qian</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+Z">Zhuokai Liu</a> , et al. (30 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2309.01280v1-abstract-short" style="display: inline;"> We investigate the previous microlensing data collected by the KMTNet survey in search of anomalous events for which no precise interpretations of the anomalies have been suggested. From this investigation, we find that the anomaly in the lensing light curve of the event KMT-2021-BLG-1547 is approximately described by a binary-lens (2L1S) model with a lens possessing a giant planet, but the model… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.01280v1-abstract-full').style.display = 'inline'; document.getElementById('2309.01280v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.01280v1-abstract-full" style="display: none;"> We investigate the previous microlensing data collected by the KMTNet survey in search of anomalous events for which no precise interpretations of the anomalies have been suggested. From this investigation, we find that the anomaly in the lensing light curve of the event KMT-2021-BLG-1547 is approximately described by a binary-lens (2L1S) model with a lens possessing a giant planet, but the model leaves unexplained residuals. We investigate the origin of the residuals by testing more sophisticated models that include either an extra lens component (3L1S model) or an extra source star (2L2S model) to the 2L1S configuration of the lens system. From these analyses, we find that the residuals from the 2L1S model originate from the existence of a faint companion to the source. The 2L2S solution substantially reduces the residuals and improves the model fit by $螖蠂^2=67.1$ with respect to the 2L1S solution. The 3L1S solution also improves the fit, but its fit is worse than that of the 2L2S solution by $螖蠂^2=24.7$. According to the 2L2S solution, the lens of the event is a planetary system with planet and host masses $(M_{\rm p}/M_{\rm J}, M_{\rm h}/M_\odot)=\left( 1.47^{+0.64}_{-0.77}, 0.72^{+0.32}_{-0.38}\right)$ lying at a distance $\D_{\rm L} =5.07^{+0.98}_{-1.50}$~kpc, and the source is a binary composed of a subgiant primary of a late G or an early K spectral type and a main-sequence companion of a K spectral type. The event demonstrates the need of sophisticated modeling for unexplained anomalies for the construction of a complete microlensing planet sample. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.01280v1-abstract-full').style.display = 'none'; document.getElementById('2309.01280v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 pages, 4 tables, 7 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.14274">arXiv:2307.14274</a> <span> [<a href="https://arxiv.org/pdf/2307.14274">pdf</a>, <a href="https://arxiv.org/format/2307.14274">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> OGLE-2019-BLG-0825: Constraints on the Source System and Effect on Binary-lens Parameters arising from a Five Day Xallarap Effect in a Candidate Planetary Microlensing Event </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Satoh%2C+Y+K">Yuki K. Satoh</a>, <a href="/search/astro-ph?searchtype=author&query=Koshimoto%2C+N">Naoki Koshimoto</a>, <a href="/search/astro-ph?searchtype=author&query=Bennett%2C+D+P">David P. Bennett</a>, <a href="/search/astro-ph?searchtype=author&query=Sumi%2C+T">Takahiro Sumi</a>, <a href="/search/astro-ph?searchtype=author&query=Rattenbury%2C+N+J">Nicholas J. Rattenbury</a>, <a href="/search/astro-ph?searchtype=author&query=Suzuki%2C+D">Daisuke Suzuki</a>, <a href="/search/astro-ph?searchtype=author&query=Miyazaki%2C+S">Shota Miyazaki</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+I+A">Ian A. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">Andrzej Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">Andrew Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Bozza%2C+V">Valerio Bozza</a>, <a href="/search/astro-ph?searchtype=author&query=Dominik%2C+M">Martin Dominik</a>, <a href="/search/astro-ph?searchtype=author&query=Hirao%2C+Y">Yuki Hirao</a>, <a href="/search/astro-ph?searchtype=author&query=Kondo%2C+I">Iona Kondo</a>, <a href="/search/astro-ph?searchtype=author&query=Kirikawa%2C+R">Rintaro Kirikawa</a>, <a href="/search/astro-ph?searchtype=author&query=Hamada%2C+R">Ryusei Hamada</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+F">Fumio Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Barry%2C+R">Richard Barry</a>, <a href="/search/astro-ph?searchtype=author&query=Bhattacharya%2C+A">Aparna Bhattacharya</a>, <a href="/search/astro-ph?searchtype=author&query=Fujii%2C+H">Hirosane Fujii</a>, <a href="/search/astro-ph?searchtype=author&query=Fukui%2C+A">Akihiko Fukui</a>, <a href="/search/astro-ph?searchtype=author&query=Fujita%2C+K">Katsuki Fujita</a>, <a href="/search/astro-ph?searchtype=author&query=Ikeno%2C+T">Tomoya Ikeno</a>, <a href="/search/astro-ph?searchtype=author&query=Silva%2C+S+I">Stela Ishitani Silva</a>, <a href="/search/astro-ph?searchtype=author&query=Itow%2C+Y">Yoshitaka Itow</a> , et al. (64 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2307.14274v1-abstract-short" style="display: inline;"> We present an analysis of microlensing event OGLE-2019-BLG-0825. This event was identified as a planetary candidate by preliminary modeling. We find that significant residuals from the best-fit static binary-lens model exist and a xallarap effect can fit the residuals very well and significantly improves $蠂^2$ values. On the other hand, by including the xallarap effect in our models, we find that… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.14274v1-abstract-full').style.display = 'inline'; document.getElementById('2307.14274v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.14274v1-abstract-full" style="display: none;"> We present an analysis of microlensing event OGLE-2019-BLG-0825. This event was identified as a planetary candidate by preliminary modeling. We find that significant residuals from the best-fit static binary-lens model exist and a xallarap effect can fit the residuals very well and significantly improves $蠂^2$ values. On the other hand, by including the xallarap effect in our models, we find that binary-lens parameters like mass-ratio, $q$, and separation, $s$, cannot be constrained well. However, we also find that the parameters for the source system like the orbital period and semi major axis are consistent between all the models we analyzed. We therefore constrain the properties of the source system better than the properties of the lens system. The source system comprises a G-type main-sequence star orbited by a brown dwarf with a period of $P\sim5$ days. This analysis is the first to demonstrate that the xallarap effect does affect binary-lens parameters in planetary events. It would not be common for the presence or absence of the xallarap effect to affect lens parameters in events with long orbital periods of the source system or events with transits to caustics, but in other cases, such as this event, the xallarap effect can affect binary-lens parameters. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.14274v1-abstract-full').style.display = 'none'; document.getElementById('2307.14274v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 7 figures, 6 tables. Accepted by AJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.13359">arXiv:2307.13359</a> <span> [<a href="https://arxiv.org/pdf/2307.13359">pdf</a>, <a href="https://arxiv.org/ps/2307.13359">ps</a>, <a href="https://arxiv.org/format/2307.13359">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Systematic KMTNet Planetary Anomaly Search. X. Complete Sample of 2017 Prime-Field Planets </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ryu%2C+Y">Yoon-Hyun Ryu</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">Andrzej Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Yee%2C+J+C">Jennifer C. Yee</a>, <a href="/search/astro-ph?searchtype=author&query=Zang%2C+W">Weicheng Zang</a>, <a href="/search/astro-ph?searchtype=author&query=Shvartzvald%2C+Y">Yossi Shvartzvald</a>, <a href="/search/astro-ph?searchtype=author&query=Han%2C+C">Cheongho Han</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">Andrew Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Albrow%2C+M+D">Michael D. Albrow</a>, <a href="/search/astro-ph?searchtype=author&query=Chung%2C+S">Sun-Ju Chung</a>, <a href="/search/astro-ph?searchtype=author&query=Hwang%2C+K">Kyu-Ha Hwang</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+Y+K">Youn Kil Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+I">In-Gu Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+H">Hongjing Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Cha%2C+S">Sang-Mok Cha</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Dong-Jin Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+S">Seung-Lee Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+C">Chung-Uk Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+D">Dong-Joo Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+Y">Yongseok Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Park%2C+B">Byeong-Gon Park</a>, <a href="/search/astro-ph?searchtype=author&query=Pogge%2C+R+W">Richard W. Pogge</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+H">Hanyue Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Mr%C3%B3z%2C+P">Przemek Mr贸z</a>, <a href="/search/astro-ph?searchtype=author&query=Szyma%C5%84ski%2C+M+K">Micha艂 K. Szyma艅ski</a>, <a href="/search/astro-ph?searchtype=author&query=Skowron%2C+J">Jan Skowron</a> , et al. (16 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2307.13359v2-abstract-short" style="display: inline;"> We complete the analysis of planetary candidates found by the KMT AnomalyFinder for the 2017 prime fields that cover $\sim 13\,{\rm deg}^2$. We report 3 unambiguous planets: OGLE-2017-BLG-0640, OGLE-2017-BLG-1275, and OGLE-2017-BLG-1237. The first two of these were not previously identified, while the last was not previously published due to technical complications induced by a nearby variable. We… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.13359v2-abstract-full').style.display = 'inline'; document.getElementById('2307.13359v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.13359v2-abstract-full" style="display: none;"> We complete the analysis of planetary candidates found by the KMT AnomalyFinder for the 2017 prime fields that cover $\sim 13\,{\rm deg}^2$. We report 3 unambiguous planets: OGLE-2017-BLG-0640, OGLE-2017-BLG-1275, and OGLE-2017-BLG-1237. The first two of these were not previously identified, while the last was not previously published due to technical complications induced by a nearby variable. We further report that a fourth anomalous event, the previously recognized OGLE-2017-BLG-1777, is very likely to be planetary, although its light curve requires unusually complex modeling because the lens and source both have orbiting companions. One of the 3 unambiguous planets, OGLE-2017-BLG-1275 is the first AnomalyFinder discovery that has a {\it Spitzer} microlens parallax measurement, $蟺_E \sim 0.045\pm0.015$, implying that this planetary system almost certainly lies in the Galactic bulge. In the order listed, the four planetary events have planet-host mass ratios $q$, and normalized projected separations $s$, of $(\log q,s)$ = $(-2.31,0.61)$, $(-2.06,0.63/1.09)$, $(-2.10,1.04)$, and $(-2.86,0.72)$. Combined with previously published events, the 2017 AnomalyFinder prime fields contain 11 unambiguous planets with well-measured $q$ and one very likely candidate, of which 3 are AnomalyFinder discoveries. In addition to these 12, there are three other unambiguous planets with large uncertainties in $q$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.13359v2-abstract-full').style.display = 'none'; document.getElementById('2307.13359v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">67 pages, 13 figures, 16 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.04921">arXiv:2307.04921</a> <span> [<a href="https://arxiv.org/pdf/2307.04921">pdf</a>, <a href="https://arxiv.org/ps/2307.04921">ps</a>, <a href="https://arxiv.org/format/2307.04921">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> </div> <p class="title is-5 mathjax"> Brown dwarf companions in binaries detected from the 2021 season high-cadence microlensing surveys </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Han%2C+C">Cheongho Han</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+Y+K">Youn Kil Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+I+A">Ian A. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Chung%2C+S">Sun-Ju Chung</a>, <a href="/search/astro-ph?searchtype=author&query=Albrow%2C+M+D">Michael D. Albrow</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">Andrew Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Hwang%2C+K">Kyu-Ha Hwang</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+C">Chung-Uk Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Ryu%2C+Y">Yoon-Hyun Ryu</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+I">In-Gu Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Shvartzvald%2C+Y">Yossi Shvartzvald</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+H">Hongjing Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Yee%2C+J+C">Jennifer C. Yee</a>, <a href="/search/astro-ph?searchtype=author&query=Zang%2C+W">Weicheng Zang</a>, <a href="/search/astro-ph?searchtype=author&query=Cha%2C+S">Sang-Mok Cha</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Doeon Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Dong-Jin Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+S">Seung-Lee Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+D">Dong-Joo Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+Y">Yongseok Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Park%2C+B">Byeong-Gon Park</a>, <a href="/search/astro-ph?searchtype=author&query=Pogge%2C+R+W">Richard W. Pogge</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+F">Fumio Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Barry%2C+R">Richard Barry</a>, <a href="/search/astro-ph?searchtype=author&query=Bennett%2C+D+P">David P. Bennett</a> , et al. (23 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2307.04921v1-abstract-short" style="display: inline;"> As a part of the project aiming to build a homogeneous sample of binary-lens (2L1S) events containing brown-dwarf (BD) companions, we investigate the 2021 season microlensing data collected by the Korea Microlensing Telescope Network (KMTNet) survey. For this purpose, we first identify 2L1S events by conducting systematic analyses of anomalous lensing events. We then select candidate BD-companion… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.04921v1-abstract-full').style.display = 'inline'; document.getElementById('2307.04921v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.04921v1-abstract-full" style="display: none;"> As a part of the project aiming to build a homogeneous sample of binary-lens (2L1S) events containing brown-dwarf (BD) companions, we investigate the 2021 season microlensing data collected by the Korea Microlensing Telescope Network (KMTNet) survey. For this purpose, we first identify 2L1S events by conducting systematic analyses of anomalous lensing events. We then select candidate BD-companion events by applying the criterion that the mass ratio between the lens components is less than $q_{\rm th}\sim 0.1$. From this procedure, we find four binary-lens events including KMT-2021-BLG-0588, KMT-2021-BLG-1110, KMT-2021-BLG-1643, and KMT-2021-BLG-1770, for which the estimated mass ratios are $q\sim 0.10$, 0.07, 0.08, and 0.15, respectively. The event KMT-2021-BLG-1770 is selected as a candidate despite the fact that the mass ratio is slightly greater than $q_{\rm th}$ because the lens mass expected from the measured short time scale of the event, $t_{\rm E}\sim 7.6$~days, is small. From the Bayesian analyses, we estimate that the primary and companion masses are $(M_1/M_\odot, M_2/M_\odot)= (0.54^{+0.31}_{-0.24}, 0.053^{+0.031}_{-0.023})$ for KMT-2021-BLG-0588L, $(0.74^{+0.27}_{-0.35}, 0.055^{+0.020}_{-0.026})$ for KMT-2021-BLG-1110L, $(0.73^{+0.24}_{-0.17}, 0.061^{+0.020}_{-0.014})$ for KMT-2021-BLG-1643L, and $(0.13^{+0.18}_{-0.07}, 0.020^{+0.028}_{-0.011})$ for KMT-2021-BLG-1770L. It is estimated that the probabilities of the lens companions being in the BD mass range are 82\%, 85\%, 91\%, and 59\% for the individual events. For confirming the BD nature of the lens companions found in this and previous works by directly imaging the lenses from future high-resolution adaptive-optics (AO) followup observations, we provide the lens-source separations expected in 2030, which is an approximate year of the first AO light on 30~m class telescopes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.04921v1-abstract-full').style.display = 'none'; document.getElementById('2307.04921v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 10 tables, 8 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.00753">arXiv:2307.00753</a> <span> [<a href="https://arxiv.org/pdf/2307.00753">pdf</a>, <a href="https://arxiv.org/ps/2307.00753">ps</a>, <a href="https://arxiv.org/format/2307.00753">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> KMT-2022-BLG-0475Lb and KMT-2022-BLG-1480Lb: Microlensing ice giants detected via non-caustic-crossing channel </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Han%2C+C">Cheongho Han</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+C">Chung-Uk Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+I+A">Ian A. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Zang%2C+W">Weicheng Zang</a>, <a href="/search/astro-ph?searchtype=author&query=Chung%2C+S">Sun-Ju Chung</a>, <a href="/search/astro-ph?searchtype=author&query=Albrow%2C+M+D">Michael D. Albrow</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">Andrew Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Hwang%2C+K">Kyu-Ha Hwang</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+Y+K">Youn Kil Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Ryu%2C+Y">Yoon-Hyun Ryu</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+I">In-Gu Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Shvartzvald%2C+Y">Yossi Shvartzvald</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+H">Hongjing Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Yee%2C+J+C">Jennifer C. Yee</a>, <a href="/search/astro-ph?searchtype=author&query=Cha%2C+S">Sang-Mok Cha</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Doeon Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Dong-Jin Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+S">Seung-Lee Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+D">Dong-Joo Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+Y">Yongseok Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Park%2C+B">Byeong-Gon Park</a>, <a href="/search/astro-ph?searchtype=author&query=Pogge%2C+R+W">Richard W. Pogge</a>, <a href="/search/astro-ph?searchtype=author&query=Mao%2C+S">Shude Mao</a>, <a href="/search/astro-ph?searchtype=author&query=Zhu%2C+W">Wei Zhu</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+F">Fumio Abe</a> , et al. (27 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2307.00753v1-abstract-short" style="display: inline;"> We investigate the microlensing data collected in the 2022 season from the high-cadence microlensing surveys in order to find weak signals produced by planetary companions to lenses. From these searches, we find that two lensing events KMT-2022-BLG-0475 and KMT-2022-BLG-1480 exhibit weak short-term anomalies. From the detailed modeling of the lensing light curves, we identify that the anomalies ar… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.00753v1-abstract-full').style.display = 'inline'; document.getElementById('2307.00753v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.00753v1-abstract-full" style="display: none;"> We investigate the microlensing data collected in the 2022 season from the high-cadence microlensing surveys in order to find weak signals produced by planetary companions to lenses. From these searches, we find that two lensing events KMT-2022-BLG-0475 and KMT-2022-BLG-1480 exhibit weak short-term anomalies. From the detailed modeling of the lensing light curves, we identify that the anomalies are produced by planetary companions with a mass ratio to the primary of $q\sim 1.8\times 10^{-4}$ for KMT-2022-BLG-0475L and a ratio $q\sim 4.3\times 10^{-4}$ for KMT-2022-BLG-1480L. It is estimated that the host and planet masses and the projected planet-host separation are $(M_{\rm h}/M_\odot, M_{\rm p}/M_{\rm U}, a_\perp/{\rm au}) = (0.43^{+0.35}_{-0.23}, 1.73^{+1.42}_{-0.92}, 2.03^{+0.25}_{-0.38})$ for KMT-2022-BLG-0475L, and $(0.18^{+0.16}_{-0.09}, 1.82^{+1.60}_{-0.92}, 1.22^{+0.15}_{-0.14})$ for KMT-2022-BLG-1480L, where $M_{\rm U}$ denotes the mass of Uranus. Both planetary systems share common characteristics that the primaries of the lenses are early-mid M dwarfs lying in the Galactic bulge and the companions are ice giants lying beyond the snow lines of the planetary systems. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.00753v1-abstract-full').style.display = 'none'; document.getElementById('2307.00753v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 10 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.04870">arXiv:2306.04870</a> <span> [<a href="https://arxiv.org/pdf/2306.04870">pdf</a>, <a href="https://arxiv.org/ps/2306.04870">ps</a>, <a href="https://arxiv.org/format/2306.04870">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/ace169">10.3847/1538-3881/ace169 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> KMT-2022-BLG-2397: Brown Dwarf at the Upper Shore of the Einstein Desert </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">Andrew Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Ryu%2C+Y">Yoon-Hyun Ryu</a>, <a href="/search/astro-ph?searchtype=author&query=Yee%2C+J+C">Jennifer C. Yee</a>, <a href="/search/astro-ph?searchtype=author&query=Albrow%2C+M+D">Michael D. Albrow</a>, <a href="/search/astro-ph?searchtype=author&query=Chung%2C+S">Sun-Ju Chung</a>, <a href="/search/astro-ph?searchtype=author&query=Han%2C+C">Cheongho Han</a>, <a href="/search/astro-ph?searchtype=author&query=Hwang%2C+K">Kyu-Ha Hwang</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+Y+K">Youn Kil Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+I">In-Gu Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Shvartzvald%2C+Y">Yossi Shvartzvald</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+H">Hongjing Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Zang%2C+W">Weicheng Zang</a>, <a href="/search/astro-ph?searchtype=author&query=Cha%2C+S">Sang-Mok Cha</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Dong-Jin Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+S">Seung-Lee Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+C">Chung-Uk Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+D">Dong-Joo Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+Y">Yongseok Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Park%2C+B">Byeong-Gon Park</a>, <a href="/search/astro-ph?searchtype=author&query=Pogge%2C+R+W">Richard W. Pogge</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2306.04870v1-abstract-short" style="display: inline;"> We measure the Einstein radius of the single-lens microlensing event KMT-2022-BLG-2397 to be theta_E=24.8 +- 3.6 uas, placing it at the upper shore of the Einstein Desert, 9 < theta_E / uas < 25, between free-floating planets (FFPs) and bulge brown dwarfs (BDs). In contrast to the six BD (25 < theta_E < 50) events presented by Gould+22, which all had giant-star source stars, KMT-2022-BLG-2397 has… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.04870v1-abstract-full').style.display = 'inline'; document.getElementById('2306.04870v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.04870v1-abstract-full" style="display: none;"> We measure the Einstein radius of the single-lens microlensing event KMT-2022-BLG-2397 to be theta_E=24.8 +- 3.6 uas, placing it at the upper shore of the Einstein Desert, 9 < theta_E / uas < 25, between free-floating planets (FFPs) and bulge brown dwarfs (BDs). In contrast to the six BD (25 < theta_E < 50) events presented by Gould+22, which all had giant-star source stars, KMT-2022-BLG-2397 has a dwarf-star source, with angular radius theta_* ~ 0.9 uas. This prompts us to study the relative utility of dwarf and giant sources for characterizing FFPs and BDs from finite-source point-lens (FSPL) microlensing events. We find `dwarfs' (including main-sequence stars and subgiants) are likely to yield twice as many theta_E measurements for BDs and a comparable (but more difficult to quantify) improvement for FFPs. We show that neither current nor planned experiments will yield complete mass measurements of isolated bulge BDs, nor will any other planned experiment yield as many theta_E measurements for these objects as KMT. Thus, the currently anticipated 10-year KMT survey will remain the best way to study bulge BDs for several decades to come. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.04870v1-abstract-full').style.display = 'none'; document.getElementById('2306.04870v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">45 pages, 9 Figures, submitted to AAS Journals</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2305.15628">arXiv:2305.15628</a> <span> [<a href="https://arxiv.org/pdf/2305.15628">pdf</a>, <a href="https://arxiv.org/ps/2305.15628">ps</a>, <a href="https://arxiv.org/format/2305.15628">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202346596">10.1051/0004-6361/202346596 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> KMT-2021-BLG-1150Lb: Microlensing planet detected through a densely covered planetary-caustic signal </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Han%2C+C">Cheongho Han</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+Y+K">Youn Kil Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+I+A">Ian A. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">Andrew Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Chung%2C+S">Sun-Ju Chung</a>, <a href="/search/astro-ph?searchtype=author&query=Albrow%2C+M+D">Michael D. Albrow</a>, <a href="/search/astro-ph?searchtype=author&query=Hwang%2C+K">Kyu-Ha Hwang</a>, <a href="/search/astro-ph?searchtype=author&query=Ryu%2C+Y">Yoon-Hyun Ryu</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+I">In-Gu Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Shvartzvald%2C+Y">Yossi Shvartzvald</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+H">Hongjing Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Yee%2C+J+C">Jennifer C. Yee</a>, <a href="/search/astro-ph?searchtype=author&query=Zang%2C+W">Weicheng Zang</a>, <a href="/search/astro-ph?searchtype=author&query=Cha%2C+S">Sang-Mok Cha</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Doeon Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Dong-Jin Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+S">Seung-Lee Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+C">Chung-Uk Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+D">Dong-Joo Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+Y">Yongseok Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Park%2C+B">Byeong-Gon Park</a>, <a href="/search/astro-ph?searchtype=author&query=Pogge%2C+R+W">Richard W. Pogge</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+F">Fumio Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Barry%2C+R">Richard Barry</a>, <a href="/search/astro-ph?searchtype=author&query=Bennett%2C+D+P">David P. Bennett</a> , et al. (27 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2305.15628v1-abstract-short" style="display: inline;"> Recently, there have been reports of various types of degeneracies in the interpretation of planetary signals induced by planetary caustics. In this work, we check whether such degeneracies persist in the case of well-covered signals by analyzing the lensing event KMT-2021-BLG-1150, for which the light curve exhibits a densely and continuously covered short-term anomaly. In order to identify degen… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.15628v1-abstract-full').style.display = 'inline'; document.getElementById('2305.15628v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.15628v1-abstract-full" style="display: none;"> Recently, there have been reports of various types of degeneracies in the interpretation of planetary signals induced by planetary caustics. In this work, we check whether such degeneracies persist in the case of well-covered signals by analyzing the lensing event KMT-2021-BLG-1150, for which the light curve exhibits a densely and continuously covered short-term anomaly. In order to identify degenerate solutions, we thoroughly investigate the parameter space by conducting dense grid searches for the lensing parameters. We then check the severity of the degeneracy among the identified solutions. We identify a pair of planetary solutions resulting from the well-known inner-outer degeneracy, and find that interpreting the anomaly is not subject to any degeneracy other than the inner-outer degeneracy. The measured parameters of the planet separation (normalized to the Einstein radius) and mass ratio between the lens components are $(s, q)_{\rm in}\sim (1.297, 1.10\times 10^{-3})$ for the inner solution and $(s, q)_{\rm out}\sim (1.242, 1.15\times 10^{-3})$ for the outer solution. According to a Bayesian estimation, the lens is a planetary system consisting of a planet with a mass $M_{\rm p}=0.88^{+0.38}_{-0.36}~M_{\rm J}$ and its host with a mass $M_{\rm h}=0.73^{+0.32}_{-0.30}~M_\odot$ lying toward the Galactic center at a distance $D_{\rm L} =3.8^{+1.3}_{-1.2}$~kpc. By conducting analyses using mock data sets prepared to mimic those obtained with data gaps and under various observational cadences, it is found that gaps in data can result in various degenerate solutions, while the observational cadence does not pose a serious degeneracy problem as long as the anomaly feature can be delineated. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.15628v1-abstract-full').style.display = 'none'; document.getElementById('2305.15628v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 pages, 8 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2305.06605">arXiv:2305.06605</a> <span> [<a href="https://arxiv.org/pdf/2305.06605">pdf</a>, <a href="https://arxiv.org/ps/2305.06605">ps</a>, <a href="https://arxiv.org/format/2305.06605">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202245455">10.1051/0004-6361/202245455 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Probable brown dwarf companions detected in binary microlensing events during the 2018-2020 seasons of the KMTNet survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Han%2C+C">Cheongho Han</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+Y+K">Youn Kil Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Doeon Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">Andrew Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Bozza%2C+V">Valerio Bozza</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+I+A">Ian A. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Chung%2C+S">Sun-Ju Chung</a>, <a href="/search/astro-ph?searchtype=author&query=Albrow%2C+M+D">Michael D. Albrow</a>, <a href="/search/astro-ph?searchtype=author&query=Hwang%2C+K">Kyu-Ha Hwang</a>, <a href="/search/astro-ph?searchtype=author&query=Ryu%2C+Y">Yoon-Hyun Ryu</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+I">In-Gu Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Shvartzvald%2C+Y">Yossi Shvartzvald</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+H">Hongjing Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Zang%2C+W">Weicheng Zang</a>, <a href="/search/astro-ph?searchtype=author&query=Cha%2C+S">Sang-Mok Cha</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Dong-Jin Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+H">Hyoun-Woo Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+S">Seung-Lee Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+C">Chung-Uk Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+D">Dong-Joo Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Yee%2C+J+C">Jennifer C. Yee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+Y">Yongseok Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Park%2C+B">Byeong-Gon Park</a>, <a href="/search/astro-ph?searchtype=author&query=Pogge%2C+R+W">Richard W. Pogge</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+F">Fumio Abe</a> , et al. (26 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2305.06605v1-abstract-short" style="display: inline;"> We inspect the microlensing data of the KMTNet survey collected during the 2018--2020 seasons in order to find lensing events produced by binaries with brown-dwarf companions. In order to pick out binary-lens events with candidate BD lens companions, we conduct systematic analyses of all anomalous lensing events observed during the seasons. By applying the selection criterion with mass ratio betwe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.06605v1-abstract-full').style.display = 'inline'; document.getElementById('2305.06605v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.06605v1-abstract-full" style="display: none;"> We inspect the microlensing data of the KMTNet survey collected during the 2018--2020 seasons in order to find lensing events produced by binaries with brown-dwarf companions. In order to pick out binary-lens events with candidate BD lens companions, we conduct systematic analyses of all anomalous lensing events observed during the seasons. By applying the selection criterion with mass ratio between the lens components of $0.03\lesssim q\lesssim 0.1$, we identify four binary-lens events with candidate BD companions, including KMT-2018-BLG-0321, KMT-2018-BLG-0885, KMT-2019-BLG-0297, and KMT-2019-BLG-0335. For the individual events, we present the interpretations of the lens systems and measure the observables that can constrain the physical lens parameters. The masses of the lens companions estimated from the Bayesian analyses based on the measured observables indicate that the probabilities for the lens companions to be in the brown-dwarf mass regime are high: 59\%, 68\%, 66\%, and 66\% for the four events respectively. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.06605v1-abstract-full').style.display = 'none'; document.getElementById('2305.06605v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 8 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2304.03871">arXiv:2304.03871</a> <span> [<a href="https://arxiv.org/pdf/2304.03871">pdf</a>, <a href="https://arxiv.org/ps/2304.03871">ps</a>, <a href="https://arxiv.org/format/2304.03871">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202346298">10.1051/0004-6361/202346298 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> KMT-2021-BLG-2010Lb, KMT-2022-BLG-0371Lb, and KMT-2022-BLG-1013Lb: Three microlensing planets detected via partially covered signals </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Han%2C+C">Cheongho Han</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+C">Chung-Uk Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Zang%2C+W">Weicheng Zang</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+Y+K">Youn Kil Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Christie%2C+G+W">Grant W. Christie</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+J">Jiyuan Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Albrow%2C+M+D">Michael D. Albrow</a>, <a href="/search/astro-ph?searchtype=author&query=Chung%2C+S">Sun-Ju Chung</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">Andrew Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Hwang%2C+K">Kyu-Ha Hwang</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Doeon Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Ryu%2C+Y">Yoon-Hyun Ryu</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+I">In-Gu Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Shvartzvald%2C+Y">Yossi Shvartzvald</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+H">Hongjing Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Yee%2C+J+C">Jennifer C. Yee</a>, <a href="/search/astro-ph?searchtype=author&query=Cha%2C+S">Sang-Mok Cha</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Dong-Jin Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+S">Seung-Lee Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+D">Dong-Joo Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+Y">Yongseok Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Park%2C+B">Byeong-Gon Park</a>, <a href="/search/astro-ph?searchtype=author&query=Pogge%2C+R+W">Richard W. Pogge</a>, <a href="/search/astro-ph?searchtype=author&query=Natusch%2C+T">Tim Natusch</a>, <a href="/search/astro-ph?searchtype=author&query=Mao%2C+S">Shude Mao</a> , et al. (3 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2304.03871v1-abstract-short" style="display: inline;"> We inspect 4 microlensing events KMT-2021-BLG-1968, KMT-2021-BLG-2010, KMT-2022-BLG-0371, and KMT-2022-BLG-1013, for which the light curves exhibit partially covered short-term central anomalies. We conduct detailed analyses of the events with the aim of revealing the nature of the anomalies. We test various models that can give rise to the anomalies of the individual events including the binary-l… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.03871v1-abstract-full').style.display = 'inline'; document.getElementById('2304.03871v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.03871v1-abstract-full" style="display: none;"> We inspect 4 microlensing events KMT-2021-BLG-1968, KMT-2021-BLG-2010, KMT-2022-BLG-0371, and KMT-2022-BLG-1013, for which the light curves exhibit partially covered short-term central anomalies. We conduct detailed analyses of the events with the aim of revealing the nature of the anomalies. We test various models that can give rise to the anomalies of the individual events including the binary-lens (2L1S) and binary-source (1L2S) interpretations. Under the 2L1S interpretation, we thoroughly inspect the parameter space to check the existence of degenerate solutions, and if they exist, we test the feasibility of resolving the degeneracy. We find that the anomalies in KMT-2021-BLG-2010 and KMT-2022-BLG-1013 are uniquely defined by planetary-lens interpretations with the planet-to-host mass ratios of $q\sim 2.8\times 10^{-3}$ and $\sim 1.6\times 10^{-3}$, respectively. For KMT-2022-BLG-0371, a planetary solution with a mass ratio $q\sim 4\times 10^{-4}$ is strongly favored over the other three degenerate 2L1S solutions with different mass ratios based on the $蠂^2$ and relative proper motion arguments, and a 1L2S solution is clearly ruled out. For KMT-2021-BLG-1968, on the other hand, we find that the anomaly can be explained either by a planetary or a binary-source interpretation, making it difficult to firmly identify the nature of the anomaly. From the Bayesian analyses of the identified planetary events, we estimate that the masses of the planet and host are $(M_{\rm p}/M_{\rm J}, M_{\rm h}/M_\odot) = (1.07^{+1.15}_{-0.68}, 0.37^{+0.40}_{-0.23})$, $(0.26^{+0.13}_{-0.11}, 0.63^{+0.32}_{-0.28})$, and $(0.31^{+0.46}_{-0.16}, 0.18^{+0.28}_{-0.10})$ for KMT-2021-BLG-2010L, KMT-2022-BLG-0371L, and KMT-2022-BLG-1013L, respectively. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.03871v1-abstract-full').style.display = 'none'; document.getElementById('2304.03871v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 17 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2304.02815">arXiv:2304.02815</a> <span> [<a href="https://arxiv.org/pdf/2304.02815">pdf</a>, <a href="https://arxiv.org/ps/2304.02815">ps</a>, <a href="https://arxiv.org/format/2304.02815">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202346166">10.1051/0004-6361/202346166 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> MOA-2022-BLG-249Lb: Nearby microlensing super-Earth planet detected from high-cadence surveys </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Han%2C+C">Cheongho Han</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">Andrew Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+Y+K">Youn Kil Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+I+A">Ian A. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Zang%2C+W">Weicheng Zang</a>, <a href="/search/astro-ph?searchtype=author&query=Chung%2C+S">Sun-Ju Chung</a>, <a href="/search/astro-ph?searchtype=author&query=Albrow%2C+M+D">Michael D. Albrow</a>, <a href="/search/astro-ph?searchtype=author&query=Hwang%2C+K">Kyu-Ha Hwang</a>, <a href="/search/astro-ph?searchtype=author&query=Ryu%2C+Y">Yoon-Hyun Ryu</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+I">In-Gu Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Shvartzvald%2C+Y">Yossi Shvartzvald</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+H">Hongjing Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Yee%2C+J+C">Jennifer C. Yee</a>, <a href="/search/astro-ph?searchtype=author&query=Cha%2C+S">Sang-Mok Cha</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Doeon Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Dong-Jin Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+S">Seung-Lee Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+C">Chung-Uk Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+D">Dong-Joo Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+Y">Yongseok Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Park%2C+B">Byeong-Gon Park</a>, <a href="/search/astro-ph?searchtype=author&query=Pogge%2C+R+W">Richard W. Pogge</a>, <a href="/search/astro-ph?searchtype=author&query=Mao%2C+S">Shude Mao</a>, <a href="/search/astro-ph?searchtype=author&query=Zhu%2C+W">Wei Zhu</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+F">Fumio Abe</a> , et al. (29 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2304.02815v1-abstract-short" style="display: inline;"> We investigate the data collected by the high-cadence microlensing surveys during the 2022 season in search for planetary signals appearing in the light curves of microlensing events. From this search, we find that the lensing event MOA-2022-BLG-249 exhibits a brief positive anomaly that lasted for about 1 day with a maximum deviation of $\sim 0.2$~mag from a single-source single-lens model. We an… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.02815v1-abstract-full').style.display = 'inline'; document.getElementById('2304.02815v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.02815v1-abstract-full" style="display: none;"> We investigate the data collected by the high-cadence microlensing surveys during the 2022 season in search for planetary signals appearing in the light curves of microlensing events. From this search, we find that the lensing event MOA-2022-BLG-249 exhibits a brief positive anomaly that lasted for about 1 day with a maximum deviation of $\sim 0.2$~mag from a single-source single-lens model. We analyze the light curve under the two interpretations of the anomaly: one originated by a low-mass companion to the lens (planetary model) and the other originated by a faint companion to the source (binary-source model). It is found that the anomaly is better explained by the planetary model than the binary-source model. We identify two solutions rooted in the inner--outer degeneracy, for both of which the estimated planet-to-host mass ratio, $q\sim 8\times 10^{-5}$, is very small. With the constraints provided by the microlens parallax and the lower limit on the Einstein radius, as well as the blend-flux constraint, we find that the lens is a planetary system, in which a super-Earth planet, with a mass $(4.83\pm 1.44)~M_\oplus$, orbits a low-mass host star, with a mass $(0.18\pm 0.05)~M_\odot$, lying in the Galactic disk at a distance $(2.00\pm 0.42)$~kpc. The planet detection demonstrates the elevated microlensing sensitivity of the current high-cadence lensing surveys to low-mass planets. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.02815v1-abstract-full').style.display = 'none'; document.getElementById('2304.02815v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 9 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.16881">arXiv:2303.16881</a> <span> [<a href="https://arxiv.org/pdf/2303.16881">pdf</a>, <a href="https://arxiv.org/ps/2303.16881">ps</a>, <a href="https://arxiv.org/format/2303.16881">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Systematic KMTNet Planetary Anomaly Search. IX. Complete Sample of 2016 Prime-Field Planets </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Shin%2C+I">In-Gu Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Yee%2C+J+C">Jennifer C. Yee</a>, <a href="/search/astro-ph?searchtype=author&query=Zang%2C+W">Weicheng Zang</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+H">Hongjing Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Hwang%2C+K">Kyu-Ha Hwang</a>, <a href="/search/astro-ph?searchtype=author&query=Han%2C+C">Cheongho Han</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">Andrew Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">Andrzej Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+I+A">Ian A. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Albrow%2C+M+D">Michael D. Albrow</a>, <a href="/search/astro-ph?searchtype=author&query=Chung%2C+S">Sun-Ju Chung</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+Y+K">Youn Kil Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Ryu%2C+Y">Yoon-Hyun Ryu</a>, <a href="/search/astro-ph?searchtype=author&query=Shvartzvald%2C+Y">Yossi Shvartzvald</a>, <a href="/search/astro-ph?searchtype=author&query=Cha%2C+S">Sang-Mok Cha</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Dong-Jin Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+S">Seung-Lee Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+C">Chung-Uk Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+D">Dong-Joo Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+Y">Yongseok Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Park%2C+B">Byeong-Gon Park</a>, <a href="/search/astro-ph?searchtype=author&query=Pogge%2C+R+W">Richard W. Pogge</a>, <a href="/search/astro-ph?searchtype=author&query=Mr%C3%B3z%2C+P">Przemek Mr贸z</a>, <a href="/search/astro-ph?searchtype=author&query=Szyma%C5%84ski%2C+M+K">Micha艂 K. Szyma艅ski</a>, <a href="/search/astro-ph?searchtype=author&query=Skowron%2C+J">Jan Skowron</a> , et al. (36 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2303.16881v1-abstract-short" style="display: inline;"> As a part of the ``Systematic KMTNet Planetary Anomaly Search" series, we report five new planets (namely, OGLE-2016-BLG-1635Lb, MOA-2016-BLG-532Lb, KMT-2016-BLG-0625Lb, OGLE-2016-BLG-1850Lb, and KMT-2016-BLG-1751Lb) and one planet candidate (KMT-2016-BLG-1855), which were found by searching $2016$ KMTNet prime fields. These $buried$ planets show a wide range of masses from Earth--class to Super--… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.16881v1-abstract-full').style.display = 'inline'; document.getElementById('2303.16881v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.16881v1-abstract-full" style="display: none;"> As a part of the ``Systematic KMTNet Planetary Anomaly Search" series, we report five new planets (namely, OGLE-2016-BLG-1635Lb, MOA-2016-BLG-532Lb, KMT-2016-BLG-0625Lb, OGLE-2016-BLG-1850Lb, and KMT-2016-BLG-1751Lb) and one planet candidate (KMT-2016-BLG-1855), which were found by searching $2016$ KMTNet prime fields. These $buried$ planets show a wide range of masses from Earth--class to Super--Jupiter--class, and are located in both the disk and the bulge. The ultimate goal of this series is to build a complete planet sample. Because our work provides a complementary sample to other planet detection methods, which have different detection sensitivities, our complete sample will help us to obtain a better understanding of planet demographics in our Galaxy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.16881v1-abstract-full').style.display = 'none'; document.getElementById('2303.16881v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">38 pages, 17 figures, 12 Tables, submitted to the AAS journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.13544">arXiv:2302.13544</a> <span> [<a href="https://arxiv.org/pdf/2302.13544">pdf</a>, <a href="https://arxiv.org/ps/2302.13544">ps</a>, <a href="https://arxiv.org/format/2302.13544">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/accb8f">10.3847/1538-3881/accb8f <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Systematic KMTNet Planetary Anomaly Search. VIII. Complete Sample of 2019 Subprime Field Planets </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Jung%2C+Y+K">Youn Kil Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Zang%2C+W">Weicheng Zang</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+H">Hanyue Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Han%2C+C">Cheongho Han</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">Andrew Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">Andrzej Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Albrow%2C+M+D">Michael D. Albrow</a>, <a href="/search/astro-ph?searchtype=author&query=Chung%2C+S">Sun-Ju Chung</a>, <a href="/search/astro-ph?searchtype=author&query=Hwang%2C+K">Kyu-Ha Hwang</a>, <a href="/search/astro-ph?searchtype=author&query=Ryu%2C+Y">Yoon-Hyun Ryu</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+I">In-Gu Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Shvartzvald%2C+Y">Yossi Shvartzvald</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+H">Hongjing Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Yee%2C+J+C">Jennifer C. Yee</a>, <a href="/search/astro-ph?searchtype=author&query=Cha%2C+S">Sang-Mok Cha</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Dong-Jin Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+S">Seung-Lee Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+C">Chung-Uk Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+D">Dong-Joo Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+Y">Yongseok Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Park%2C+B">Byeong-Gon Park</a>, <a href="/search/astro-ph?searchtype=author&query=Pogge%2C+R+W">Richard W. Pogge</a>, <a href="/search/astro-ph?searchtype=author&query=Mr%C3%B3z%2C+P">Przemek Mr贸z</a>, <a href="/search/astro-ph?searchtype=author&query=Szyma%C5%84ski%2C+M+K">Micha艂 K. Szyma艅ski</a>, <a href="/search/astro-ph?searchtype=author&query=Skowron%2C+J">Jan Skowron</a> , et al. (19 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2302.13544v1-abstract-short" style="display: inline;"> We complete the publication of all microlensing planets (and ``possible planets'') identified by the uniform approach of the KMT AnomalyFinder system in the 21 KMT subprime fields during the 2019 observing season, namely KMT-2019-BLG-0298, KMT-2019-BLG-1216, KMT-2019-BLG-2783, OGLE-2019-BLG-0249, and OGLE-2019-BLG-0679 (planets), as well as OGLE-2019-BLG-0344, and KMT-2019-BLG-0304 (possible plane… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.13544v1-abstract-full').style.display = 'inline'; document.getElementById('2302.13544v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.13544v1-abstract-full" style="display: none;"> We complete the publication of all microlensing planets (and ``possible planets'') identified by the uniform approach of the KMT AnomalyFinder system in the 21 KMT subprime fields during the 2019 observing season, namely KMT-2019-BLG-0298, KMT-2019-BLG-1216, KMT-2019-BLG-2783, OGLE-2019-BLG-0249, and OGLE-2019-BLG-0679 (planets), as well as OGLE-2019-BLG-0344, and KMT-2019-BLG-0304 (possible planets). The five planets have mean log mass-ratio measurements of $(-2.6,-3.6,-2.5,-2.2,-2.3)$, median mass estimates of $(1.81,0.094,1.16,7.12,3.34)\, M_{\rm Jup}$, and median distance estimates of $(6.7,2.7,5.9,6.4,5.6)\, {\rm kpc}$, respectively. The main scientific interest of these planets is that they complete the AnomalyFinder sample for 2019, which has a total of 25 planets that are likely to enter the statistical sample. We find statistical consistency with the previously published 33 planets from the 2018 AnomalyFinder analysis according to an ensemble of five tests. Of the 58 planets from 2018-2019, 23 were newly discovered by AnomalyFinder. Within statistical precision, half of all the planets have caustic crossings while half do not (as predicted by Zhu et al. 2014), an equal number of detected planets result from major-image and minor-image light-curve perturbations, and an equal number come from KMT prime fields versus subprime fields. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.13544v1-abstract-full').style.display = 'none'; document.getElementById('2302.13544v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 tables, 20 figures, submitted to AAS journals</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.07497">arXiv:2302.07497</a> <span> [<a href="https://arxiv.org/pdf/2302.07497">pdf</a>, <a href="https://arxiv.org/format/2302.07497">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/ac7d4c">10.3847/1538-3881/ac7d4c <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> OGLE-2017-BLG-1038: A Possible Brown-dwarf Binary Revealed by Spitzer Microlensing Parallax </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Malpas%2C+A">Amber Malpas</a>, <a href="/search/astro-ph?searchtype=author&query=Albrow%2C+M+D">Michael D. Albrow</a>, <a href="/search/astro-ph?searchtype=author&query=Yee%2C+J+C">Jennifer C. Yee</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">Andrew Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">Andrzej Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Martin%2C+A+H">Antonio Herrera Martin</a>, <a href="/search/astro-ph?searchtype=author&query=Team%2C+S">Spitzer Team</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Beichman%2C+C+A">Charles A. Beichman</a>, <a href="/search/astro-ph?searchtype=author&query=Bryden%2C+G">Geoffery Bryden</a>, <a href="/search/astro-ph?searchtype=author&query=Novati%2C+S+C">Sebastiano Calchi Novati</a>, <a href="/search/astro-ph?searchtype=author&query=Carey%2C+S">Sean Carey</a>, <a href="/search/astro-ph?searchtype=author&query=Henderson%2C+C+B">Calen B. Henderson</a>, <a href="/search/astro-ph?searchtype=author&query=Gaudi%2C+B+S">B. Scott Gaudi</a>, <a href="/search/astro-ph?searchtype=author&query=Shvartzvald%2C+Y">Yossi Shvartzvald</a>, <a href="/search/astro-ph?searchtype=author&query=Zhu%2C+W">Wei Zhu</a>, <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+K">KMTNet Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Cha%2C+S">Sang-Mok Cha</a>, <a href="/search/astro-ph?searchtype=author&query=Chung%2C+S">Sun-Ju Chung</a>, <a href="/search/astro-ph?searchtype=author&query=Han%2C+C">Cheongho Han</a>, <a href="/search/astro-ph?searchtype=author&query=Hwang%2C+K">Kyu-Ha Hwang</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+Y+K">Youn Kil Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Dong-Jin Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+H">Hyoun-Woo Kim</a> , et al. (21 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2302.07497v1-abstract-short" style="display: inline;"> We report the analysis of microlensing event OGLE-2017-BLG-1038, observed by the Optical Gravitational Lensing Experiment, Korean Microlensing Telescope Network, and Spitzer telescopes. The event is caused by a giant source star in the Galactic Bulge passing over a large resonant binary lens caustic. The availability of space-based data allows the full set of physical parameters to be calculated.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.07497v1-abstract-full').style.display = 'inline'; document.getElementById('2302.07497v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.07497v1-abstract-full" style="display: none;"> We report the analysis of microlensing event OGLE-2017-BLG-1038, observed by the Optical Gravitational Lensing Experiment, Korean Microlensing Telescope Network, and Spitzer telescopes. The event is caused by a giant source star in the Galactic Bulge passing over a large resonant binary lens caustic. The availability of space-based data allows the full set of physical parameters to be calculated. However, there exists an eightfold degeneracy in the parallax measurement. The four best solutions correspond to very-low-mass binaries near ($M_1 = 170^{+40}_{-50} M_J$ and $M_2 = 110^{+20}_{-30} M_J$), or well below ($M_1 = 22.5^{+0.7}_{-0.4} M_J$ and $M_2 = 13.3^{+0.4}_{-0.3} M_J$) the boundary between stars and brown dwarfs. A conventional analysis, with scaled uncertainties for Spitzer data, implies a very-low-mass brown dwarf binary lens at a distance of 2 kpc. Compensating for systematic Spitzer errors using a Gaussian process model suggests that a higher mass M-dwarf binary at 6 kpc is equally likely. A Bayesian comparison based on a galactic model favors the larger-mass solutions. We demonstrate how this degeneracy can be resolved within the next ten years through infrared adaptive-optics imaging with a 40 m class telescope. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.07497v1-abstract-full').style.display = 'none'; document.getElementById('2302.07497v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 11 figures, 4 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> AJ 164 (2022) 102 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.05613">arXiv:2302.05613</a> <span> [<a href="https://arxiv.org/pdf/2302.05613">pdf</a>, <a href="https://arxiv.org/ps/2302.05613">ps</a>, <a href="https://arxiv.org/format/2302.05613">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202245644">10.1051/0004-6361/202245644 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> KMT-2021-BLG-1122L: The first microlensing triple stellar system </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Han%2C+C">Cheongho Han</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+Y+K">Youn Kil Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">Andrew Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Doeon Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+C">Chung-Uk Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Albrow%2C+M+D">Michael D. Albrow</a>, <a href="/search/astro-ph?searchtype=author&query=Chung%2C+S">Sun-Ju Chung</a>, <a href="/search/astro-ph?searchtype=author&query=Hwang%2C+K">Kyu-Ha Hwang</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+H">Hyoun-Woo Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Ryu%2C+Y">Yoon-Hyun Ryu</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+I">In-Gu Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Shvartzvald%2C+Y">Yossi Shvartzvald</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+H">Hongjing Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Yee%2C+J+C">Jennifer C. Yee</a>, <a href="/search/astro-ph?searchtype=author&query=Zang%2C+W">Weicheng Zang</a>, <a href="/search/astro-ph?searchtype=author&query=Cha%2C+S">Sang-Mok Cha</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Dong-Jin Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+S">Seung-Lee Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+D">Dong-Joo Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+Y">Yongseok Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Park%2C+B">Byeong-Gon Park</a>, <a href="/search/astro-ph?searchtype=author&query=Pogge%2C+R+W">Richard W. Pogge</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2302.05613v1-abstract-short" style="display: inline;"> We systematically inspect the microlensing data acquired by the KMTNet survey during the previous seasons in order to find anomalous lensing events for which the anomalies in the lensing light curves cannot be explained by the usual binary-lens or binary-source interpretations. From the inspection, we find that interpreting the three lensing events OGLE-2018-BLG-0584, KMT-2018-BLG-2119, and KMT-20… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.05613v1-abstract-full').style.display = 'inline'; document.getElementById('2302.05613v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.05613v1-abstract-full" style="display: none;"> We systematically inspect the microlensing data acquired by the KMTNet survey during the previous seasons in order to find anomalous lensing events for which the anomalies in the lensing light curves cannot be explained by the usual binary-lens or binary-source interpretations. From the inspection, we find that interpreting the three lensing events OGLE-2018-BLG-0584, KMT-2018-BLG-2119, and KMT-2021-BLG-1122 requires four-body (lens+source) models, in which either both the lens and source are binaries (2L2S event) or the lens is a triple system (3L1S event). Following the analyses of the 2L2S events presented in \citet{Han2023}, here we present the 3L1S analysis of the KMT-2021-BLG-1122. It is found that the lens of the event KMT-2021-BLG-1122 is composed of three masses, in which the projected separations (normalized to the angular Einstein radius) and mass ratios between the lens companions and the primary are $(s_2, q_2)\sim (1.4, 0.53)$ and $(s_3, q_3) \sim (1.6, 0.24)$. By conducting a Bayesian analysis, we estimate that the masses of the individual lens components are $(M_1, M_2, M_3)\sim (0.47\,M_\odot, 0.24\,M_\odot, 0.11\,M_\odot)$. The companions are separated in projection from the primary by $(a_{\perp,2}, a_{\perp,3})\sim (3.5, 4.0)$~AU. The lens of KMT-2018-BLG-2119 is the first triple stellar system detected via microlensing. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.05613v1-abstract-full').style.display = 'none'; document.getElementById('2302.05613v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 7 figures, 2 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2301.06779">arXiv:2301.06779</a> <span> [<a href="https://arxiv.org/pdf/2301.06779">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stad1398">10.1093/mnras/stad1398 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> KMT-2022-BLG-0440Lb: A New $q < 10^{-4}$ Microlensing Planet with the Central-Resonant Caustic Degeneracy Broken </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+J">Jiyuan Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Zang%2C+W">Weicheng Zang</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+Y+K">Youn Kil Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+H">Hongjing Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">Andrew Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Sumi%2C+T">Takahiro Sumi</a>, <a href="/search/astro-ph?searchtype=author&query=Mao%2C+S">Shude Mao</a>, <a href="/search/astro-ph?searchtype=author&query=Dong%2C+S">Subo Dong</a>, <a href="/search/astro-ph?searchtype=author&query=Albrow%2C+M+D">Michael D. Albrow</a>, <a href="/search/astro-ph?searchtype=author&query=Chung%2C+S">Sun-Ju Chung</a>, <a href="/search/astro-ph?searchtype=author&query=Han%2C+C">Cheongho Han</a>, <a href="/search/astro-ph?searchtype=author&query=Hwang%2C+K">Kyu-Ha Hwang</a>, <a href="/search/astro-ph?searchtype=author&query=Ryu%2C+Y">Yoon-Hyun Ryu</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+I">In-Gu Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Shvartzvald%2C+Y">Yossi Shvartzvald</a>, <a href="/search/astro-ph?searchtype=author&query=Yee%2C+J+C">Jennifer C. Yee</a>, <a href="/search/astro-ph?searchtype=author&query=Cha%2C+S">Sang-Mok Cha</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Dong-Jin Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+H">Hyoun-Woo Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+S">Seung-Lee Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+C">Chung-Uk Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+D">Dong-Joo Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+Y">Yongseok Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Park%2C+B">Byeong-Gon Park</a>, <a href="/search/astro-ph?searchtype=author&query=Pogge%2C+R+W">Richard W. Pogge</a> , et al. (35 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2301.06779v2-abstract-short" style="display: inline;"> We present the observations and analysis of a high-magnification microlensing planetary event, KMT-2022-BLG-0440, for which the weak and short-lived planetary signal was covered by both the KMTNet survey and follow-up observations. The binary-lens models with a central caustic provide the best fits, with a planet/host mass ratio, $q = 0.75$--$1.00 \times 10^{-4}$ at $1蟽$. The binary-lens models wi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.06779v2-abstract-full').style.display = 'inline'; document.getElementById('2301.06779v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.06779v2-abstract-full" style="display: none;"> We present the observations and analysis of a high-magnification microlensing planetary event, KMT-2022-BLG-0440, for which the weak and short-lived planetary signal was covered by both the KMTNet survey and follow-up observations. The binary-lens models with a central caustic provide the best fits, with a planet/host mass ratio, $q = 0.75$--$1.00 \times 10^{-4}$ at $1蟽$. The binary-lens models with a resonant caustic and a brown-dwarf mass ratio are both excluded by $螖蠂^2 > 70$. The binary-source model can fit the anomaly well but is rejected by the ``color argument'' on the second source. From Bayesian analyses, it is estimated that the host star is likely a K or M dwarf located in the Galactic disk, the planet probably has a Neptune-mass, and the projected planet-host separation is $1.9^{+0.6}_{-0.7}$ or $4.6^{+1.4}_{-1.7}$ au, subject to the close/wide degeneracy. This is the third $q < 10^{-4}$ planet from a high-magnification planetary signal ($A \gtrsim 65$). Together with another such planet, KMT-2021-BLG-0171Lb, the ongoing follow-up program for the KMTNet high-magnification events has demonstrated its ability in detecting high-magnification planetary signals for $q < 10^{-4}$ planets, which are challenging for the current microlensing surveys. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.06779v2-abstract-full').style.display = 'none'; document.getElementById('2301.06779v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">MNRAS accepted</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2212.13019">arXiv:2212.13019</a> <span> [<a href="https://arxiv.org/pdf/2212.13019">pdf</a>, <a href="https://arxiv.org/ps/2212.13019">ps</a>, <a href="https://arxiv.org/format/2212.13019">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202245525">10.1051/0004-6361/202245525 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> OGLE-2018-BLG-0584 and KMT-2018-BLG-2119: two microlensing events with two lens masses and two source stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Han%2C+C">Cheongho Han</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">Andrzej Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+Y+K">Youn Kil Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Doeon Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+H">Hongjing Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Albrow%2C+M+D">Michael D. Albrow</a>, <a href="/search/astro-ph?searchtype=author&query=Chung%2C+S">Sun-Ju Chung</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">Andrew Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Hwang%2C+K">Kyu-Ha Hwang</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+H">Hyoun-Woo Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+C">Chung-Uk Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Ryu%2C+Y">Yoon-Hyun Ryu</a>, <a href="/search/astro-ph?searchtype=author&query=Shvartzvald%2C+Y">Yossi Shvartzvald</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+I">In-Gu Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Yee%2C+J+C">Jennifer C. Yee</a>, <a href="/search/astro-ph?searchtype=author&query=Zang%2C+W">Weicheng Zang</a>, <a href="/search/astro-ph?searchtype=author&query=Cha%2C+S">Sang-Mok Cha</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Dong-Jin Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+S">Seung-Lee Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+D">Dong-Joo Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+Y">Yongseok Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Park%2C+B">Byeong-Gon Park</a>, <a href="/search/astro-ph?searchtype=author&query=Pogge%2C+R+W">Richard W. Pogge</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+C">Chun-Hwey Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+W">Woong-Tae Kim</a> , et al. (12 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2212.13019v1-abstract-short" style="display: inline;"> We conduct a systematic investigation of the microlensing data collected during the previous observation seasons for the purpose of reanalyzing anomalous lensing events with no suggested plausible models. We find that two anomalous lensing events OGLE-2018-BLG-0584 and KMT-2018-BLG-2119 cannot be explained with the usual models based on either a binary-lens single-source (2L1S) or a single-lens bi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.13019v1-abstract-full').style.display = 'inline'; document.getElementById('2212.13019v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.13019v1-abstract-full" style="display: none;"> We conduct a systematic investigation of the microlensing data collected during the previous observation seasons for the purpose of reanalyzing anomalous lensing events with no suggested plausible models. We find that two anomalous lensing events OGLE-2018-BLG-0584 and KMT-2018-BLG-2119 cannot be explained with the usual models based on either a binary-lens single-source (2L1S) or a single-lens binary-source (1L2S) interpretation. We test the feasibility of explaining the light curves with more sophisticated models by adding an extra lens (3L1S model) or a source (2L2S model) component to the 2L1S lens-system configuration. We find that a 2L2S interpretation well explains the light curves of both events, for each of which there are a pair of solutions resulting from the close and wide degeneracy. For the event OGLE-2018-BLG-0584, the source is a binary composed of two K-type stars, and the lens is a binary composed of two M dwarfs. For KMT-2018-BLG-2119, the source is a binary composed of two dwarfs of G and K spectral types, and the lens is a binary composed of a low-mass M dwarf and a brown dwarf. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.13019v1-abstract-full').style.display = 'none'; document.getElementById('2212.13019v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 December, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 pages, 9 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2210.12344">arXiv:2210.12344</a> <span> [<a href="https://arxiv.org/pdf/2210.12344">pdf</a>, <a href="https://arxiv.org/format/2210.12344">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/acb34b">10.3847/1538-3881/acb34b <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Systematic KMTNet Planetary Anomaly Search, Paper VII: Complete Sample of $q < 10^{-4}$ Planets from the First Four-Year Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zang%2C+W">Weicheng Zang</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+Y+K">Youn Kil Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+H">Hongjing Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+X">Xiangyu Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">Andrzej Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Yee%2C+J+C">Jennifer C. Yee</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">Andrew Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Mao%2C+S">Shude Mao</a>, <a href="/search/astro-ph?searchtype=author&query=Albrow%2C+M+D">Michael D. Albrow</a>, <a href="/search/astro-ph?searchtype=author&query=Chung%2C+S">Sun-Ju Chung</a>, <a href="/search/astro-ph?searchtype=author&query=Han%2C+C">Cheongho Han</a>, <a href="/search/astro-ph?searchtype=author&query=Hwang%2C+K">Kyu-Ha Hwang</a>, <a href="/search/astro-ph?searchtype=author&query=Ryu%2C+Y">Yoon-Hyun Ryu</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+I">In-Gu Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Shvartzvald%2C+Y">Yossi Shvartzvald</a>, <a href="/search/astro-ph?searchtype=author&query=Cha%2C+S">Sang-Mok Cha</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Dong-Jin Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+H">Hyoun-Woo Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+S">Seung-Lee Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+C">Chung-Uk Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+D">Dong-Joo Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+Y">Yongseok Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Park%2C+B">Byeong-Gon Park</a>, <a href="/search/astro-ph?searchtype=author&query=Pogge%2C+R+W">Richard W. Pogge</a>, <a href="/search/astro-ph?searchtype=author&query=Mr%C3%B3z%2C+P">Przemek Mr贸z</a> , et al. (14 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2210.12344v2-abstract-short" style="display: inline;"> We present the analysis of seven microlensing planetary events with planet/host mass ratios $q < 10^{-4}$: KMT-2017-BLG-1194, KMT-2017-BLG-0428, KMT-2019-BLG-1806, KMT-2017-BLG-1003, KMT-2019-BLG-1367, OGLE-2017-BLG-1806, and KMT-2016-BLG-1105. They were identified by applying the Korea Microlensing Telescope Network (KMTNet) AnomalyFinder algorithm to 2016--2019 KMTNet events. A Bayesian analysis… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.12344v2-abstract-full').style.display = 'inline'; document.getElementById('2210.12344v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.12344v2-abstract-full" style="display: none;"> We present the analysis of seven microlensing planetary events with planet/host mass ratios $q < 10^{-4}$: KMT-2017-BLG-1194, KMT-2017-BLG-0428, KMT-2019-BLG-1806, KMT-2017-BLG-1003, KMT-2019-BLG-1367, OGLE-2017-BLG-1806, and KMT-2016-BLG-1105. They were identified by applying the Korea Microlensing Telescope Network (KMTNet) AnomalyFinder algorithm to 2016--2019 KMTNet events. A Bayesian analysis indicates that all the lens systems consist of a cold super-Earth orbiting an M or K dwarf. Together with 17 previously published and three that will be published elsewhere, AnomalyFinder has found a total of 27 planets that have solutions with $q < 10^{-4}$ from 2016--2019 KMTNet events, which lays the foundation for the first statistical analysis of the planetary mass-ratio function based on KMTNet data. By reviewing the 27 planets, we find that the missing planetary caustics problem in the KMTNet planetary sample has been solved by AnomalyFinder. We also find a desert of high-magnification planetary signals ($A \gtrsim 65$), and a follow-up project for KMTNet high-magnification events could detect at least two more $q < 10^{-4}$ planets per year and form an independent statistical sample. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.12344v2-abstract-full').style.display = 'none'; document.getElementById('2210.12344v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">AJ in press</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2210.02436">arXiv:2210.02436</a> <span> [<a href="https://arxiv.org/pdf/2210.02436">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/acbcc8">10.3847/1538-3881/acbcc8 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> MOA-2020-BLG-208Lb: Cool Sub-Saturn Planet Within Predicted Desert </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Olmschenk%2C+G">Greg Olmschenk</a>, <a href="/search/astro-ph?searchtype=author&query=Bennett%2C+D+P">David P. Bennett</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+I+A">Ian A. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Zang%2C+W">Weicheng Zang</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+Y+K">Youn Kil Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Yee%2C+J+C">Jennifer C. Yee</a>, <a href="/search/astro-ph?searchtype=author&query=Bachelet%2C+E">Etienne Bachelet</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+F">Fumio Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Barry%2C+R+K">Richard K. Barry</a>, <a href="/search/astro-ph?searchtype=author&query=Bhattacharya%2C+A">Aparna Bhattacharya</a>, <a href="/search/astro-ph?searchtype=author&query=Fujii%2C+H">Hirosane Fujii</a>, <a href="/search/astro-ph?searchtype=author&query=Fukui%2C+A">Akihiko Fukui</a>, <a href="/search/astro-ph?searchtype=author&query=Hirao%2C+Y">Yuki Hirao</a>, <a href="/search/astro-ph?searchtype=author&query=Silva%2C+S+I">Stela Ishitani Silva</a>, <a href="/search/astro-ph?searchtype=author&query=Itow%2C+Y">Yoshitaka Itow</a>, <a href="/search/astro-ph?searchtype=author&query=Kirikawa%2C+R">Rintaro Kirikawa</a>, <a href="/search/astro-ph?searchtype=author&query=Kondo%2C+I">Iona Kondo</a>, <a href="/search/astro-ph?searchtype=author&query=Koshimoto%2C+N">Naoki Koshimoto</a>, <a href="/search/astro-ph?searchtype=author&query=Matsubara%2C+Y">Yutaka Matsubara</a>, <a href="/search/astro-ph?searchtype=author&query=Matsumoto%2C+S">Sho Matsumoto</a>, <a href="/search/astro-ph?searchtype=author&query=Miyazaki%2C+S">Shota Miyazaki</a>, <a href="/search/astro-ph?searchtype=author&query=Munford%2C+B">Brandon Munford</a>, <a href="/search/astro-ph?searchtype=author&query=Muraki%2C+Y">Yasushi Muraki</a>, <a href="/search/astro-ph?searchtype=author&query=Okamura%2C+A">Arisa Okamura</a>, <a href="/search/astro-ph?searchtype=author&query=Ranc%2C+C">Cl茅ment Ranc</a> , et al. (52 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2210.02436v2-abstract-short" style="display: inline;"> We analyze the MOA-2020-BLG-208 gravitational microlensing event and present the discovery and characterization of a new planet, MOA-2020-BLG-208Lb, with an estimated sub-Saturn mass. With a mass ratio $q = 3.17^{+0.28}_{-0.26} \times 10^{-4}$ and a separation $s = 1.3807^{+0.0018}_{-0.0018}$, the planet lies near the peak of the mass-ratio function derived by the MOA collaboration (Suzuki et al.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.02436v2-abstract-full').style.display = 'inline'; document.getElementById('2210.02436v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.02436v2-abstract-full" style="display: none;"> We analyze the MOA-2020-BLG-208 gravitational microlensing event and present the discovery and characterization of a new planet, MOA-2020-BLG-208Lb, with an estimated sub-Saturn mass. With a mass ratio $q = 3.17^{+0.28}_{-0.26} \times 10^{-4}$ and a separation $s = 1.3807^{+0.0018}_{-0.0018}$, the planet lies near the peak of the mass-ratio function derived by the MOA collaboration (Suzuki et al. 2016), near the edge of expected sample sensitivity. For these estimates we provide results using two mass law priors: one assuming that all stars have an equal planet-hosting probability, and the other assuming that planets are more likely to orbit around more massive stars. In the first scenario, we estimate that the lens system is likely to be a planet of mass $m_\mathrm{planet} = 46^{+42}_{-24} \; M_\oplus$ and a host star of mass $M_\mathrm{host} = 0.43^{+0.39}_{-0.23} \; M_\odot$, located at a distance $D_L = 7.49^{+0.99}_{-1.13} \; \mathrm{kpc}$. For the second scenario, we estimate $m_\mathrm{planet} = 69^{+37}_{-34} \; M_\oplus$, $M_\mathrm{host} = 0.66^{+0.35}_{-0.32} \; M_\odot$, and $D_L = 7.81^{+0.93}_{-0.93} \; \mathrm{kpc}$. As a cool sub-Saturn-mass planet, this planet adds to a growing collection of evidence for revised planetary formation models and qualifies for inclusion in the extended MOA-II exoplanet microlensing sample. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.02436v2-abstract-full').style.display = 'none'; document.getElementById('2210.02436v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The Astronomical Journal, 2023, Volume 165, Page 175 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.04607">arXiv:2209.04607</a> <span> [<a href="https://arxiv.org/pdf/2209.04607">pdf</a>, <a href="https://arxiv.org/ps/2209.04607">ps</a>, <a href="https://arxiv.org/format/2209.04607">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202244186">10.1051/0004-6361/202244186 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Brown-dwarf companions in microlensing binaries detected during the 2016--2018 seasons </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Han%2C+C">Cheongho Han</a>, <a href="/search/astro-ph?searchtype=author&query=Ryu%2C+Y">Yoon-Hyun Ryu</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+I">In-Gu Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+Y+K">Youn Kil Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Doeon Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Hirao%2C+Y">Yuki Hirao</a>, <a href="/search/astro-ph?searchtype=author&query=Bozza%2C+V">Valerio Bozza</a>, <a href="/search/astro-ph?searchtype=author&query=Albrow%2C+M+D">Michael D. Albrow</a>, <a href="/search/astro-ph?searchtype=author&query=Zang%2C+W">Weicheng Zang</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">Andrzej Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+I+A">Ian A. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Chung%2C+S">Sun-Ju Chung</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">Andrew Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Hwang%2C+K">Kyu-Ha Hwang</a>, <a href="/search/astro-ph?searchtype=author&query=Shvartzvald%2C+Y">Yossi Shvartzvald</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+H">Hongjing Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Cha%2C+S">Sang-Mok Cha</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Dong-Jin Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+H">Hyoun-Woo Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+S">Seung-Lee Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+C">Chung-Uk Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+D">Dong-Joo Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Yee%2C+J+C">Jennifer C. Yee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+Y">Yongseok Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Park%2C+B">Byeong-Gon Park</a> , et al. (38 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2209.04607v1-abstract-short" style="display: inline;"> With the aim of finding microlensing binaries containing brown-dwarf (BD) companions, we investigate the microlensing survey data collected during the 2016--2018 seasons. For this purpose, we first conducted modeling of lensing events with light curves exhibiting anomaly features that are likely to be produced by binary lenses. We then sorted out BD-companion binary-lens events by applying the cri… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.04607v1-abstract-full').style.display = 'inline'; document.getElementById('2209.04607v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.04607v1-abstract-full" style="display: none;"> With the aim of finding microlensing binaries containing brown-dwarf (BD) companions, we investigate the microlensing survey data collected during the 2016--2018 seasons. For this purpose, we first conducted modeling of lensing events with light curves exhibiting anomaly features that are likely to be produced by binary lenses. We then sorted out BD-companion binary-lens events by applying the criterion that the companion-to-primary mass ratio is $q \lesssim 0.1$. From this procedure, we identify 6 binaries with candidate BD companions, including OGLE-2016-BLG-0890L, MOA-2017-BLG-477L, OGLE-2017-BLG-0614L, KMT-2018-BLG-0357L, OGLE-2018-BLG-1489L, and OGLE-2018-BLG-0360L. We estimate the masses of the binary companions by conducting Bayesian analyses using the observables of the individual lensing events. According to the Bayesian estimation of the lens masses, the probabilities for the lens companions of the events OGLE-2016-BLG-0890, OGLE-2017-BLG-0614, OGLE-2018-BLG-1489, and OGLE-2018-BLG-0360 to be in the BD mass regime are very high with $P_{\rm BD}> 80\%$. For MOA-2017-BLG-477 and KMT-2018-BLG-0357, the probabilities are relatively low with $P_{\rm BD}=61\%$ and 69\%, respectively. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.04607v1-abstract-full').style.display = 'none'; document.getElementById('2209.04607v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 10 figures, 10 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.03886">arXiv:2209.03886</a> <span> [<a href="https://arxiv.org/pdf/2209.03886">pdf</a>, <a href="https://arxiv.org/ps/2209.03886">ps</a>, <a href="https://arxiv.org/format/2209.03886">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/ac9d93">10.3847/1538-3881/ac9d93 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Mass Production of 2021 KMTNet Microlensing Planets III: Analysis of Three Giant Planets </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Shin%2C+I">In-Gu Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Yee%2C+J+C">Jennifer C. Yee</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">Andrew Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Hwang%2C+K">Kyu-Ha Hwang</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+H">Hongjing Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+I+A">Ian A. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Albrow%2C+M+D">Michael D. Albrow</a>, <a href="/search/astro-ph?searchtype=author&query=Chung%2C+S">Sun-Ju Chung</a>, <a href="/search/astro-ph?searchtype=author&query=Han%2C+C">Cheongho Han</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+Y+K">Youn Kil Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Ryu%2C+Y">Yoon-Hyun Ryu</a>, <a href="/search/astro-ph?searchtype=author&query=Shvartzvald%2C+Y">Yossi Shvartzvald</a>, <a href="/search/astro-ph?searchtype=author&query=Zang%2C+W">Weicheng Zang</a>, <a href="/search/astro-ph?searchtype=author&query=Cha%2C+S">Sang-Mok Cha</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Dong-Jin Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+S">Seung-Lee Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+C">Chung-Uk Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+D">Dong-Joo Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+Y">Yongseok Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Park%2C+B">Byeong-Gon Park</a>, <a href="/search/astro-ph?searchtype=author&query=Pogge%2C+R+W">Richard W. Pogge</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+F">Fumio Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Barry%2C+R">Richard Barry</a>, <a href="/search/astro-ph?searchtype=author&query=Bennett%2C+D+P">David P. Bennett</a>, <a href="/search/astro-ph?searchtype=author&query=Bhattacharya%2C+A">Aparna Bhattacharya</a> , et al. (23 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2209.03886v2-abstract-short" style="display: inline;"> We present the analysis of three more planets from the KMTNet 2021 microlensing season. KMT-2021-BLG-0119Lb is a $\sim 6\, M_{\rm Jup}$ planet orbiting an early M-dwarf or a K-dwarf, KMT-2021-BLG-0192Lb is a $\sim 2\, M_{\rm Nep}$ planet orbiting an M-dwarf, and KMT-2021-BLG-0192Lb is a $\sim 1.25\, M_{\rm Nep}$ planet orbiting a very--low-mass M dwarf or a brown dwarf. These by-eye planet detecti… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.03886v2-abstract-full').style.display = 'inline'; document.getElementById('2209.03886v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.03886v2-abstract-full" style="display: none;"> We present the analysis of three more planets from the KMTNet 2021 microlensing season. KMT-2021-BLG-0119Lb is a $\sim 6\, M_{\rm Jup}$ planet orbiting an early M-dwarf or a K-dwarf, KMT-2021-BLG-0192Lb is a $\sim 2\, M_{\rm Nep}$ planet orbiting an M-dwarf, and KMT-2021-BLG-0192Lb is a $\sim 1.25\, M_{\rm Nep}$ planet orbiting a very--low-mass M dwarf or a brown dwarf. These by-eye planet detections provide an important comparison sample to the sample selected with the AnomalyFinder algorithm, and in particular, KMT-2021-BLG-2294, is a case of a planet detected by-eye but not by-algorithm. KMT-2021-BLG-2294Lb is part of a population of microlensing planets around very-low-mass host stars that spans the full range of planet masses, in contrast to the planet population at $\lesssim 0.1\, $ au, which shows a strong preference for small planets. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.03886v2-abstract-full').style.display = 'none'; document.getElementById('2209.03886v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, 12 figures, 7 tables. Accept for publication in The Astronomical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.00112">arXiv:2209.00112</a> <span> [<a href="https://arxiv.org/pdf/2209.00112">pdf</a>, <a href="https://arxiv.org/ps/2209.00112">ps</a>, <a href="https://arxiv.org/format/2209.00112">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202244438">10.1051/0004-6361/202244438 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> KMT-2017-BLG-0673Lb and KMT-2019-BLG-0414Lb: Two microlensing planets detected in peripheral fields of KMTNet survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Han%2C+C">Cheongho Han</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+C">Chung-Uk Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">Andrew Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+Y+K">Youn Kil Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Albrow%2C+M+D">Michael D. Albrow</a>, <a href="/search/astro-ph?searchtype=author&query=Chung%2C+S">Sun-Ju Chung</a>, <a href="/search/astro-ph?searchtype=author&query=Hwang%2C+K">Kyu-Ha Hwang</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Doeon Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Ryu%2C+Y">Yoon-Hyun Ryu</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+I">In-Gu Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Shvartzvald%2C+Y">Yossi Shvartzvald</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+H">Hongjing Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Yee%2C+J+C">Jennifer C. Yee</a>, <a href="/search/astro-ph?searchtype=author&query=Zang%2C+W">Weicheng Zang</a>, <a href="/search/astro-ph?searchtype=author&query=Cha%2C+S">Sang-Mok Cha</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Dong-Jin Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+S">Seung-Lee Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+D">Dong-Joo Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+Y">Yongseok Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Park%2C+B">Byeong-Gon Park</a>, <a href="/search/astro-ph?searchtype=author&query=Pogge%2C+R+W">Richard W. Pogge</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2209.00112v1-abstract-short" style="display: inline;"> We investigate the microlensing data collected during the 2017--2019 seasons in the peripheral Galactic bulge fields with the aim of finding planetary signals in microlensing light curves observed with relatively sparse coverage. We first sort out lensing events with weak short-term anomalies in the lensing light curves from the visual inspection of all non-prime-field events, and then test variou… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.00112v1-abstract-full').style.display = 'inline'; document.getElementById('2209.00112v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.00112v1-abstract-full" style="display: none;"> We investigate the microlensing data collected during the 2017--2019 seasons in the peripheral Galactic bulge fields with the aim of finding planetary signals in microlensing light curves observed with relatively sparse coverage. We first sort out lensing events with weak short-term anomalies in the lensing light curves from the visual inspection of all non-prime-field events, and then test various interpretations of the anomalies. From this procedure, we find two previously unidentified candidate planetary lensing events KMT-2017-BLG-0673 and KMT-2019-BLG-0414. It is found that the planetary signal of KMT-2017-BLG-0673 was produced by the source crossing over a planet-induced caustic, but it was previously missed because of the sparse coverage of the signal. On the other hand, the possibly planetary signal of KMT-2019-BLG-0414 was generated without caustic crossing, and it was previously missed due to the weakness of the signal. We identify a unique planetary solution for KMT-2017-BLG-0673. However, for KMT-2019-BLG-0414, we identify two pairs of planetary solutions, for each of which there are two solutions caused by the close-wide degeneracy, and a slightly less favored binary-source solution, in which a single lens mass gravitationally magnified a rapidly orbiting binary source with a faint companion (xallarap). From Bayesian analyses, it is estimated that the planet KMT-2017-BLG-0673Lb has a mass of $3.7^{+2.2}_{-2.1}~M_{\rm J}$, and it is orbiting a late K-type host star with a mass of $0.63^{+0.37}_{-0.35}~M_\odot$. Under the planetary interpretation of KMT-2010-BLG-0414L, a star with a mass of $0.74^{+0.43}_{-0.38}~M_\odot$ hosts a planet with a mass of $\sim 3.2$--3.6~$M_{\rm J}$ depending on the solution. We discuss the possible resolution of the planet-xallarap degeneracy of KMT-2019-BLG-0414 by future adaptive-optics observations on 30~m class telescopes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.00112v1-abstract-full').style.display = 'none'; document.getElementById('2209.00112v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 31 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 pages, 7 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2208.04230">arXiv:2208.04230</a> <span> [<a href="https://arxiv.org/pdf/2208.04230">pdf</a>, <a href="https://arxiv.org/ps/2208.04230">ps</a>, <a href="https://arxiv.org/format/2208.04230">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.5303/JKAS.2022.55.4.123">10.5303/JKAS.2022.55.4.123 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> OGLE-2019-BLG-0362Lb: A super-Jovian-mass planet around a low-mass star </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Chung%2C+S">Sun-Ju Chung</a>, <a href="/search/astro-ph?searchtype=author&query=Yee%2C+J+C">Jennifer C. Yee</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">Andrej Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">Andrew Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Albrow%2C+M+D">Michael D. Albrow</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+Y+K">Youn Kil Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Hwang%2C+K">Kyu-Ha Hwang</a>, <a href="/search/astro-ph?searchtype=author&query=Han%2C+C">Cheongho Han</a>, <a href="/search/astro-ph?searchtype=author&query=Ryu%2C+Y">Yoon-Hyun Ryu</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+I">In-Gu Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Shvartzvald%2C+Y">Yossi Shvartzvald</a>, <a href="/search/astro-ph?searchtype=author&query=Zang%2C+W">Weicheng Zang</a>, <a href="/search/astro-ph?searchtype=author&query=Cha%2C+S">Sang-Mok Cha</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Dong-Jin Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+S">Seung-Lee Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+C">Chung-Uk Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+D">Dong-Joo Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+Y">Yongseok Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Park%2C+B">Byeong-Gon Park</a>, <a href="/search/astro-ph?searchtype=author&query=Pogge%2C+R+W">Richard W. Pogge</a>, <a href="/search/astro-ph?searchtype=author&query=Poleski%2C+R">Radek Poleski</a>, <a href="/search/astro-ph?searchtype=author&query=Pietrukowicz%2C+P+M+P">Przemek Mr贸z Pawe艂 Pietrukowicz</a>, <a href="/search/astro-ph?searchtype=author&query=Skowron%2C+J">Jan Skowron</a>, <a href="/search/astro-ph?searchtype=author&query=Szyma%C5%84ski%2C+M+K">Micha艂 K. Szyma艅ski</a>, <a href="/search/astro-ph?searchtype=author&query=Soszy%C5%84ski%2C+I">Igor Soszy艅ski</a> , et al. (6 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2208.04230v1-abstract-short" style="display: inline;"> We present the analysis of a planetary microlensing event OGLE-2019-BLG-0362 with a short-duration anomaly $(\sim 0.4\, \rm days)$ near the peak of the light curve, which is caused by the resonant caustic. The event has a severe degeneracy with $螖蠂^2 = 0.9$ between the close and the wide binary lens models both with planet-host mass ratio $q \simeq 0.007$. We measure the angular Einstein radius bu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.04230v1-abstract-full').style.display = 'inline'; document.getElementById('2208.04230v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2208.04230v1-abstract-full" style="display: none;"> We present the analysis of a planetary microlensing event OGLE-2019-BLG-0362 with a short-duration anomaly $(\sim 0.4\, \rm days)$ near the peak of the light curve, which is caused by the resonant caustic. The event has a severe degeneracy with $螖蠂^2 = 0.9$ between the close and the wide binary lens models both with planet-host mass ratio $q \simeq 0.007$. We measure the angular Einstein radius but not the microlens parallax, and thus we perform a Bayesian analysis to estimate the physical parameters of the lens. We find that the OGLE-2019-BLG-0362L system is a super-Jovian-mass planet $M_{\rm p}=3.26^{+0.83}_{-0.58}\, M_{\rm J}$ orbiting an M dwarf $M_{\rm h}=0.42^{+0.34}_{-0.23}\, M_\odot$ at a distance $D_{\rm L} =5.83^{+1.04}_{-1.55}\, \rm kpc$. The projected star-planet separation is $a_{\perp} = 2.18^{+0.58}_{-0.72}\, \rm AU$, which indicates that the planet lies beyond the snow line of the host star. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.04230v1-abstract-full').style.display = 'none'; document.getElementById('2208.04230v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 5 figures, Accepted in JKAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2207.07295">arXiv:2207.07295</a> <span> [<a href="https://arxiv.org/pdf/2207.07295">pdf</a>, <a href="https://arxiv.org/ps/2207.07295">ps</a>, <a href="https://arxiv.org/format/2207.07295">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/acab6b">10.3847/1538-3881/acab6b <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Mass Production of 2021 KMTNet Microlensing Planets II </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ryu%2C+Y">Yoon-Hyun Ryu</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+I">In-Gu Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+H">Hongjing Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">Andrew Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Albrow%2C+M+D">Michael D. Albrow</a>, <a href="/search/astro-ph?searchtype=author&query=Chung%2C+S">Sun-Ju Chung</a>, <a href="/search/astro-ph?searchtype=author&query=Han%2C+C">Cheongho Han</a>, <a href="/search/astro-ph?searchtype=author&query=Hwang%2C+K">Kyu-Ha Hwang</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+Y+K">Youn Kil Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Shvartzvald%2C+Y">Yossi Shvartzvald</a>, <a href="/search/astro-ph?searchtype=author&query=Yee%2C+J+C">Jennifer C. Yee</a>, <a href="/search/astro-ph?searchtype=author&query=Zang%2C+W">Weicheng Zang</a>, <a href="/search/astro-ph?searchtype=author&query=Cha%2C+S">Sang-Mok Cha</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Dong-Jin Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+%25">%Hyoun-Woo Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+S">Seung-Lee Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+C">Chung-Uk Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+D">Dong-Joo Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+Y">Yongseok Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Park%2C+B">Byeong-Gon Park</a>, <a href="/search/astro-ph?searchtype=author&query=Pogge%2C+R+W">Richard W. Pogge</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2207.07295v1-abstract-short" style="display: inline;"> We continue our program of publishing all planets (and possible planets) found by eye in 2021 Korea Microlensing Telescope Network (KMTNet) online data. We present 4 planets, (KMT-2021-BLG-0712Lb, KMT-2021-BLG-0909Lb, KMT-2021-BLG-2478Lb, and KMT-2021-BLG-1105Lb), with planet-host mass ratios in the range -3.3 < log q < -2.2. This brings the total of secure, by-eye, 2021 KMTNet planets to 16, incl… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.07295v1-abstract-full').style.display = 'inline'; document.getElementById('2207.07295v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2207.07295v1-abstract-full" style="display: none;"> We continue our program of publishing all planets (and possible planets) found by eye in 2021 Korea Microlensing Telescope Network (KMTNet) online data. We present 4 planets, (KMT-2021-BLG-0712Lb, KMT-2021-BLG-0909Lb, KMT-2021-BLG-2478Lb, and KMT-2021-BLG-1105Lb), with planet-host mass ratios in the range -3.3 < log q < -2.2. This brings the total of secure, by-eye, 2021 KMTNet planets to 16, including 8 in this series. The by-eye sample is an important check of the completeness of semi-automated detections, which are the basis for statistical analyses. One of the planets, KMT-2021-BLG-1105Lb, is blended with a relatively bright $(I,V)\sim (18.9,21.6)$ star that may be the host. This could be verified immediately by high-resolution imaging. If so, the host is an early G dwarf, and the planet could be characterized by radial-velocity observations on 30m class telescopes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.07295v1-abstract-full').style.display = 'none'; document.getElementById('2207.07295v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2022. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2206.11409">arXiv:2206.11409</a> <span> [<a href="https://arxiv.org/pdf/2206.11409">pdf</a>, <a href="https://arxiv.org/ps/2206.11409">ps</a>, <a href="https://arxiv.org/format/2206.11409">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/ac9c5c">10.3847/1538-3881/ac9c5c <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Systematic KMTNet Planetary Anomaly Search. VI. Complete Sample of 2018 Sub-Prime-Field Planets </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Jung%2C+Y+K">Youn Kil Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Zang%2C+W">Weicheng Zang</a>, <a href="/search/astro-ph?searchtype=author&query=Han%2C+C">Cheongho Han</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">Andrew Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">Andrzej Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Albrow%2C+M+D">Michael D. Albrow</a>, <a href="/search/astro-ph?searchtype=author&query=Chung%2C+S">Sun-Ju Chung</a>, <a href="/search/astro-ph?searchtype=author&query=Hwang%2C+K">Kyu-Ha Hwang</a>, <a href="/search/astro-ph?searchtype=author&query=Ryu%2C+Y">Yoon-Hyun Ryu</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+I">In-Gu Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Shvartzvald%2C+Y">Yossi Shvartzvald</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+H">Hongjing Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Yee%2C+J+C">Jennifer C. Yee</a>, <a href="/search/astro-ph?searchtype=author&query=Cha%2C+S">Sang-Mok Cha</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Dong-Jin Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+S">Seung-Lee Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+C">Chung-Uk Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+D">Dong-Joo Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+Y">Yongseok Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Park%2C+B">Byeong-Gon Park</a>, <a href="/search/astro-ph?searchtype=author&query=Pogge%2C+R+W">Richard W. Pogge</a>, <a href="/search/astro-ph?searchtype=author&query=Mr%C3%B3z%2C+P">Przemek Mr贸z</a>, <a href="/search/astro-ph?searchtype=author&query=Szyma%C5%84ski%2C+M+K">Micha艂 K. Szyma艅ski</a>, <a href="/search/astro-ph?searchtype=author&query=Skowron%2C+J">Jan Skowron</a>, <a href="/search/astro-ph?searchtype=author&query=Poleski%2C+R">Radek Poleski</a> , et al. (7 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2206.11409v1-abstract-short" style="display: inline;"> We complete the analysis of all 2018 sub-prime-field microlensing planets identified by the KMTNet AnomalyFinder. Among the 9 previously unpublished events with clear planetary solutions, 6 are clearly planetary (KMT-2018-BLG-0030, KMT-2018-BLG-0087, KMT-2018-BLG-0247, OGLE-2018-BLG-0298, KMT-2018-BLG-2602, and OGLE-2018-BLG-1119), while the remaining 3 are ambiguous in nature. In addition, there… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.11409v1-abstract-full').style.display = 'inline'; document.getElementById('2206.11409v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.11409v1-abstract-full" style="display: none;"> We complete the analysis of all 2018 sub-prime-field microlensing planets identified by the KMTNet AnomalyFinder. Among the 9 previously unpublished events with clear planetary solutions, 6 are clearly planetary (KMT-2018-BLG-0030, KMT-2018-BLG-0087, KMT-2018-BLG-0247, OGLE-2018-BLG-0298, KMT-2018-BLG-2602, and OGLE-2018-BLG-1119), while the remaining 3 are ambiguous in nature. In addition, there are 8 previously published sub-prime field planets that were selected by the AnomalyFinder algorithm. Together with a companion paper (Gould et al. 2022) on 2018 prime-field planets, this work lays the basis for the first statistical analysis of the planet mass-ratio function based on planets identified in KMTNet data. As expected (Zhu et al. 2014), half (17/33) of the 2018 planets likely to enter the mass-ratio analysis have non-caustic-crossing anomalies. However, only 1 of the 5 non-caustic anomalies with planet-host mass ratio $q<10^{-3}$ was discovered by eye (compared to 7 of the 12 with $q>10^{-3}$), showing the importance of the semi-automated AnomalyFinder search. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.11409v1-abstract-full').style.display = 'none'; document.getElementById('2206.11409v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">56 pages, 13 tables, 14 figures, submitted to AAS Journals</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2205.12584">arXiv:2205.12584</a> <span> [<a href="https://arxiv.org/pdf/2205.12584">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stac2023">10.1093/mnras/stac2023 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> KMT-2021-BLG-0171Lb and KMT-2021-BLG-1689Lb: Two Microlensing Planets in the KMTNet High-cadence Fields with Followup Observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Yang%2C+H">Hongjing Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Zang%2C+W">Weicheng Zang</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">Andrew Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Yee%2C+J+C">Jennifer C. Yee</a>, <a href="/search/astro-ph?searchtype=author&query=Hwang%2C+K">Kyu-Ha Hwang</a>, <a href="/search/astro-ph?searchtype=author&query=Christie%2C+G">Grant Christie</a>, <a href="/search/astro-ph?searchtype=author&query=Sumi%2C+T">Takahiro Sumi</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+J">Jiyuan Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Mao%2C+S">Shude Mao</a>, <a href="/search/astro-ph?searchtype=author&query=Albrow%2C+M+D">Michael D. Albrow</a>, <a href="/search/astro-ph?searchtype=author&query=Chung%2C+S">Sun-Ju Chung</a>, <a href="/search/astro-ph?searchtype=author&query=Han%2C+C">Cheongho Han</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+Y+K">Youn Kil Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Ryu%2C+Y">Yoon-Hyun Ryu</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+I">In-Gu Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Shvartzvald%2C+Y">Yossi Shvartzvald</a>, <a href="/search/astro-ph?searchtype=author&query=Cha%2C+S">Sang-Mok Cha</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Dong-Jin Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+H">Hyoun-Woo Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+S">Seung-Lee Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+C">Chung-Uk Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+D">Dong-Joo Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+Y">Yongseok Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Park%2C+B">Byeong-Gon Park</a>, <a href="/search/astro-ph?searchtype=author&query=Pogge%2C+R+W">Richard W. Pogge</a> , et al. (34 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2205.12584v1-abstract-short" style="display: inline;"> Follow-up observations of high-magnification gravitational microlensing events can fully exploit their intrinsic sensitivity to detect extrasolar planets, especially those with small mass ratios. To make followup more uniform and efficient, we develop a system, HighMagFinder, based on the real-time data from the Korean Microlensing Telescope Network (KMTNet) to automatically alert possible ongoing… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.12584v1-abstract-full').style.display = 'inline'; document.getElementById('2205.12584v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2205.12584v1-abstract-full" style="display: none;"> Follow-up observations of high-magnification gravitational microlensing events can fully exploit their intrinsic sensitivity to detect extrasolar planets, especially those with small mass ratios. To make followup more uniform and efficient, we develop a system, HighMagFinder, based on the real-time data from the Korean Microlensing Telescope Network (KMTNet) to automatically alert possible ongoing high-magnification events. We started a new phase of follow-up observations with the help of HighMagFinder in 2021. Here we report the discovery of two planets in high-magnification microlensing events, KMT-2021-BLG-0171 and KMT-2021-BLG-1689, which were identified by the HighMagFinder. We find that both events suffer the ``central-resonant'' caustic degeneracy. The planet-host mass-ratio is $q\sim4.7\times10^{-5}$ or $q\sim 2.2\times10^{-5}$ for KMT-2021-BLG-0171, and $q\sim2.5\times10^{-4}$ or $q\sim 1.8\times10^{-4}$ for KMT-2021-BLG-1689. Together with two events reported by Ryu et al. (2022), four cases that suffer such degeneracy have been discovered in the 2021 season alone, indicating that the degenerate solutions may have been missed in some previous studies. We also propose a new factor for weighting the probability of each solution from the phase-space. The resonant interpretations for the two events are disfavored under this consideration. This factor can be included in future statistical studies to weight degenerate solutions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.12584v1-abstract-full').style.display = 'none'; document.getElementById('2205.12584v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 15 figures, 10 tabels; submitted to MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2205.10510">arXiv:2205.10510</a> <span> [<a href="https://arxiv.org/pdf/2205.10510">pdf</a>, <a href="https://arxiv.org/ps/2205.10510">ps</a>, <a href="https://arxiv.org/format/2205.10510">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202243484">10.1051/0004-6361/202243484 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Four sub-Jovian-mass planets detected by high-cadence microlensing surveys </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Han%2C+C">Cheongho Han</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Doeon Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">Andrew Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">Andrzej Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+I+A">Ian A. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Bozza%2C+V">Valerio Bozza</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+Y+K">Youn Kil Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Albrow%2C+M+D">Michael D. Albrow</a>, <a href="/search/astro-ph?searchtype=author&query=Chung%2C+S">Sun-Ju Chung</a>, <a href="/search/astro-ph?searchtype=author&query=Hwang%2C+K">Kyu-Ha Hwang</a>, <a href="/search/astro-ph?searchtype=author&query=Ryu%2C+Y">Yoon-Hyun Ryu</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+I">In-Gu Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Shvartzvald%2C+Y">Yossi Shvartzvald</a>, <a href="/search/astro-ph?searchtype=author&query=Yee%2C+J+C">Jennifer C. Yee</a>, <a href="/search/astro-ph?searchtype=author&query=Zang%2C+W">Weicheng Zang</a>, <a href="/search/astro-ph?searchtype=author&query=Cha%2C+S">Sang-Mok Cha</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Dong-Jin Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+S">Seung-Lee Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+C">Chung-Uk Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+D">Dong-Joo Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+Y">Yongseok Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Park%2C+B">Byeong-Gon Park</a>, <a href="/search/astro-ph?searchtype=author&query=Pogge%2C+R+W">Richard W. Pogge</a>, <a href="/search/astro-ph?searchtype=author&query=Mr%C3%B3z%2C+P">Przemek Mr贸z</a>, <a href="/search/astro-ph?searchtype=author&query=Szyma%C5%84ski%2C+M+K">Micha艂 K. Szyma艅ski</a> , et al. (35 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2205.10510v1-abstract-short" style="display: inline;"> With the aim of finding short-term planetary signals, we investigated the data collected from the high-cadence microlensing surveys. From this investigation, we found four planetary systems with low planet-to-host mass ratios, including OGLE-2017-BLG-1691L, KMT-2021-BLG-0320L, KMT-2021-BLG-1303L, and KMT-2021-BLG-1554L. Despite the short durations, ranging from a few hours to a couple of days, the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.10510v1-abstract-full').style.display = 'inline'; document.getElementById('2205.10510v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2205.10510v1-abstract-full" style="display: none;"> With the aim of finding short-term planetary signals, we investigated the data collected from the high-cadence microlensing surveys. From this investigation, we found four planetary systems with low planet-to-host mass ratios, including OGLE-2017-BLG-1691L, KMT-2021-BLG-0320L, KMT-2021-BLG-1303L, and KMT-2021-BLG-1554L. Despite the short durations, ranging from a few hours to a couple of days, the planetary signals were clearly detected by the combined data of the lensing surveys. It is found that three of the planetary systems have mass ratios of the order of $10^{-4}$ and the other has a mass ratio slightly greater than $10^{-3}$. The estimated masses indicate that all discovered planets have sub-Jovian masses. The planet masses of KMT-2021-BLG-0320Lb, KMT-2021-BLG-1303Lb, and KMT-2021-BLG-1554Lb correspond to $\sim 0.10$, $\sim 0.38$, and $\sim 0.12$ times of the mass of the Jupiter, and the mass of OGLE-2017-BLG-1691Lb corresponds to that of the Uranus. The estimated mass of the planet host KMT-2021-BLG-1554L, $M_{\rm host}\sim 0.08~M_\odot$, corresponds to the boundary between a star and a brown dwarf. Besides this system, the host stars of the other planetary systems are low-mass stars with masses in the range of $\sim [0.3$--$0.6]~M_\odot$. The discoveries of the planets well demonstrate the capability of the current high-cadence microlensing surveys in detecting low-mass planets. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.10510v1-abstract-full').style.display = 'none'; document.getElementById('2205.10510v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 12 figures, 9 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2205.07522">arXiv:2205.07522</a> <span> [<a href="https://arxiv.org/pdf/2205.07522">pdf</a>, <a href="https://arxiv.org/format/2205.07522">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/ac78ed">10.3847/1538-3881/ac78ed <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> MOA-2019-BLG-008Lb: a new microlensing detection of an object at the planet/brown dwarf boundary </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bachelet%2C+E">E. Bachelet</a>, <a href="/search/astro-ph?searchtype=author&query=Tsapras%2C+Y">Y. Tsapras</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">Andrew Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Street%2C+R+A">R. A. Street</a>, <a href="/search/astro-ph?searchtype=author&query=Bennett%2C+D+P">David P. Bennett</a>, <a href="/search/astro-ph?searchtype=author&query=Hundertmark%2C+M+P+G">M. P. G. Hundertmark</a>, <a href="/search/astro-ph?searchtype=author&query=Bozza%2C+V">V. Bozza</a>, <a href="/search/astro-ph?searchtype=author&query=Bramich%2C+D+M">D. M. Bramich</a>, <a href="/search/astro-ph?searchtype=author&query=Cassan%2C+A">A. Cassan</a>, <a href="/search/astro-ph?searchtype=author&query=Dominik%2C+M">M. Dominik</a>, <a href="/search/astro-ph?searchtype=author&query=Horne%2C+K">K. Horne</a>, <a href="/search/astro-ph?searchtype=author&query=Mao%2C+S">S. Mao</a>, <a href="/search/astro-ph?searchtype=author&query=Saha%2C+A">A. Saha</a>, <a href="/search/astro-ph?searchtype=author&query=Wambsganss%2C+J">J. Wambsganss</a>, <a href="/search/astro-ph?searchtype=author&query=Zang%2C+W">Weicheng Zang</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+F">Fumio Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Barry%2C+R">Richard Barry</a>, <a href="/search/astro-ph?searchtype=author&query=Bhattacharya%2C+A">Aparna Bhattacharya</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+I+A">Ian A. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Fukui%2C+A">Akihiko Fukui</a>, <a href="/search/astro-ph?searchtype=author&query=Fujii%2C+H">Hirosane Fujii</a>, <a href="/search/astro-ph?searchtype=author&query=Hirao%2C+Y">Yuki Hirao</a>, <a href="/search/astro-ph?searchtype=author&query=Itow%2C+Y">Yoshitaka Itow</a>, <a href="/search/astro-ph?searchtype=author&query=Kirikawa%2C+R">Rintaro Kirikawa</a>, <a href="/search/astro-ph?searchtype=author&query=Koshimoto%2C+N">Naoki Koshimoto</a> , et al. (46 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2205.07522v1-abstract-short" style="display: inline;"> We report on the observations, analysis and interpretation of the microlensing event MOA-2019- BLG-008. The observed anomaly in the photometric light curve is best described through a binary lens model. In this model, the source did not cross caustics and no finite source effects were observed. Therefore the angular Einstein ring radius cannot be measured from the light curve alone. However, the l… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.07522v1-abstract-full').style.display = 'inline'; document.getElementById('2205.07522v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2205.07522v1-abstract-full" style="display: none;"> We report on the observations, analysis and interpretation of the microlensing event MOA-2019- BLG-008. The observed anomaly in the photometric light curve is best described through a binary lens model. In this model, the source did not cross caustics and no finite source effects were observed. Therefore the angular Einstein ring radius cannot be measured from the light curve alone. However, the large event duration, t E about 80 days, allows a precise measurement of the microlensing parallax. In addition to the constraints on the angular radius and the apparent brightness I s of the source, we employ the Besancon and GalMod galactic models to estimate the physical properties of the lens. We find excellent agreement between the predictions of the two Galactic models: the companion is likely a resident of the brown dwarf desert with a mass Mp about 30 MJup and the host is a main sequence dwarf star. The lens lies along the line of sight to the Galactic Bulge, at a distance of less then4 kpc. We estimate that in about 10 years, the lens and source will be separated by 55 mas, and it will be possible to confirm the exact nature of the lensing system by using high-resolution imaging from ground or space-based observatories. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.07522v1-abstract-full').style.display = 'none'; document.getElementById('2205.07522v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted in AJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2204.11383">arXiv:2204.11383</a> <span> [<a href="https://arxiv.org/pdf/2204.11383">pdf</a>, <a href="https://arxiv.org/ps/2204.11383">ps</a>, <a href="https://arxiv.org/format/2204.11383">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202243161">10.1051/0004-6361/202243161 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> KMT-2021-BLG-0240: Microlensing event with a deformed planetary signal </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Han%2C+C">Cheongho Han</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Doeon Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+H">Hongjing Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">Andrew Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+Y+K">Youn Kil Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Albrow%2C+M+D">Michael D. Albrow</a>, <a href="/search/astro-ph?searchtype=author&query=Chung%2C+S">Sun-Ju Chung</a>, <a href="/search/astro-ph?searchtype=author&query=Hwang%2C+K">Kyu-Ha Hwang</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+C">Chung-Uk Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Ryu%2C+Y">Yoon-Hyun Ryu</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+I">In-Gu Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Shvartzvald%2C+Y">Yossi Shvartzvald</a>, <a href="/search/astro-ph?searchtype=author&query=Yee%2C+J+C">Jennifer C. Yee</a>, <a href="/search/astro-ph?searchtype=author&query=Zang%2C+W">Weicheng Zang</a>, <a href="/search/astro-ph?searchtype=author&query=Cha%2C+S">Sang-Mok Cha</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Dong-Jin Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+S">Seung-Lee Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+D">Dong-Joo Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+Y">Yongseok Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Park%2C+B">Byeong-Gon Park</a>, <a href="/search/astro-ph?searchtype=author&query=Pogge%2C+R+W">Richard W. Pogge</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2204.11383v1-abstract-short" style="display: inline;"> The light curve of the microlensing event KMT-2021-BLG-0240 exhibits a short-lasting anomaly with complex features near the peak at the 0.1~mag level from a single-lens single-source model. We conducted modeling of the lensing light curve under various interpretations to reveal the nature of the anomaly. It is found that the anomaly cannot be explained with the usual model based on a binary-lens (… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.11383v1-abstract-full').style.display = 'inline'; document.getElementById('2204.11383v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.11383v1-abstract-full" style="display: none;"> The light curve of the microlensing event KMT-2021-BLG-0240 exhibits a short-lasting anomaly with complex features near the peak at the 0.1~mag level from a single-lens single-source model. We conducted modeling of the lensing light curve under various interpretations to reveal the nature of the anomaly. It is found that the anomaly cannot be explained with the usual model based on a binary-lens (2L1S) or a binary-source (1L2S) interpretation. However, a 2L1S model with a planet companion can describe part of the anomaly, suggesting that the anomaly may be deformed by a tertiary lens component or a close companion to the source. From the additional modeling, we find that all the features of the anomaly can be explained with either a triple-lens (3L1S) model or a binary-lens binary-source (2L2S) model obtained under the 3L1S interpretation. However, it is difficult to validate the 2L2S model because the light curve does not exhibit signatures induced by the source orbital motion and the ellipsoidal variations expected by the close separation between the source stars according to the model. We, therefore, conclude that the two interpretations cannot be distinguished with the available data, and either can be correct. According to the 3L1S solution, the lens is a planetary system with two sub-Jovian-mass planets in which the planets have masses of 0.32--0.47~$M_{\rm J}$ and 0.44--0.93~$M_{\rm J}$, and they orbit an M dwarf host. According to the 2L2S solution, on the other hand, the lens is a single planet system with a mass of $\sim 0.21~M_{\rm J}$ orbiting a late K-dwarf host, and the source is a binary composed of a primary of a subgiant or a turnoff star and a secondary of a late G dwarf. The distance to the planetary system varies depending on the solution: $\sim 7.0$~kpc according to the 3L1S solution and $\sim 6.6$~kpc according to the 2L2S solution. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.11383v1-abstract-full').style.display = 'none'; document.getElementById('2204.11383v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 8 figures, 3 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2204.11378">arXiv:2204.11378</a> <span> [<a href="https://arxiv.org/pdf/2204.11378">pdf</a>, <a href="https://arxiv.org/ps/2204.11378">ps</a>, <a href="https://arxiv.org/format/2204.11378">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202243102">10.1051/0004-6361/202243102 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> KMT-2021-BLG-1898: Planetary microlensing event involved with binary source stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Han%2C+C">Cheongho Han</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">Andrew Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Doeon Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+Y+K">Youn Kil Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Albrow%2C+M+D">Michael D. Albrow</a>, <a href="/search/astro-ph?searchtype=author&query=Chung%2C+S">Sun-Ju Chung</a>, <a href="/search/astro-ph?searchtype=author&query=Hwang%2C+K">Kyu-Ha Hwang</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+C">Chung-Uk Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Ryu%2C+Y">Yoon-Hyun Ryu</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+I">In-Gu Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Shvartzvald%2C+Y">Yossi Shvartzvald</a>, <a href="/search/astro-ph?searchtype=author&query=Yee%2C+J+C">Jennifer C. Yee</a>, <a href="/search/astro-ph?searchtype=author&query=Zang%2C+W">Weicheng Zang</a>, <a href="/search/astro-ph?searchtype=author&query=Cha%2C+S">Sang-Mok Cha</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Dong-Jin Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+S">Seung-Lee Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+D">Dong-Joo Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+Y">Yongseok Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Park%2C+B">Byeong-Gon Park</a>, <a href="/search/astro-ph?searchtype=author&query=Pogge%2C+R+W">Richard W. Pogge</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2204.11378v1-abstract-short" style="display: inline;"> The light curve of the microlensing event KMT-2021-BLG-1898 exhibits a short-term central anomaly with double-bump features that cannot be explained by the usual binary-lens or binary-source interpretations. With the aim of interpreting the anomaly, we analyze the lensing light curve under various sophisticated models. We find that the anomaly is explained by a model, in which both the lens and so… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.11378v1-abstract-full').style.display = 'inline'; document.getElementById('2204.11378v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.11378v1-abstract-full" style="display: none;"> The light curve of the microlensing event KMT-2021-BLG-1898 exhibits a short-term central anomaly with double-bump features that cannot be explained by the usual binary-lens or binary-source interpretations. With the aim of interpreting the anomaly, we analyze the lensing light curve under various sophisticated models. We find that the anomaly is explained by a model, in which both the lens and source are binaries (2L2S model). For this interpretation, the lens is a planetary system with a planet/host mass ratio of $q\sim 1.5\times 10^{-3}$, and the source is a binary composed of a turn off or a subgiant star and a mid K dwarf. The double-bump feature of the anomaly can also be depicted by a triple-lens model (3L1S model), in which the lens is a planetary system containing two planets. Among the two interpretations, the 2L2S model is favored over the 3L1S model not only because it yields a better fit to the data, by $螖蠂^2=[14.3$--18.5], but also the Einstein radii derived independently from the two stars of the binary source result in consistent values. According to the 2L2S interpretation, KMT-2021-BLG-1898 is the third planetary lensing event occurring on a binary stellar system, following MOA-2010-BLG-117 and KMT-2018-BLG-1743. Under the 2L2S interpretation, we identify two solutions resulting from the close-wide degeneracy in determining the planet-host separation. From a Bayesian analysis, we estimate that the planet has a mass of $\sim 0.7$--0.8~$M_{\rm J}$, and it orbits an early M dwarf host with a mass of $\sim 0.5~M_\odot$. The projected planet-host separation is $\sim 1.9$~AU and $\sim 3.0$~AU according to the close and wide solutions, respectively. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.11378v1-abstract-full').style.display = 'none'; document.getElementById('2204.11378v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 pages, 9 figures, 4 tables</span> </p> </li> </ol> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a 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