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<button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Iwanek%2C+P&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Iwanek%2C+P&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Iwanek%2C+P&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Iwanek%2C+P&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </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/2412.09676">arXiv:2412.09676</a> <span> [<a href="https://arxiv.org/pdf/2412.09676">pdf</a>, <a href="https://arxiv.org/format/2412.09676">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-2015-BLG-1609Lb: Sub-jovian planet orbiting a low-mass stellar or brown dwarf host </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mr%C3%B3z%2C+M+J">M. J. Mr贸z</a>, <a href="/search/astro-ph?searchtype=author&query=Poleski%2C+R">R. Poleski</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">A. Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Sumi%2C+T">T. Sumi</a>, <a href="/search/astro-ph?searchtype=author&query=Tsapras%2C+Y">Y. Tsapras</a>, <a href="/search/astro-ph?searchtype=author&query=Hundertmark%2C+M">M. Hundertmark</a>, <a href="/search/astro-ph?searchtype=author&query=Pietrukowicz%2C+P">P. Pietrukowicz</a>, <a href="/search/astro-ph?searchtype=author&query=Szyma%C5%84ski%2C+M+K">M. K. Szyma艅ski</a>, <a href="/search/astro-ph?searchtype=author&query=Skowron%2C+J">J. Skowron</a>, <a href="/search/astro-ph?searchtype=author&query=Mr%C3%B3z%2C+P">P. Mr贸z</a>, <a href="/search/astro-ph?searchtype=author&query=Gromadzki%2C+M">M. Gromadzki</a>, <a href="/search/astro-ph?searchtype=author&query=Iwanek%2C+P">P. Iwanek</a>, <a href="/search/astro-ph?searchtype=author&query=Koz%C5%82owski%2C+S">S. Koz艂owski</a>, <a href="/search/astro-ph?searchtype=author&query=Ratajczak%2C+M">M. Ratajczak</a>, <a href="/search/astro-ph?searchtype=author&query=Rybicki%2C+K+A">K. A. Rybicki</a>, <a href="/search/astro-ph?searchtype=author&query=Skowron%2C+D+M">D. M. Skowron</a>, <a href="/search/astro-ph?searchtype=author&query=Soszy%C5%84ski%2C+I">I. Soszy艅ski</a>, <a href="/search/astro-ph?searchtype=author&query=Ulaczyk%2C+K">K. Ulaczyk</a>, <a href="/search/astro-ph?searchtype=author&query=Wrona%2C+M">M. Wrona</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+F">F. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Bando%2C+K">K. Bando</a>, <a href="/search/astro-ph?searchtype=author&query=Bennett%2C+D+P">D. P. Bennett</a>, <a href="/search/astro-ph?searchtype=author&query=Bhattacharya%2C+A">A. Bhattacharya</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+I+A">I. A. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Fukui%2C+A">A. Fukui</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="2412.09676v2-abstract-short" style="display: inline;"> We present a comprehensive analysis of a planetary microlensing event OGLE-2015-BLG-1609. The planetary anomaly was detected by two survey telescopes, OGLE and MOA. Each of these surveys collected enough data over the planetary anomaly to allow for an unambiguous planet detection. Such survey detections of planetary anomalies are needed to build a robust sample of planets that could improve studie… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.09676v2-abstract-full').style.display = 'inline'; document.getElementById('2412.09676v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.09676v2-abstract-full" style="display: none;"> We present a comprehensive analysis of a planetary microlensing event OGLE-2015-BLG-1609. The planetary anomaly was detected by two survey telescopes, OGLE and MOA. Each of these surveys collected enough data over the planetary anomaly to allow for an unambiguous planet detection. Such survey detections of planetary anomalies are needed to build a robust sample of planets that could improve studies on the microlensing planetary occurrence rate by reducing biases and statistical uncertainties. In this work, we examined different methods for modeling microlensing events using individual datasets, particularly we incorporated a Galactic model prior to better constrain poorly defined microlensing parallax. Ultimately, we fitted a comprehensive model to all available data, identifying three potential typologies, with two showing comparably high Bayesian evidence. Our analysis indicates that the host of the planet is a brown dwarf with a probability of 34%, or a low-mass stellar object (M-dwarf) with the probability of 66%. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.09676v2-abstract-full').style.display = 'none'; document.getElementById('2412.09676v2-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 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 12 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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, 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/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/2410.06251">arXiv:2410.06251</a> <span> [<a href="https://arxiv.org/pdf/2410.06251">pdf</a>, <a href="https://arxiv.org/format/2410.06251">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</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="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</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/10.3847/2041-8213/ad8e68">10.3847/2041-8213/ad8e68 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Limits on planetary-mass primordial black holes from the OGLE high-cadence survey of the Magellanic Clouds </p> <p class="authors"> <span class="search-hit">Authors:</span> <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=Udalski%2C+A">Andrzej Udalski</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>, <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=Poleski%2C+R">Rados艂aw Poleski</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=Gromadzki%2C+M">Mariusz Gromadzki</a>, <a href="/search/astro-ph?searchtype=author&query=Rybicki%2C+K">Krzysztof Rybicki</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=Mr%C3%B3z%2C+M+J">Mateusz J. Mr贸z</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="2410.06251v2-abstract-short" style="display: inline;"> Observations of the Galactic bulge revealed an excess of short-timescale gravitational microlensing events that are generally attributed to a large population of free-floating or wide-orbit exoplanets. However, in recent years, some authors suggested that planetary-mass primordial black holes (PBHs) comprising a substantial fraction (1%-10%) of the dark matter in the Milky Way may be responsible f… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.06251v2-abstract-full').style.display = 'inline'; document.getElementById('2410.06251v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.06251v2-abstract-full" style="display: none;"> Observations of the Galactic bulge revealed an excess of short-timescale gravitational microlensing events that are generally attributed to a large population of free-floating or wide-orbit exoplanets. However, in recent years, some authors suggested that planetary-mass primordial black holes (PBHs) comprising a substantial fraction (1%-10%) of the dark matter in the Milky Way may be responsible for these events. If that was the case, a large number of short-timescale microlensing events should also be seen toward the Magellanic Clouds. Here, we report the results of a high-cadence survey of the Magellanic Clouds carried out from 2022 October through 2024 May as part of the Optical Gravitational Lensing Experiment. We observed almost 35 million source stars located in the central regions of the Large and Small Magellanic Clouds and found only one long-timescale microlensing event candidate. No short-timescale events were detected despite high sensitivity to such events. That allows us to infer the strongest available limits on the frequency of planetary-mass PBHs in dark matter. We find that PBHs and other compact objects with masses from $1.4 \times 10^{-8}\,M_{\odot}$ (half of the Moon mass) to $0.013\,M_{\odot}$ (planet/brown dwarf boundary) may comprise at most 1% of dark matter. That rules out the PBH origin hypothesis for the short-timescale events detected toward the Galactic bulge and indicates they are caused by the population of free-floating or wide-orbit planets. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.06251v2-abstract-full').style.display = 'none'; document.getElementById('2410.06251v2-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> 12 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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 Letters</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJL 976, 19 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.17338">arXiv:2409.17338</a> <span> [<a href="https://arxiv.org/pdf/2409.17338">pdf</a>, <a href="https://arxiv.org/format/2409.17338">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="High Energy Astrophysical Phenomena">astro-ph.HE</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/10.3847/2041-8213/ad969b">10.3847/2041-8213/ad969b <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Millinovae: A New Class of Transient Supersoft X-ray Sources without a Classical Nova Eruption </p> <p class="authors"> <span class="search-hit">Authors:</span> <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=Kr%C3%B3l%2C+K">Krzysztof Kr贸l</a>, <a href="/search/astro-ph?searchtype=author&query=Szegedi%2C+H">H茅l猫ne Szegedi</a>, <a href="/search/astro-ph?searchtype=author&query=Charles%2C+P">Philip Charles</a>, <a href="/search/astro-ph?searchtype=author&query=Page%2C+K+L">Kim L. Page</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">Andrzej Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+D+A+H">David A. H. Buckley</a>, <a href="/search/astro-ph?searchtype=author&query=Dewangan%2C+G">Gulab Dewangan</a>, <a href="/search/astro-ph?searchtype=author&query=Meintjes%2C+P">Pieter Meintjes</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>, <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=Poleski%2C+R">Rados艂aw Poleski</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=Gromadzki%2C+M">Mariusz Gromadzki</a>, <a href="/search/astro-ph?searchtype=author&query=Rybicki%2C+K">Krzysztof Rybicki</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=Mr%C3%B3z%2C+M+J">Mateusz J. Mr贸z</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="2409.17338v2-abstract-short" style="display: inline;"> Some accreting binary systems containing a white dwarf (such as classical novae or persistent supersoft sources) are seen to emit low-energy X-rays with temperatures of ~10^6 K and luminosities exceeding 10^35 erg/s. These X-rays are thought to originate from nuclear burning on the white dwarf surface, either caused by a thermonuclear runaway (classical novae) or a high mass-accretion rate that su… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.17338v2-abstract-full').style.display = 'inline'; document.getElementById('2409.17338v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.17338v2-abstract-full" style="display: none;"> Some accreting binary systems containing a white dwarf (such as classical novae or persistent supersoft sources) are seen to emit low-energy X-rays with temperatures of ~10^6 K and luminosities exceeding 10^35 erg/s. These X-rays are thought to originate from nuclear burning on the white dwarf surface, either caused by a thermonuclear runaway (classical novae) or a high mass-accretion rate that sustains steady nuclear burning (persistent sources). The discovery of transient supersoft X-rays from ASASSN-16oh challenged these ideas, as no clear signatures of mass ejection indicative of a classical nova eruption were detected, and the origin of these X-rays remains controversial. It was unclear whether this star was one of a kind or representative of a larger, as yet undiscovered, group. Here, we present the discovery of 29 stars located in the direction of the Magellanic Clouds exhibiting long-duration, symmetrical optical outbursts similar to that seen in ASASSN-16oh. We observed one of these objects during an optical outburst and found it to be emitting transient supersoft X-rays, while no signatures of mass ejection (indicative of a classical nova eruption) were detected. We therefore propose that these objects form a homogeneous group of transient supersoft X-ray sources, which we dub ``millinovae'' because their optical luminosities are approximately a thousand times fainter than those of ordinary classical novae. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.17338v2-abstract-full').style.display = 'none'; document.getElementById('2409.17338v2-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 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 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 Letters</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJL 977, 37 (2024) </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/2407.13740">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/2406.18728">arXiv:2406.18728</a> <span> [<a href="https://arxiv.org/pdf/2406.18728">pdf</a>, <a href="https://arxiv.org/ps/2406.18728">ps</a>, <a href="https://arxiv.org/format/2406.18728">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="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> The OGLE Collection of Variable Stars: Over 18 000 Rotating Variables toward the Galactic Bulge </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Iwanek%2C+P">P. Iwanek</a>, <a href="/search/astro-ph?searchtype=author&query=Soszy%C5%84ski%2C+I">I. Soszy艅ski</a>, <a href="/search/astro-ph?searchtype=author&query=St%C4%99pie%C5%84%2C+K">K. St臋pie艅</a>, <a href="/search/astro-ph?searchtype=author&query=Koz%C5%82owski%2C+S">S. Koz艂owski</a>, <a href="/search/astro-ph?searchtype=author&query=Skowron%2C+J">J. Skowron</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">A. Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Szyma%C5%84ski%2C+M+K">M. K. Szyma艅ski</a>, <a href="/search/astro-ph?searchtype=author&query=Wrona%2C+M">M. Wrona</a>, <a href="/search/astro-ph?searchtype=author&query=Pietrukowicz%2C+P">P. Pietrukowicz</a>, <a href="/search/astro-ph?searchtype=author&query=Poleski%2C+R">R. Poleski</a>, <a href="/search/astro-ph?searchtype=author&query=Mr%C3%B3z%2C+P">P. Mr贸z</a>, <a href="/search/astro-ph?searchtype=author&query=Ulaczyk%2C+K">K. Ulaczyk</a>, <a href="/search/astro-ph?searchtype=author&query=Skowron%2C+D+M">D. M. Skowron</a>, <a href="/search/astro-ph?searchtype=author&query=Gromadzki%2C+M">M. Gromadzki</a>, <a href="/search/astro-ph?searchtype=author&query=Rybicki%2C+K">K. Rybicki</a>, <a href="/search/astro-ph?searchtype=author&query=Mr%C3%B3z%2C+M+J">M. J. Mr贸z</a>, <a href="/search/astro-ph?searchtype=author&query=Ratajczak%2C+M">M. Ratajczak</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="2406.18728v1-abstract-short" style="display: inline;"> Stellar rotation, a key factor influencing stellar structure and evolution, also drives magnetic activity, which is manifested as spots or flares on stellar surface. Here, we present a collection of 18 443 rotating variables located toward the Galactic bulge, identified in the photometric database of the Optical Gravitational Lensing Experiment (OGLE) project. These stars exhibit distinct magnetic… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.18728v1-abstract-full').style.display = 'inline'; document.getElementById('2406.18728v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.18728v1-abstract-full" style="display: none;"> Stellar rotation, a key factor influencing stellar structure and evolution, also drives magnetic activity, which is manifested as spots or flares on stellar surface. Here, we present a collection of 18 443 rotating variables located toward the Galactic bulge, identified in the photometric database of the Optical Gravitational Lensing Experiment (OGLE) project. These stars exhibit distinct magnetic activity, including starspots and flares. With this collection, we provide long-term, time-series photometry in Cousins I- and Johnson V-band obtained by OGLE since 1997, and basic observational parameters, i.e., equatorial coordinates, rotation periods, mean brightness, and brightness amplitudes in both bands. This is a unique dataset for studying stellar magnetic activity, including activity cycles. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.18728v1-abstract-full').style.display = 'none'; document.getElementById('2406.18728v1-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 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">Accepted for publication in Acta Astronomica vol. 74. 24 pages, 12 figures, 4 tables. The OGLE Collection of rotating variables toward the Galactic bulge is publicly available through https://www.astrouw.edu.pl/ogle/ogle4/OCVS/blg/rot/</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/2404.17715">arXiv:2404.17715</a> <span> [<a href="https://arxiv.org/pdf/2404.17715">pdf</a>, <a href="https://arxiv.org/ps/2404.17715">ps</a>, <a href="https://arxiv.org/format/2404.17715">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> </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/10.32023/0001-5237/73.4.2">10.32023/0001-5237/73.4.2 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Blue Large-Amplitude Pulsators and Other Short-Period Variable Stars in OGLE-IV Fields of the Outer Galactic Bulge </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Borowicz%2C+J">J. Borowicz</a>, <a href="/search/astro-ph?searchtype=author&query=Pietrukowicz%2C+P">P. Pietrukowicz</a>, <a href="/search/astro-ph?searchtype=author&query=Skowron%2C+J">J. Skowron</a>, <a href="/search/astro-ph?searchtype=author&query=Soszy%C5%84ski%2C+I">I. Soszy艅ski</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">A. Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Szyma%C5%84ski%2C+M+K">M. K. Szyma艅ski</a>, <a href="/search/astro-ph?searchtype=author&query=Ulaczyk%2C+K">K. Ulaczyk</a>, <a href="/search/astro-ph?searchtype=author&query=Poleski%2C+R">R. Poleski</a>, <a href="/search/astro-ph?searchtype=author&query=Koz%C5%82owski%2C+S">S. Koz艂owski</a>, <a href="/search/astro-ph?searchtype=author&query=Mr%C3%B3z%2C+P">P. Mr贸z</a>, <a href="/search/astro-ph?searchtype=author&query=Skowron%2C+D+M">D. M. Skowron</a>, <a href="/search/astro-ph?searchtype=author&query=Rybicki%2C+K">K. Rybicki</a>, <a href="/search/astro-ph?searchtype=author&query=Iwanek%2C+P">P. Iwanek</a>, <a href="/search/astro-ph?searchtype=author&query=Wrona%2C+M">M. Wrona</a>, <a href="/search/astro-ph?searchtype=author&query=Gromadzki%2C+M">M. Gromadzki</a>, <a href="/search/astro-ph?searchtype=author&query=Mr%C3%B3z%2C+M+J">M. J. Mr贸z</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="2404.17715v2-abstract-short" style="display: inline;"> In this work, we search the OGLE-IV outer Galactic bulge fields for short-period variable objects. The investigation focuses on unexplored timescales roughly below one hour in an area containing about 700 million stellar sources down to approximately I=20 mag. We concentrate mainly on Blue Large-Amplitude Pulsators (BLAPs), which represent a recently discovered enigmatic class of short-period hot… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.17715v2-abstract-full').style.display = 'inline'; document.getElementById('2404.17715v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.17715v2-abstract-full" style="display: none;"> In this work, we search the OGLE-IV outer Galactic bulge fields for short-period variable objects. The investigation focuses on unexplored timescales roughly below one hour in an area containing about 700 million stellar sources down to approximately I=20 mag. We concentrate mainly on Blue Large-Amplitude Pulsators (BLAPs), which represent a recently discovered enigmatic class of short-period hot subluminous stars. We find 33 BLAPs in the period range from 7.5 to 66.5 min. Thirty-one of them are new discoveries, which increases the number of known stars of this class to over one hundred. Additional eighteen objects with pulsation-like light curve shapes and periods ranging from 17.3 to 53.7 min are presented. Very likely, these are $未$ Sct/SX Phe-type stars, but some of them could be pulsating hot subdwarfs or BLAPs. We also report on the detection of five eclipsing binary systems with orbital periods between 61.2 and 121.9 min and three mysterious variable objects with I-band amplitudes larger than 0.9 mag. A spectroscopic follow-up would help in the final classification of the variables. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.17715v2-abstract-full').style.display = 'none'; document.getElementById('2404.17715v2-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> 30 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 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">published in Acta Astronomica</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Acta Astronomica, Vol. 73 (2023), No. 4, pp. 265-290 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.16089">arXiv:2404.16089</a> <span> [<a href="https://arxiv.org/pdf/2404.16089">pdf</a>, <a href="https://arxiv.org/format/2404.16089">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> </div> </div> <p class="title is-5 mathjax"> Observational parameters of Blue Large-Amplitude Pulsators </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pietrukowicz%2C+P">P. Pietrukowicz</a>, <a href="/search/astro-ph?searchtype=author&query=Latour%2C+M">M. Latour</a>, <a href="/search/astro-ph?searchtype=author&query=Soszynski%2C+I">I. Soszynski</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Mille%2C+F">F. Di Mille</a>, <a href="/search/astro-ph?searchtype=author&query=King%2C+P+S">P. Soto King</a>, <a href="/search/astro-ph?searchtype=author&query=Angeloni%2C+R">R. Angeloni</a>, <a href="/search/astro-ph?searchtype=author&query=Poleski%2C+R">R. Poleski</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">A. Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Szymanski%2C+M+K">M. K. Szymanski</a>, <a href="/search/astro-ph?searchtype=author&query=Ulaczyk%2C+K">K. Ulaczyk</a>, <a href="/search/astro-ph?searchtype=author&query=Kozlowski%2C+S">S. Kozlowski</a>, <a href="/search/astro-ph?searchtype=author&query=Skowron%2C+J">J. Skowron</a>, <a href="/search/astro-ph?searchtype=author&query=Skowron%2C+D+M">D. M. Skowron</a>, <a href="/search/astro-ph?searchtype=author&query=Mroz%2C+P">P. Mroz</a>, <a href="/search/astro-ph?searchtype=author&query=Rybicki%2C+K">K. Rybicki</a>, <a href="/search/astro-ph?searchtype=author&query=Iwanek%2C+P">P. Iwanek</a>, <a href="/search/astro-ph?searchtype=author&query=Wrona%2C+M">M. Wrona</a>, <a href="/search/astro-ph?searchtype=author&query=Gromadzki%2C+M">M. Gromadzki</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="2404.16089v1-abstract-short" style="display: inline;"> Blue Large-Amplitude Pulsators (BLAPs) are a recently discovered class of short-period pulsating variable stars. In this work, we present new information on these stars based on photometric and spectroscopic data obtained for known and new objects detected by the OGLE survey. BLAPs are evolved objects with pulsation periods in the range of 3--75 min, stretching between subdwarf B-type stars and up… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.16089v1-abstract-full').style.display = 'inline'; document.getElementById('2404.16089v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.16089v1-abstract-full" style="display: none;"> Blue Large-Amplitude Pulsators (BLAPs) are a recently discovered class of short-period pulsating variable stars. In this work, we present new information on these stars based on photometric and spectroscopic data obtained for known and new objects detected by the OGLE survey. BLAPs are evolved objects with pulsation periods in the range of 3--75 min, stretching between subdwarf B-type stars and upper main-sequence stars in the Hertzsprung-Russell diagram. In general, BLAPs are single-mode stars pulsating in the fundamental radial mode. Their phase-folded light curves are typically sawtooth shaped, but light curves of shorter-period objects are more rounded and symmetric, while many longer-period objects exhibit an additional bump. The long-term OGLE observations show that the period change rates of BLAPs are usually of the order of 10^-7 per year and in a quarter of the sample are negative. An exception is the triple-mode object OGLE-BLAP-030, which changes its dominant period much faster, at a rate of about +4.6 x 10^-6 per year. The spectroscopic data indicate that the BLAPs form a homogeneous group in the period, surface gravity, and effective temperature spaces. However, we observe a split into two groups in terms of helium-to-hydrogen content. The atmospheres of the He-enriched BLAPs are more abundant in metals (about five times) than the atmosphere of the Sun. We discover that the BLAPs obey a period--gravity relationship and we use the distance to OGLE-BLAP-009 to derive a period--luminosity relation. Most of the stars observed in the OGLE Galactic bulge fields seem to reside in the bulge, while the remaining objects likely are in the foreground Galactic disk. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.16089v1-abstract-full').style.display = 'none'; document.getElementById('2404.16089v1-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, 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">submitted to ApJ, 21 pages, 14 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/2404.13031">arXiv:2404.13031</a> <span> [<a href="https://arxiv.org/pdf/2404.13031">pdf</a>, <a href="https://arxiv.org/format/2404.13031">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> <p class="title is-5 mathjax"> OGLE-2015-BLG-0845L: A low-mass M dwarf from the microlensing parallax and xallarap effects </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hu%2C+Z">Zhecheng Hu</a>, <a href="/search/astro-ph?searchtype=author&query=Zhu%2C+W">Wei Zhu</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=Sumi%2C+T">Takahiro Sumi</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+P">Ping Chen</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=Yee%2C+J+C">Jennifer C. Yee</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=Carey%2C+S">Sean Carey</a>, <a href="/search/astro-ph?searchtype=author&query=Fausnaugh%2C+M">Michael Fausnaugh</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=Henderson%2C+C+B">Calen B. Henderson</a>, <a href="/search/astro-ph?searchtype=author&query=Shvartzvald%2C+Y">Yossi Shvartzvald</a>, <a href="/search/astro-ph?searchtype=author&query=Wibking%2C+B">Benjamin Wibking</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=Poleski%2C+R">Rados艂aw Poleski</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>, <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=Ulaczyk%2C+K">Krzysztof Ulaczyk</a>, <a href="/search/astro-ph?searchtype=author&query=Rybicki%2C+K+A">Krzysztof A. Rybicki</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="2404.13031v2-abstract-short" style="display: inline;"> We present the analysis of the microlensing event OGLE-2015-BLG-0845, which was affected by both the microlensing parallax and xallarap effects. The former was detected via the simultaneous observations from the ground and Spitzer, and the latter was caused by the orbital motion of the source star in a relatively close binary. The combination of these two effects led to a mass measurement of the l… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.13031v2-abstract-full').style.display = 'inline'; document.getElementById('2404.13031v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.13031v2-abstract-full" style="display: none;"> We present the analysis of the microlensing event OGLE-2015-BLG-0845, which was affected by both the microlensing parallax and xallarap effects. The former was detected via the simultaneous observations from the ground and Spitzer, and the latter was caused by the orbital motion of the source star in a relatively close binary. The combination of these two effects led to a mass measurement of the lens object, revealing a low-mass ($0.14 \pm 0.05 M_{\odot}$) M-dwarf at the bulge distance ($7.6 \pm 1.0$ kpc). The source binary consists of a late F-type subgiant and a K-type dwarf of $\sim1.2 M_{\odot}$ and $\sim 0.9 M_{\odot}$, respectively, and the orbital period is $70 \pm 10$ days. OGLE-2015-BLG-0845 is the first single-lens event in which the lens mass is measured via the binarity of the source. Given the abundance of binary systems as potential microlensing sources, the xallarap effect may not be a rare phenomenon. Our work thus highlights the application of the xallarap effect in the mass determination of microlenses, and the same method can be used to identify isolated dark lenses. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.13031v2-abstract-full').style.display = 'none'; document.getElementById('2404.13031v2-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> 6 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 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">New version after the review process. Accepted for publication in Monthly Notices of the Royal Astronomical Society</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.05912">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/2404.00151">arXiv:2404.00151</a> <span> [<a href="https://arxiv.org/pdf/2404.00151">pdf</a>, <a href="https://arxiv.org/ps/2404.00151">ps</a>, <a href="https://arxiv.org/format/2404.00151">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="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Discovery of the Longest-Period Classical Cepheid in the Milky Way </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Soszy%C5%84ski%2C+I">I. Soszy艅ski</a>, <a href="/search/astro-ph?searchtype=author&query=Skowron%2C+D+M">D. M. Skowron</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">A. Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Pietrukowicz%2C+P">P. Pietrukowicz</a>, <a href="/search/astro-ph?searchtype=author&query=Gromadzki%2C+M">M. Gromadzki</a>, <a href="/search/astro-ph?searchtype=author&query=Szyma%C5%84ski%2C+M+K">M. K. Szyma艅ski</a>, <a href="/search/astro-ph?searchtype=author&query=Skowron%2C+J">J. Skowron</a>, <a href="/search/astro-ph?searchtype=author&query=Mr%C3%B3z%2C+P">P. Mr贸z</a>, <a href="/search/astro-ph?searchtype=author&query=Poleski%2C+R">R. Poleski</a>, <a href="/search/astro-ph?searchtype=author&query=Koz%C5%82owski%2C+S">S. Koz艂owski</a>, <a href="/search/astro-ph?searchtype=author&query=Iwanek%2C+P">P. Iwanek</a>, <a href="/search/astro-ph?searchtype=author&query=Wrona%2C+M">M. Wrona</a>, <a href="/search/astro-ph?searchtype=author&query=Ulaczyk%2C+K">K. Ulaczyk</a>, <a href="/search/astro-ph?searchtype=author&query=Rybicki%2C+K">K. Rybicki</a>, <a href="/search/astro-ph?searchtype=author&query=Mr%C3%B3z%2C+M">M. Mr贸z</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="2404.00151v1-abstract-short" style="display: inline;"> We report the discovery of the classical Cepheid OGLE-GD-CEP-1884 (= GDS_J1535467-555656) with the longest pulsation period known in our Galaxy. The period of 78.14 d is nearly 10 d longer than that of the previous record-holding Cepheid, S Vulpeculae, and thus, OGLE-GD-CEP-1884 can be categorized as the first ultra long period Cepheid in the Milky Way. This star is present in the ASAS-SN and Gaia… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.00151v1-abstract-full').style.display = 'inline'; document.getElementById('2404.00151v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.00151v1-abstract-full" style="display: none;"> We report the discovery of the classical Cepheid OGLE-GD-CEP-1884 (= GDS_J1535467-555656) with the longest pulsation period known in our Galaxy. The period of 78.14 d is nearly 10 d longer than that of the previous record-holding Cepheid, S Vulpeculae, and thus, OGLE-GD-CEP-1884 can be categorized as the first ultra long period Cepheid in the Milky Way. This star is present in the ASAS-SN and Gaia DR3 catalogs of variable stars, but it has been classified as a long-period variable in those catalogs. Based on more than 10 years of the photometric monitoring of this star carried out by the OGLE project in the I and V bands and a radial velocity curve from the Gaia Focused Product Release, we unequivocally demonstrate that this object is a fundamental-mode classical Cepheid. By employing the mid-infrared period-luminosity relation, we determine the distance to OGLE-GD-CEP-1884 (4.47 +- 0.34 kpc) and place it on the Milky Way map, along with about 2400 other classical Cepheids. We also discuss the potential of finding additional ultra long period Cepheids in our Galaxy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.00151v1-abstract-full').style.display = 'none'; document.getElementById('2404.00151v1-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, 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">9 pages, 3 figures, accepted for publication in The Astrophysical Journal Letters</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.10233">arXiv:2403.10233</a> <span> [<a href="https://arxiv.org/pdf/2403.10233">pdf</a>, <a href="https://arxiv.org/format/2403.10233">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="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Virial Black Hole Masses for AGNs behind the Magellanic Clouds </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Panda%2C+S">Swayamtrupta Panda</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=Gromadzki%2C+M">Mariusz Gromadzki</a>, <a href="/search/astro-ph?searchtype=author&query=Wrona%2C+M">Marcin Wrona</a>, <a href="/search/astro-ph?searchtype=author&query=Iwanek%2C+P">Patryk Iwanek</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">Andrzej Udalski</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>, <a href="/search/astro-ph?searchtype=author&query=Pietrukowicz%2C+P">Pawe艂 Pietrukowicz</a>, <a href="/search/astro-ph?searchtype=author&query=Ulaczyk%2C+K">Krzysztof Ulaczyk</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">Rados艂aw 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+D+M">Dorota M. Skowron</a>, <a href="/search/astro-ph?searchtype=author&query=Rybicki%2C+K">Krzysztof Rybicki</a>, <a href="/search/astro-ph?searchtype=author&query=Mr%C3%B3z%2C+M">Mateusz Mr贸z</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="2403.10233v1-abstract-short" style="display: inline;"> We use the spectroscopic data collected by the Magellanic Quasars Survey (MQS) as well as the photometric V- and I-band data from the Optical Gravitational Lensing Experiment (OGLE) to measure the physical parameters for active galactic nuclei (AGNs) located behind the Magellanic Clouds. The flux-uncalibrated MQS spectra were obtained with the 4-m Anglo-Australian Telescope and the AAOmega spectro… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.10233v1-abstract-full').style.display = 'inline'; document.getElementById('2403.10233v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.10233v1-abstract-full" style="display: none;"> We use the spectroscopic data collected by the Magellanic Quasars Survey (MQS) as well as the photometric V- and I-band data from the Optical Gravitational Lensing Experiment (OGLE) to measure the physical parameters for active galactic nuclei (AGNs) located behind the Magellanic Clouds. The flux-uncalibrated MQS spectra were obtained with the 4-m Anglo-Australian Telescope and the AAOmega spectroscope (R=1300) in a typical ~1.5-hour visit. They span a spectral range of 3700-8500 Angstroms and have S/N ratios in a range of 3-300. We report the discovery and observational properties of 161 AGNs in this footprint, which expands the total number of spectroscopically confirmed AGNs by MQS to 919. After converting the OGLE mean magnitudes to the monochromatic luminosities at 5100 Angstroms, 3000 Angstroms, and 1350 Angstroms, we reliably measured the black hole masses for 165 out of 919 AGNs. The remaining physical parameters we provide are the bolometric luminosities and the Eddington ratios. A fraction of these AGNs have been observed by the OGLE survey since 1997 (all of them since 2001), enabling studies of correlations between their variability and physical parameters. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.10233v1-abstract-full').style.display = 'none'; document.getElementById('2403.10233v1-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 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">15 pages, 8 figures, 8 tables, accepted for publication in The Astrophysical Journal Supplement Series</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.02398">arXiv:2403.02398</a> <span> [<a href="https://arxiv.org/pdf/2403.02398">pdf</a>, <a href="https://arxiv.org/format/2403.02398">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="Cosmology and Nongalactic Astrophysics">astro-ph.CO</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="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</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/10.3847/1538-4365/ad452e">10.3847/1538-4365/ad452e <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations </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=Udalski%2C+A">A. Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Szymanski%2C+M+K">M. K. Szymanski</a>, <a href="/search/astro-ph?searchtype=author&query=Kapusta%2C+M">M. Kapusta</a>, <a href="/search/astro-ph?searchtype=author&query=Soszynski%2C+I">I. Soszynski</a>, <a href="/search/astro-ph?searchtype=author&query=Wyrzykowski%2C+L">L. Wyrzykowski</a>, <a href="/search/astro-ph?searchtype=author&query=Pietrukowicz%2C+P">P. Pietrukowicz</a>, <a href="/search/astro-ph?searchtype=author&query=Kozlowski%2C+S">S. Kozlowski</a>, <a href="/search/astro-ph?searchtype=author&query=Poleski%2C+R">R. Poleski</a>, <a href="/search/astro-ph?searchtype=author&query=Skowron%2C+J">J. Skowron</a>, <a href="/search/astro-ph?searchtype=author&query=Skowron%2C+D">D. Skowron</a>, <a href="/search/astro-ph?searchtype=author&query=Ulaczyk%2C+K">K. Ulaczyk</a>, <a href="/search/astro-ph?searchtype=author&query=Gromadzki%2C+M">M. Gromadzki</a>, <a href="/search/astro-ph?searchtype=author&query=Rybicki%2C+K">K. Rybicki</a>, <a href="/search/astro-ph?searchtype=author&query=Iwanek%2C+P">P. Iwanek</a>, <a href="/search/astro-ph?searchtype=author&query=Wrona%2C+M">M. Wrona</a>, <a href="/search/astro-ph?searchtype=author&query=Ratajczak%2C+M">M. Ratajczak</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="2403.02398v2-abstract-short" style="display: inline;"> Measurements of the microlensing optical depth and event rate toward the Large Magellanic Cloud (LMC) can be used to probe the distribution and mass function of compact objects in the direction toward that galaxy - in the Milky Way disk, the Milky Way dark matter halo, and the LMC itself. The previous measurements, based on small statistical samples of events, found that the optical depth is an or… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.02398v2-abstract-full').style.display = 'inline'; document.getElementById('2403.02398v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.02398v2-abstract-full" style="display: none;"> Measurements of the microlensing optical depth and event rate toward the Large Magellanic Cloud (LMC) can be used to probe the distribution and mass function of compact objects in the direction toward that galaxy - in the Milky Way disk, the Milky Way dark matter halo, and the LMC itself. The previous measurements, based on small statistical samples of events, found that the optical depth is an order of magnitude smaller than that expected from the entire dark matter halo in the form of compact objects. However, these previous studies were not sensitive to long-duration events with Einstein timescales longer than 2.5-3 yr, which are expected from massive ($10-100\,M_{\odot}$) and intermediate-mass ($10^2-10^5\,M_{\odot}$) black holes. Such events would have been missed by the previous studies and would not have been taken into account in calculations of the optical depth. Here, we present the analysis of nearly 20-year-long photometric monitoring of 78.7 million stars in the LMC by the Optical Gravitational Lensing Experiment (OGLE) from 2001 through 2020. We describe the observing setup, the construction of the 20-year OGLE dataset, the methods used for searching for microlensing events in the light-curve data, and the calculation of the event detection efficiency. In total, we find 16 microlensing events (thirteen using an automated pipeline and three with manual searches), all of which have timescales shorter than 1 yr. We use a sample of thirteen events to measure the microlensing optical depth toward the LMC $蟿=(0.121 \pm 0.037)\times 10^{-7}$ and the event rate $螕=(0.74 \pm 0.25)\times 10^{-7}\,\mathrm{yr}^{-1}\,\mathrm{star}^{-1}$. These numbers are consistent with lensing by stars in the Milky Way disk and the LMC itself, and they demonstrate that massive and intermediate-mass black holes cannot comprise a significant fraction of the dark matter. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.02398v2-abstract-full').style.display = 'none'; document.getElementById('2403.02398v2-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 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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 ApJS</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJS 273, 4 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.02386">arXiv:2403.02386</a> <span> [<a href="https://arxiv.org/pdf/2403.02386">pdf</a>, <a href="https://arxiv.org/format/2403.02386">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="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</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/10.1038/s41586-024-07704-6">10.1038/s41586-024-07704-6 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> No massive black holes in the Milky Way halo </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=Udalski%2C+A">A. Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Szymanski%2C+M+K">M. K. Szymanski</a>, <a href="/search/astro-ph?searchtype=author&query=Soszynski%2C+I">I. Soszynski</a>, <a href="/search/astro-ph?searchtype=author&query=Wyrzykowski%2C+L">L. Wyrzykowski</a>, <a href="/search/astro-ph?searchtype=author&query=Pietrukowicz%2C+P">P. Pietrukowicz</a>, <a href="/search/astro-ph?searchtype=author&query=Kozlowski%2C+S">S. Kozlowski</a>, <a href="/search/astro-ph?searchtype=author&query=Poleski%2C+R">R. Poleski</a>, <a href="/search/astro-ph?searchtype=author&query=Skowron%2C+J">J. Skowron</a>, <a href="/search/astro-ph?searchtype=author&query=Skowron%2C+D">D. Skowron</a>, <a href="/search/astro-ph?searchtype=author&query=Ulaczyk%2C+K">K. Ulaczyk</a>, <a href="/search/astro-ph?searchtype=author&query=Gromadzki%2C+M">M. Gromadzki</a>, <a href="/search/astro-ph?searchtype=author&query=Rybicki%2C+K">K. Rybicki</a>, <a href="/search/astro-ph?searchtype=author&query=Iwanek%2C+P">P. Iwanek</a>, <a href="/search/astro-ph?searchtype=author&query=Wrona%2C+M">M. Wrona</a>, <a href="/search/astro-ph?searchtype=author&query=Ratajczak%2C+M">M. Ratajczak</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="2403.02386v3-abstract-short" style="display: inline;"> The gravitational wave detectors have unveiled a population of massive black holes that do not resemble those observed in the Milky Way and whose origin is debated. According to one possible explanation, these black holes may have formed from density fluctuations in the early Universe (primordial black holes), and they should comprise from several to 100% of dark matter to explain the observed bla… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.02386v3-abstract-full').style.display = 'inline'; document.getElementById('2403.02386v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.02386v3-abstract-full" style="display: none;"> The gravitational wave detectors have unveiled a population of massive black holes that do not resemble those observed in the Milky Way and whose origin is debated. According to one possible explanation, these black holes may have formed from density fluctuations in the early Universe (primordial black holes), and they should comprise from several to 100% of dark matter to explain the observed black hole merger rates. If such black holes existed in the Milky Way dark matter halo, they would cause long-timescale gravitational microlensing events lasting years. The previous experiments were not sufficiently sensitive to such events. Here we present the results of the search for long-timescale microlensing events among the light curves of nearly 80 million stars located in the Large Magellanic Cloud that were monitored for 20 years by the OGLE survey. We did not find any events with timescales longer than one year, whereas all shorter events detected may be explained by known stellar populations. We find that compact objects in the mass range from $1.8 \times 10^{-4}$ to $6.3\,M_{\odot}$ cannot compose more than 1% of dark matter, and those in the mass range from $1.3 \times 10^{-5}$ to $860\,M_{\odot}$ cannot make up more than 10% of dark matter. Thus, primordial black holes in this mass range cannot simultaneously explain a significant fraction of dark matter and gravitational wave events. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.02386v3-abstract-full').style.display = 'none'; document.getElementById('2403.02386v3-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 4 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">Published in Nature. This version of the article has been accepted for publication, after peer review but is not the Version of Record and does not reflect post-acceptance improvements, or any corrections. The Version of Record is available online at https://doi.org/10.1038/s41586-024-07704-6</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nature 632, 749 (2024) </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/2401.13759">arXiv:2401.13759</a> <span> [<a href="https://arxiv.org/pdf/2401.13759">pdf</a>, <a href="https://arxiv.org/format/2401.13759">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> </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/10.1051/0004-6361/202449322">10.1051/0004-6361/202449322 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Dark lens candidates from Gaia Data Release 3 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kruszy%C5%84ska%2C+K">K. Kruszy艅ska</a>, <a href="/search/astro-ph?searchtype=author&query=Wyrzykowski%2C+%C5%81">艁. Wyrzykowski</a>, <a href="/search/astro-ph?searchtype=author&query=Rybicki%2C+K+A">K. A. Rybicki</a>, <a href="/search/astro-ph?searchtype=author&query=Howil%2C+K">K. Howil</a>, <a href="/search/astro-ph?searchtype=author&query=Jab%C5%82o%C5%84ska%2C+M">M. Jab艂o艅ska</a>, <a href="/search/astro-ph?searchtype=author&query=Kaczmarek%2C+Z">Z. Kaczmarek</a>, <a href="/search/astro-ph?searchtype=author&query=Ihanec%2C+N">N. Ihanec</a>, <a href="/search/astro-ph?searchtype=author&query=Maskoli%C5%ABnas%2C+M">M. Maskoli奴nas</a>, <a href="/search/astro-ph?searchtype=author&query=Bronikowski%2C+M">M. Bronikowski</a>, <a href="/search/astro-ph?searchtype=author&query=Pylypenko%2C+U">U. Pylypenko</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">A. Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Mr%C3%B3z%2C+P">P. Mr贸z</a>, <a href="/search/astro-ph?searchtype=author&query=Poleski%2C+R">R. Poleski</a>, <a href="/search/astro-ph?searchtype=author&query=Skowron%2C+J">J. Skowron</a>, <a href="/search/astro-ph?searchtype=author&query=Szyma%C5%84ski%2C+M+K">M. K. Szyma艅ski</a>, <a href="/search/astro-ph?searchtype=author&query=Soszy%C5%84ski%2C+I">I. Soszy艅ski</a>, <a href="/search/astro-ph?searchtype=author&query=Pietrukowicz%2C+P">P. Pietrukowicz</a>, <a href="/search/astro-ph?searchtype=author&query=Koz%C5%82owski%2C+S">S. Koz艂owski</a>, <a href="/search/astro-ph?searchtype=author&query=Ulaczyk%2C+K">K. Ulaczyk</a>, <a href="/search/astro-ph?searchtype=author&query=Iwanek%2C+P">P. Iwanek</a>, <a href="/search/astro-ph?searchtype=author&query=Wrona%2C+M">M. Wrona</a>, <a href="/search/astro-ph?searchtype=author&query=Gromadzki%2C+M">M. Gromadzki</a>, <a href="/search/astro-ph?searchtype=author&query=Mr%C3%B3z%2C+M+J">M. J. Mr贸z</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+F">F. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Bando%2C+K">K. Bando</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="2401.13759v2-abstract-short" style="display: inline;"> Gravitational microlensing is a phenomenon that allows us to observe dark remnants of stellar evolution even if they no longer emit electromagnetic radiation. In particular, it can be useful to observe solitary neutron stars or stellar-mass black holes, providing a unique window through which to understand stellar evolution. Obtaining direct mass measurements with this technique requires precise o… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.13759v2-abstract-full').style.display = 'inline'; document.getElementById('2401.13759v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.13759v2-abstract-full" style="display: none;"> Gravitational microlensing is a phenomenon that allows us to observe dark remnants of stellar evolution even if they no longer emit electromagnetic radiation. In particular, it can be useful to observe solitary neutron stars or stellar-mass black holes, providing a unique window through which to understand stellar evolution. Obtaining direct mass measurements with this technique requires precise observations of both the change in brightness and the position of the microlensed star. The European Space Agency's Gaia satellite can provide both. Using publicly available data from different surveys, we analysed events published in the Gaia Data Release 3 (Gaia DR3) microlensing catalogue. Here we describe our selection of candidate dark lenses, where we suspect the lens is a white dwarf (WD), a neutron star (NS), a black hole (BH), or a mass-gap object, with a mass in a range between the heaviest NS and the least massive BH. We estimated the mass of the lenses using information obtained from the best-fitting microlensing models, the source star, the Galactic model and the expected distribution of the parameters. We found eleven candidates for dark remnants: one WDs, three NS, three mass-gap objects, and four BHs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.13759v2-abstract-full').style.display = 'none'; document.getElementById('2401.13759v2-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 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 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">Accepted to Astronomy&Astrophysics, 20 pages, 4 figures, 6 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 692, A28 (2024) </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/2311.07647">arXiv:2311.07647</a> <span> [<a href="https://arxiv.org/pdf/2311.07647">pdf</a>, <a href="https://arxiv.org/ps/2311.07647">ps</a>, <a href="https://arxiv.org/format/2311.07647">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/10.32023/0001-5237/73.2.2">10.32023/0001-5237/73.2.2 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Candidates for Transiting Planets in OGLE-IV Galactic Bulge Fields </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mr%C3%B3z%2C+M+J">M. J. Mr贸z</a>, <a href="/search/astro-ph?searchtype=author&query=Pietrukowicz%2C+P">P. Pietrukowicz</a>, <a href="/search/astro-ph?searchtype=author&query=Poleski%2C+R">R. Poleski</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">A. Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Szyma%C5%84ski%2C+M+K">M. K. Szyma艅ski</a>, <a href="/search/astro-ph?searchtype=author&query=Gromadzki%2C+M">M. Gromadzki</a>, <a href="/search/astro-ph?searchtype=author&query=Ulaczyk%2C+K">K. Ulaczyk</a>, <a href="/search/astro-ph?searchtype=author&query=Koz%C5%82owski%2C+S">S. Koz艂owski</a>, <a href="/search/astro-ph?searchtype=author&query=Skowron%2C+J">J. Skowron</a>, <a href="/search/astro-ph?searchtype=author&query=Skowron%2C+D+M">D. M. Skowron</a>, <a href="/search/astro-ph?searchtype=author&query=Soszy%C5%84ski%2C+I">I. Soszy艅ski</a>, <a href="/search/astro-ph?searchtype=author&query=Mr%C3%B3z%2C+P">P. Mr贸z</a>, <a href="/search/astro-ph?searchtype=author&query=Ratajczak%2C+M">M. Ratajczak</a>, <a href="/search/astro-ph?searchtype=author&query=Rybicki%2C+K+A">K. A. Rybicki</a>, <a href="/search/astro-ph?searchtype=author&query=Iwanek%2C+P">P. Iwanek</a>, <a href="/search/astro-ph?searchtype=author&query=Wrona%2C+M">M. Wrona</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="2311.07647v1-abstract-short" style="display: inline;"> We present results of a search for transiting exoplanets in 10-yr long photometry with thousands of epochs taken in the direction of the Galactic bulge. This photometry was collected in the fourth phase of the Optical Gravitational Lensing Experiment (OGLE-IV). Our search covered approx. 222 000 stars brighter than I = 15.5 mag. Selected transits were verified using a probabilistic method. The sea… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.07647v1-abstract-full').style.display = 'inline'; document.getElementById('2311.07647v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.07647v1-abstract-full" style="display: none;"> We present results of a search for transiting exoplanets in 10-yr long photometry with thousands of epochs taken in the direction of the Galactic bulge. This photometry was collected in the fourth phase of the Optical Gravitational Lensing Experiment (OGLE-IV). Our search covered approx. 222 000 stars brighter than I = 15.5 mag. Selected transits were verified using a probabilistic method. The search resulted in 99 high-probability candidates for transiting exoplanets. The estimated distances to these targets are between 0.4 kpc and 5.5 kpc, which is a significantly wider range than for previous transit searches. The planets found are Jupiter-size, with the exception of one (named OGLE-TR-1003b) located in the hot Neptune desert. If the candidate is confirmed, it can be important for studies of highly irradiated intermediate-size planets. The existing long-term, high-cadence photometry of our candidates increases the chances of detecting transit timing variations at long timescales. Selected candidates will be observed by the future NASA flagship mission, the Nancy Grace Roman Space Telescope, in its search for Galactic bulge microlensing events, which will further enhance the photometric coverage of these stars. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.07647v1-abstract-full').style.display = 'none'; document.getElementById('2311.07647v1-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, 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">35 pages, 13 figures, 4 tables. Published in Acta Astronomica, online catalog: https://ogledb.astrouw.edu.pl/~ogle/OCVS/</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Acta Astronomica, vol, 73, no 2, p. 127-158 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.15147">arXiv:2309.15147</a> <span> [<a href="https://arxiv.org/pdf/2309.15147">pdf</a>, <a href="https://arxiv.org/ps/2309.15147">ps</a>, <a href="https://arxiv.org/format/2309.15147">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="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/10.32023/0001-5237/73.2.1">10.32023/0001-5237/73.2.1 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The OGLE Collection of Variable Stars. Over 15 000 Delta Scuti Stars in the Large Magellanic Cloud </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Soszy%C5%84ski%2C+I">I. Soszy艅ski</a>, <a href="/search/astro-ph?searchtype=author&query=Pietrukowicz%2C+P">P. Pietrukowicz</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">A. Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Skowron%2C+J">J. Skowron</a>, <a href="/search/astro-ph?searchtype=author&query=Szyma%C5%84ski%2C+M+K">M. K. Szyma艅ski</a>, <a href="/search/astro-ph?searchtype=author&query=Poleski%2C+R">R. Poleski</a>, <a href="/search/astro-ph?searchtype=author&query=Skowron%2C+D+M">D. M. Skowron</a>, <a href="/search/astro-ph?searchtype=author&query=Koz%C5%82owski%2C+S">S. Koz艂owski</a>, <a href="/search/astro-ph?searchtype=author&query=Mr%C3%B3z%2C+P">P. Mr贸z</a>, <a href="/search/astro-ph?searchtype=author&query=Iwanek%2C+P">P. Iwanek</a>, <a href="/search/astro-ph?searchtype=author&query=Wrona%2C+M">M. Wrona</a>, <a href="/search/astro-ph?searchtype=author&query=Ulaczyk%2C+K">K. Ulaczyk</a>, <a href="/search/astro-ph?searchtype=author&query=Rybicki%2C+K">K. Rybicki</a>, <a href="/search/astro-ph?searchtype=author&query=Gromadzki%2C+M">M. Gromadzki</a>, <a href="/search/astro-ph?searchtype=author&query=Mr%C3%B3z%2C+M">M. Mr贸z</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="2309.15147v2-abstract-short" style="display: inline;"> We present the OGLE collection of delta Scuti stars in the Large Magellanic Cloud and in its foreground. Our dataset encompasses a total of 15 256 objects, constituting the largest sample of extragalactic delta Sct stars published so far. In the case of 12 delta Sct pulsators, we detected additional eclipsing or ellipsoidal variations in their light curves. These are the first known candidates for… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.15147v2-abstract-full').style.display = 'inline'; document.getElementById('2309.15147v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.15147v2-abstract-full" style="display: none;"> We present the OGLE collection of delta Scuti stars in the Large Magellanic Cloud and in its foreground. Our dataset encompasses a total of 15 256 objects, constituting the largest sample of extragalactic delta Sct stars published so far. In the case of 12 delta Sct pulsators, we detected additional eclipsing or ellipsoidal variations in their light curves. These are the first known candidates for binary systems containing delta Sct components beyond the Milky Way. We provide observational parameters for all variables, including pulsation periods, mean magnitudes, amplitudes, and Fourier coefficients, as well as long-term light curves in the I- and V-bands collected during the fourth phase of the OGLE project. We construct the period-luminosity (PL) diagram, in which fundamental-mode and first-overtone delta Sct stars form two nearly parallel ridges. The latter ridge is an extension of the PL relation obeyed by first-overtone classical Cepheids. The slopes of the PL relations for delta Sct variables are steeper than those for classical Cepheids, indicating that the continuous PL relation for first-overtone delta Sct variables and Cepheids is non-linear, exhibiting a break at a period of approximately 0.5 d. We also report the enhancement of the OGLE collection of Cepheids and RR Lyr stars with newly identified and reclassified objects, including pulsators contained in the recently published Gaia DR3 catalog of variable stars. As a by-product, we estimate the contamination rate in the Gaia DR3 catalogs of Cepheids and RR Lyr variables. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.15147v2-abstract-full').style.display = 'none'; document.getElementById('2309.15147v2-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> 12 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 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">22 pages, 8 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Acta Astronomica 73 (2023) 105 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.06012">arXiv:2309.06012</a> <span> [<a href="https://arxiv.org/pdf/2309.06012">pdf</a>, <a href="https://arxiv.org/ps/2309.06012">ps</a>, <a href="https://arxiv.org/format/2309.06012">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="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/10.32023/0001-5237/73.1.1">10.32023/0001-5237/73.1.1 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Blue Large-Amplitude Pulsators and Other Short-Period Variable Stars in the OGLE-IV Galactic Disk Fields </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Borowicz%2C+J">J. Borowicz</a>, <a href="/search/astro-ph?searchtype=author&query=Pietrukowicz%2C+P">P. Pietrukowicz</a>, <a href="/search/astro-ph?searchtype=author&query=Mr%C3%B3z%2C+P">P. Mr贸z</a>, <a href="/search/astro-ph?searchtype=author&query=Soszy%C5%84ski%2C+I">I. Soszy艅ski</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">A. Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Szyma%C5%84ski%2C+M+K">M. K. Szyma艅ski</a>, <a href="/search/astro-ph?searchtype=author&query=Ulaczyk%2C+K">K. Ulaczyk</a>, <a href="/search/astro-ph?searchtype=author&query=Poleski%2C+R">R. Poleski</a>, <a href="/search/astro-ph?searchtype=author&query=Koz%C5%82owski%2C+S">S. Koz艂owski</a>, <a href="/search/astro-ph?searchtype=author&query=Skowron%2C+J">J. Skowron</a>, <a href="/search/astro-ph?searchtype=author&query=Skowron%2C+D+M">D. M. Skowron</a>, <a href="/search/astro-ph?searchtype=author&query=Rybicki%2C+K">K. Rybicki</a>, <a href="/search/astro-ph?searchtype=author&query=Iwanek%2C+P">P. Iwanek</a>, <a href="/search/astro-ph?searchtype=author&query=Wrona%2C+M">M. Wrona</a>, <a href="/search/astro-ph?searchtype=author&query=Gromadzki%2C+M">M. Gromadzki</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="2309.06012v3-abstract-short" style="display: inline;"> Blue Large-Amplitude Pulsators (BLAPs) form a mysterious class of variable stars with typical periods of tens of minutes and amplitudes above 0.1 mag. In this work, we present results of a variability search focused on timescales shorter than 1 h, conducted in OGLE-IV Galactic disk fields containing about 1.1 billion stellar sources down to I$\approx$20 mag. Twenty-five BLAPs have been detected, 2… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.06012v3-abstract-full').style.display = 'inline'; document.getElementById('2309.06012v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.06012v3-abstract-full" style="display: none;"> Blue Large-Amplitude Pulsators (BLAPs) form a mysterious class of variable stars with typical periods of tens of minutes and amplitudes above 0.1 mag. In this work, we present results of a variability search focused on timescales shorter than 1 h, conducted in OGLE-IV Galactic disk fields containing about 1.1 billion stellar sources down to I$\approx$20 mag. Twenty-five BLAPs have been detected, 20 of which are new discoveries. Their periods range from 8.4 min to 62.1 min. We have also found six new eclipsing binary systems with orbital periods from 38.3 min to 121.3 min and five short-period large-amplitude (> 0.17 mag in the I-band) variable stars of unknown type. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.06012v3-abstract-full').style.display = 'none'; document.getElementById('2309.06012v3-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 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 12 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">Journal ref:</span> Acta Astronomica, vol 73, no 1, p. 1-19, July 2023 </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/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/2301.04663">arXiv:2301.04663</a> <span> [<a href="https://arxiv.org/pdf/2301.04663">pdf</a>, <a href="https://arxiv.org/ps/2301.04663">ps</a>, <a href="https://arxiv.org/format/2301.04663">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="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/10.32023/0001-5237/72.4.1">10.32023/0001-5237/72.4.1 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The OGLE Collection of Variable Stars. Over 2600 Delta Scuti Stars in the Small Magellanic Cloud </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Soszy%C5%84ski%2C+I">I. Soszy艅ski</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">A. Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Skowron%2C+J">J. Skowron</a>, <a href="/search/astro-ph?searchtype=author&query=Pietrukowicz%2C+P">P. Pietrukowicz</a>, <a href="/search/astro-ph?searchtype=author&query=Szyma%C5%84ski%2C+M+K">M. K. Szyma艅ski</a>, <a href="/search/astro-ph?searchtype=author&query=Poleski%2C+R">R. Poleski</a>, <a href="/search/astro-ph?searchtype=author&query=Skowron%2C+D+M">D. M. Skowron</a>, <a href="/search/astro-ph?searchtype=author&query=Koz%C5%82owski%2C+S">S. Koz艂owski</a>, <a href="/search/astro-ph?searchtype=author&query=Mr%C3%B3z%2C+P">P. Mr贸z</a>, <a href="/search/astro-ph?searchtype=author&query=Iwanek%2C+P">P. Iwanek</a>, <a href="/search/astro-ph?searchtype=author&query=Wrona%2C+M">M. Wrona</a>, <a href="/search/astro-ph?searchtype=author&query=Ulaczyk%2C+K">K. Ulaczyk</a>, <a href="/search/astro-ph?searchtype=author&query=Rybicki%2C+K">K. Rybicki</a>, <a href="/search/astro-ph?searchtype=author&query=Gromadzki%2C+M">M. Gromadzki</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="2301.04663v1-abstract-short" style="display: inline;"> We present the first-ever collection of delta Scuti stars found over the entire area of the Small Magellanic Cloud (SMC). The sample consists of 2810 variables of which over 2600 objects belong to the SMC while the remaining stars are most likely members of the Milky Way's halo. The sample has been divided into 2733 singlemode and 77 multimode pulsators. We provide observational parameters (pulsat… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.04663v1-abstract-full').style.display = 'inline'; document.getElementById('2301.04663v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.04663v1-abstract-full" style="display: none;"> We present the first-ever collection of delta Scuti stars found over the entire area of the Small Magellanic Cloud (SMC). The sample consists of 2810 variables of which over 2600 objects belong to the SMC while the remaining stars are most likely members of the Milky Way's halo. The sample has been divided into 2733 singlemode and 77 multimode pulsators. We provide observational parameters (pulsation periods, mean magnitudes, amplitudes, Fourier coefficients) of all delta Sct stars and the long-term I- and V-band time-series photometric measurements collected during the fourth phase of the Optical Gravitational Lensing Experiment (OGLE-IV). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.04663v1-abstract-full').style.display = 'none'; document.getElementById('2301.04663v1-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 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">12 pages, 5 figures, submitted to Acta Astronomica</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Acta Astronomica 72 (2022) 245 </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/2212.07355">arXiv:2212.07355</a> <span> [<a href="https://arxiv.org/pdf/2212.07355">pdf</a>, <a href="https://arxiv.org/ps/2212.07355">ps</a>, <a href="https://arxiv.org/format/2212.07355">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> </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/10.32023/0001-5237/72.3.1">10.32023/0001-5237/72.3.1 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> New Short-Period Delta Scuti Stars in OGLE-IV Fields toward the Galactic Bulge </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pietrukowicz%2C+P">P. Pietrukowicz</a>, <a href="/search/astro-ph?searchtype=author&query=Ratajczak%2C+M">M. Ratajczak</a>, <a href="/search/astro-ph?searchtype=author&query=Soszynski%2C+I">I. Soszynski</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">A. Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Szymanski%2C+M+K">M. K. Szymanski</a>, <a href="/search/astro-ph?searchtype=author&query=Ulaczyk%2C+K">K. Ulaczyk</a>, <a href="/search/astro-ph?searchtype=author&query=Poleski%2C+R">R. Poleski</a>, <a href="/search/astro-ph?searchtype=author&query=Kozlowski%2C+S">S. Kozlowski</a>, <a href="/search/astro-ph?searchtype=author&query=Skowron%2C+J">J. Skowron</a>, <a href="/search/astro-ph?searchtype=author&query=Skowron%2C+D+M">D. M. Skowron</a>, <a href="/search/astro-ph?searchtype=author&query=Mroz%2C+P">P. Mroz</a>, <a href="/search/astro-ph?searchtype=author&query=Rybicki%2C+K">K. Rybicki</a>, <a href="/search/astro-ph?searchtype=author&query=Iwanek%2C+P">P. Iwanek</a>, <a href="/search/astro-ph?searchtype=author&query=Wrona%2C+M">M. Wrona</a>, <a href="/search/astro-ph?searchtype=author&query=Gromadzki%2C+M">M. Gromadzki</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="2212.07355v1-abstract-short" style="display: inline;"> We report the classification of 24 puzzling short-period variable stars located in OGLE-IV Galactic bulge fields. The stars are low-amplitude (<0.05 mag) multi-periodic objects with dominant periods between 22 and 54 min whose type could not have been unambiguously established based on photometry only. A low-resolution spectroscopic follow-up has shown that all the objects are main sequence A/F-ty… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.07355v1-abstract-full').style.display = 'inline'; document.getElementById('2212.07355v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.07355v1-abstract-full" style="display: none;"> We report the classification of 24 puzzling short-period variable stars located in OGLE-IV Galactic bulge fields. The stars are low-amplitude (<0.05 mag) multi-periodic objects with dominant periods between 22 and 54 min whose type could not have been unambiguously established based on photometry only. A low-resolution spectroscopic follow-up has shown that all the objects are main sequence A/F-type stars. Thus, all the variables are delta Sct-type pulsators. We have added them to the OGLE-IV Collection of Variable Stars. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.07355v1-abstract-full').style.display = 'none'; document.getElementById('2212.07355v1-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> 14 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">The OGLE data are available at https://www.astrouw.edu.pl/ogle/</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Acta Astronomica, 72, 161 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2212.00035">arXiv:2212.00035</a> <span> [<a href="https://arxiv.org/pdf/2212.00035">pdf</a>, <a href="https://arxiv.org/format/2212.00035">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 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/10.3847/1538-4365/acad7a">10.3847/1538-4365/acad7a <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A three-dimensional map of the Milky Way using 66,000 Mira variable stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Iwanek%2C+P">Patryk Iwanek</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=Koz%C5%82owski%2C+S">Szymon Koz艂owski</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=Ban%2C+M">Makiko Ban</a>, <a href="/search/astro-ph?searchtype=author&query=Skowron%2C+J">Jan Skowron</a>, <a href="/search/astro-ph?searchtype=author&query=Mr%C3%B3z%2C+P">Przemys艂aw Mr贸z</a>, <a href="/search/astro-ph?searchtype=author&query=Wrona%2C+M">Marcin Wrona</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">Andrzej Udalski</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+D+M">Dorota M. Skowron</a>, <a href="/search/astro-ph?searchtype=author&query=Ulaczyk%2C+K">Krzysztof Ulaczyk</a>, <a href="/search/astro-ph?searchtype=author&query=Gromadzki%2C+M">Mariusz Gromadzki</a>, <a href="/search/astro-ph?searchtype=author&query=Rybicki%2C+K">Krzysztof Rybicki</a>, <a href="/search/astro-ph?searchtype=author&query=Ratajczak%2C+M">Milena Ratajczak</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="2212.00035v2-abstract-short" style="display: inline;"> We study the three-dimensional structure of the Milky Way using 65,981 Mira variable stars discovered by the Optical Gravitational Lensing Experiment (OGLE) survey. The spatial distribution of the Mira stars is analyzed with a model containing three barred components that include the X-shaped boxy component in the Galactic center (GC), and an axisymmetric disk. We take into account the distance un… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.00035v2-abstract-full').style.display = 'inline'; document.getElementById('2212.00035v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.00035v2-abstract-full" style="display: none;"> We study the three-dimensional structure of the Milky Way using 65,981 Mira variable stars discovered by the Optical Gravitational Lensing Experiment (OGLE) survey. The spatial distribution of the Mira stars is analyzed with a model containing three barred components that include the X-shaped boxy component in the Galactic center (GC), and an axisymmetric disk. We take into account the distance uncertainties by implementing the Bayesian hierarchical inference method. The distance to the GC is $R_0 = 7.66 \pm 0.01 \mathrm{(stat.)} \pm 0.39 \mathrm{(sys.)}$ kpc, while the inclination of the major axis of the bulge to the Sun-GC line-of-sight is $胃= 20.2^\circ \pm 0.6^\circ \mathrm{(stat.)} \pm 0.7^\circ \mathrm{(sys.)} $. We present, for the first time, a detailed three-dimensional map of the Milky Way composed of young and intermediate-age stellar populations. Our analysis provides independent evidence for both the X-shaped bulge component and the flaring disk (being plausibly warped). We provide the complete dataset of properties of Miras that were used for calculations in this work. The table includes: mean brightness and amplitudes in nine photometric bands (covering a range of wavelength from 0.5 to 12 $渭$m), photometric chemical type, estimated extinction, and calculated distance with its uncertainty for each Mira variable. The median distance accuracy to a Mira star is at the level of $6.6\%$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.00035v2-abstract-full').style.display = 'none'; document.getElementById('2212.00035v2-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 December, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 30 November, 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">Accepted for publication in The Astrophysical Journal Supplement Series. 22 pages, 7 figures, 2 tables. The full machine readable Table 1 and corner plot are available through the OGLE website via https://www.astrouw.edu.pl/ogle/ogle4/MILKY_WAY_3D_MAP/, and Zenodo via https://doi.org/10.5281/zenodo.7472598</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/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/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/2207.07675">arXiv:2207.07675</a> <span> [<a href="https://arxiv.org/pdf/2207.07675">pdf</a>, <a href="https://arxiv.org/format/2207.07675">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</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/10.1038/s41550-022-01730-y">10.1038/s41550-022-01730-y <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> An X-ray quiet black hole born with a negligible kick in a massive binary within the Large Magellanic Cloud </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Shenar%2C+T">Tomer Shenar</a>, <a href="/search/astro-ph?searchtype=author&query=Sana%2C+H">Hugues Sana</a>, <a href="/search/astro-ph?searchtype=author&query=Mahy%2C+L">Laurent Mahy</a>, <a href="/search/astro-ph?searchtype=author&query=El-Badry%2C+K">Kareem El-Badry</a>, <a href="/search/astro-ph?searchtype=author&query=Marchant%2C+P">Pablo Marchant</a>, <a href="/search/astro-ph?searchtype=author&query=Langer%2C+N">Norbert Langer</a>, <a href="/search/astro-ph?searchtype=author&query=Hawcroft%2C+C">Calum Hawcroft</a>, <a href="/search/astro-ph?searchtype=author&query=Fabry%2C+M">Matthias Fabry</a>, <a href="/search/astro-ph?searchtype=author&query=Sen%2C+K">Koushik Sen</a>, <a href="/search/astro-ph?searchtype=author&query=Almeida%2C+L+A">Leonardo A. Almeida</a>, <a href="/search/astro-ph?searchtype=author&query=Abdul-Masih%2C+M">Michael Abdul-Masih</a>, <a href="/search/astro-ph?searchtype=author&query=Bodensteiner%2C+J">Julia Bodensteiner</a>, <a href="/search/astro-ph?searchtype=author&query=Crowther%2C+P+A">Paul A. Crowther</a>, <a href="/search/astro-ph?searchtype=author&query=Gieles%2C+M">Mark Gieles</a>, <a href="/search/astro-ph?searchtype=author&query=Gromadzki%2C+M">Mariusz Gromadzki</a>, <a href="/search/astro-ph?searchtype=author&query=Henault-Brunet%2C+V">Vincent Henault-Brunet</a>, <a href="/search/astro-ph?searchtype=author&query=Herrero%2C+A">Artemio Herrero</a>, <a href="/search/astro-ph?searchtype=author&query=de+Koter%2C+A">Alex de Koter</a>, <a href="/search/astro-ph?searchtype=author&query=Iwanek%2C+P">Patryk Iwanek</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=Lennon%2C+D+J">Daniel J. Lennon</a>, <a href="/search/astro-ph?searchtype=author&query=Apellaniz%2C+J+M">Jesus Ma谋z Apellaniz</a>, <a href="/search/astro-ph?searchtype=author&query=Mroz%2C+P">Przemys艂aw Mroz</a>, <a href="/search/astro-ph?searchtype=author&query=Moffat%2C+A+F+J">Anthony F. J. Moffat</a>, <a href="/search/astro-ph?searchtype=author&query=Picco%2C+A">Annachiara Picco</a> , et al. (13 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="2207.07675v1-abstract-short" style="display: inline;"> Stellar-mass black holes are the final remnants of stars born with more than 15 solar masses. Billions are expected to reside in the Local Group, yet only few are known, mostly detected through X-rays emitted as they accrete material from a companion star. Here, we report on VFTS 243: a massive X-ray faint binary in the Large Magellanic Cloud. With an orbital period of 10.4-d, it comprises an O-ty… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.07675v1-abstract-full').style.display = 'inline'; document.getElementById('2207.07675v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2207.07675v1-abstract-full" style="display: none;"> Stellar-mass black holes are the final remnants of stars born with more than 15 solar masses. Billions are expected to reside in the Local Group, yet only few are known, mostly detected through X-rays emitted as they accrete material from a companion star. Here, we report on VFTS 243: a massive X-ray faint binary in the Large Magellanic Cloud. With an orbital period of 10.4-d, it comprises an O-type star of 25 solar masses and an unseen companion of at least nine solar masses. Our spectral analysis excludes a non-degenerate companion at a 5-sigma confidence level. The minimum companion mass implies that it is a black hole. No other X-ray quiet black hole is unambiguously known outside our Galaxy. The (near-)circular orbit and kinematics of VFTS 243 imply that the collapse of the progenitor into a black hole was associated with little or no ejected material or black-hole kick. Identifying such unique binaries substantially impacts the predicted rates of gravitational-wave detections and properties of core-collapse supernovae across the Cosmos. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.07675v1-abstract-full').style.display = 'none'; document.getElementById('2207.07675v1-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> <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 to Nature Astronomy, 64 pages, 15 figures, 2 tables; ESO press release: https://www.eso.org/public/news/eso2210/; Nat Asr paper URL: https://www.nature.com/articles/s41550-022-01730-y</span> </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/2205.10510">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/2204.05606">arXiv:2204.05606</a> <span> [<a href="https://arxiv.org/pdf/2204.05606">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="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/10.1093/mnras/stac2315">10.1093/mnras/stac2315 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> OGLE-2019-BLG-1470LABc: Another Microlensing Giant Planet in a Binary System? </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kuang%2C+R">Renkun Kuang</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=Yang%2C+H">Hongjing Yang</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=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=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+L">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="2204.05606v2-abstract-short" style="display: inline;"> We report the discovery and analysis of a candidate triple-lens single-source (3L1S) microlensing event, OGLE-2019-BLG-1470. This event was first classified as a normal binary-lens single-source (2L1S) event, but a careful 2L1S modelling showed that it needs an additional lens or source to fit the observed data. It is found that the 3L1S model provides the best fit, but the binary-lens binary-sour… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.05606v2-abstract-full').style.display = 'inline'; document.getElementById('2204.05606v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.05606v2-abstract-full" style="display: none;"> We report the discovery and analysis of a candidate triple-lens single-source (3L1S) microlensing event, OGLE-2019-BLG-1470. This event was first classified as a normal binary-lens single-source (2L1S) event, but a careful 2L1S modelling showed that it needs an additional lens or source to fit the observed data. It is found that the 3L1S model provides the best fit, but the binary-lens binary-source (2L2S) model is only disfavoured by $螖蠂^2 \simeq 18$. All of the feasible models include a planet with planet-to-host mass-ratios $10^{-3} \lesssim q \lesssim 10^{-2}$. A Bayesian analysis based on a Galactic model indicates that the planet is super-Jovian, and the projected host-planet separation is about 3 $\mathrm{au}$. Specifically, for the best-fit 3L1S model, the two stars have masses of $M_1=0.57^{+0.43}_{-0.32}M_{\odot}$, and $M_2=0.18^{+0.15}_{-0.10}M_{\odot}$, with projected separation of $1.3^{+0.5}_{-0.5}$ $\mathrm{au}$, and the planetary mass is $M_3=2.2^{+1.8}_{-1.3}M_{\rm{Jupiter}}$. For the 2L2S model, the masses of the host star and the planet are $0.55^{+0.44}_{-0.31}M_{\odot}$ and $4.6^{+3.7}_{-2.6}M_{\rm{Jupiter}}$, respectively. By investigating the properties of all known microlensing planets in binary systems, we find that all planets in binary systems published by the KMTNet survey are located inside the resonant caustics range with $q \gtrsim 2 \times 10^{-3}$, indicating the incompleteness of the KMTNet sample for planets in binary systems. Thus, planets in binary systems cannot be included in the current study of the KMTNet mass-ratio function, and a systematic search for planetary anomalies in KMTNet microlensing light curves of binary systems is needed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.05606v2-abstract-full').style.display = 'none'; document.getElementById('2204.05606v2-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> 6 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 12 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">17 pages, 14 figures, published in MNRAS</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> MNRAS 516, 1704-1720 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2204.04354">arXiv:2204.04354</a> <span> [<a href="https://arxiv.org/pdf/2204.04354">pdf</a>, <a href="https://arxiv.org/ps/2204.04354">ps</a>, <a href="https://arxiv.org/format/2204.04354">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/10.1051/0004-6361/202243744">10.1051/0004-6361/202243744 <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. V. Complete Sample of 2018 Prime-Field </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=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=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=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=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>, <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. (43 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="2204.04354v1-abstract-short" style="display: inline;"> We complete the analysis of all 2018 prime-field microlensing planets identified by the KMTNet AnomalyFinder. Among the 10 previously unpublished events with clear planetary solutions, 8 are either unambiguously planetary or are very likely to be planetary in nature: OGLE-2018-BLG-1126, KMT-2018-BLG-2004, OGLE-2018-BLG-1647, OGLE-2018-BLG-1367, OGLE-2018-BLG-1544, OGLE-2018-BLG-0932, OGLE-2018-BLG… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.04354v1-abstract-full').style.display = 'inline'; document.getElementById('2204.04354v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.04354v1-abstract-full" style="display: none;"> We complete the analysis of all 2018 prime-field microlensing planets identified by the KMTNet AnomalyFinder. Among the 10 previously unpublished events with clear planetary solutions, 8 are either unambiguously planetary or are very likely to be planetary in nature: OGLE-2018-BLG-1126, KMT-2018-BLG-2004, OGLE-2018-BLG-1647, OGLE-2018-BLG-1367, OGLE-2018-BLG-1544, OGLE-2018-BLG-0932, OGLE-2018-BLG-1212, and KMT-2018-BLG-2718. Combined with the 4 previously published new AnomalyFinder events and 12 previously published (or in preparation) planets that were discovered by eye, thismakes a total of 24 2018 prime-field planets discovered or recovered by AnomalyFinder. Together with a paper in preparation on 2018 sub-prime planets, this work lays the basis for the first statistical analysis of the planet mass-ratio function based on planets identified in KMTNet data. By systematically applying the heuristic analysis of Hwang et al. (2022) to each event, we identify the small modification in their formalism that is needed to unify the so-called close/wide and inner/outer degeneracies, as conjectured by <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.04354v1-abstract-full').style.display = 'none'; document.getElementById('2204.04354v1-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, 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">22 pages, 14 tables, 15 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/2204.02017">arXiv:2204.02017</a> <span> [<a href="https://arxiv.org/pdf/2204.02017">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/stac1883">10.1093/mnras/stac1883 <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. IV. Complete Sample of 2019 Prime-Field </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=Yang%2C+H">Hongjing Yang</a>, <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=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=Mao%2C+S">Shude Mao</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+X">Xiangyu Zhang</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=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=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+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=Mr%C3%B3z%2C+P">Przemek Mr贸z</a> , et al. (11 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="2204.02017v2-abstract-short" style="display: inline;"> We report the complete statistical planetary sample from the prime fields ($螕\geq 2~{\rm hr}^{-1}$) of the 2019 Korea Microlensing Telescope Network (KMTNet) microlensing survey. We develop the optimized KMTNet AnomalyFinder algorithm and apply it to the 2019 KMTNet prime fields. We find a total of 14 homogeneously selected planets and report the analysis of three planetary events, KMT-2019-BLG-(1… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.02017v2-abstract-full').style.display = 'inline'; document.getElementById('2204.02017v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.02017v2-abstract-full" style="display: none;"> We report the complete statistical planetary sample from the prime fields ($螕\geq 2~{\rm hr}^{-1}$) of the 2019 Korea Microlensing Telescope Network (KMTNet) microlensing survey. We develop the optimized KMTNet AnomalyFinder algorithm and apply it to the 2019 KMTNet prime fields. We find a total of 14 homogeneously selected planets and report the analysis of three planetary events, KMT-2019-BLG-(1042,1552,2974). The planet-host mass ratios, $q$, for the three planetary events are $6.34 \times 10^{-4}, 4.89 \times 10^{-3}$ and $6.18 \times 10^{-4}$, respectively. A Bayesian analysis indicates the three planets are all cold giant planets beyond the snow line of their host stars. The 13 planets are basically uniform in $\log q$ over the range $-5.0 < \log q < -1.5$. This result suggests that the planets below $q_{\rm break} = 1.7 \times 10^{-4}$ proposed by the MOA-II survey may be more common than previously believed. This work is an early component of a large project to determine the KMTNet mass-ratio function, and the whole sample of 2016--2019 KMTNet events should contain about 120 planets. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.02017v2-abstract-full').style.display = 'none'; document.getElementById('2204.02017v2-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 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 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">Accepted by 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/2203.16552">arXiv:2203.16552</a> <span> [<a href="https://arxiv.org/pdf/2203.16552">pdf</a>, <a href="https://arxiv.org/format/2203.16552">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="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/10.3847/1538-4365/ac6676">10.3847/1538-4365/ac6676 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The OGLE Collection of Variable Stars. Nearly 66,000 Mira stars in the Milky Way </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Iwanek%2C+P">Patryk Iwanek</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=Koz%C5%82owski%2C+S">Szymon Koz艂owski</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=Pietrukowicz%2C+P">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=Wrona%2C+M">Marcin Wrona</a>, <a href="/search/astro-ph?searchtype=author&query=Mr%C3%B3z%2C+P">Przemys艂aw Mr贸z</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">Andrzej Udalski</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+D+M">Dorota M. Skowron</a>, <a href="/search/astro-ph?searchtype=author&query=Ulaczyk%2C+K">Krzysztof Ulaczyk</a>, <a href="/search/astro-ph?searchtype=author&query=Gromadzki%2C+M">Mariusz Gromadzki</a>, <a href="/search/astro-ph?searchtype=author&query=Rybicki%2C+K">Krzysztof Rybicki</a>, <a href="/search/astro-ph?searchtype=author&query=Ratajczak%2C+M">Milena Ratajczak</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="2203.16552v2-abstract-short" style="display: inline;"> We present a collection of 65,981 Mira-type variable stars found in the Optical Gravitational Lensing Experiment (OGLE) project database. Two-thirds of our sample (40,356 objects) are located in the Galactic bulge fields, whereas 25,625 stars are in the Galactic disk. The vast majority of the collection (47,532 objects) are new discoveries. We provide basic observational parameters of the Mira var… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.16552v2-abstract-full').style.display = 'inline'; document.getElementById('2203.16552v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.16552v2-abstract-full" style="display: none;"> We present a collection of 65,981 Mira-type variable stars found in the Optical Gravitational Lensing Experiment (OGLE) project database. Two-thirds of our sample (40,356 objects) are located in the Galactic bulge fields, whereas 25,625 stars are in the Galactic disk. The vast majority of the collection (47,532 objects) are new discoveries. We provide basic observational parameters of the Mira variables: equatorial coordinates, pulsation periods, $I$-band and $V$-band mean magnitudes, $I$-band brightness amplitudes, and identifications in other catalogs of variable stars. We also provide the $I$-band and $V$-band time-series photometry collected since 1997 during the OGLE-II, OGLE-III, and OGLE-IV phases. The classical selection process, i.e., mostly based on the visual inspection of light curves by experienced astronomers, led us to the high purity of the catalog. As a result, this collection can be used as a training set in the machine learning classification algorithms. Using overlapping parts of adjacent OGLE fields, we estimate the completeness of the catalog to be about 96%. We compare and discuss the statistical features of Miras located in different regions of the Milky Way. We show examples of stars that change their type over time, from a semi-regular variable to Mira and vice versa. This dataset is perfectly suited to study the three-dimensional structure of the Milky Way, and it may help to explain the puzzle of the X-shaped bulge. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.16552v2-abstract-full').style.display = 'none'; document.getElementById('2203.16552v2-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> 12 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 30 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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 for publication in The Astrophysical Journal Supplement Series. 18 pages, 8 figures, 3 tables. The OGLE Collection of Miras in the Milky Way is publicly available through http://www.astrouw.edu.pl/ogle/ogle4/OCVS/blg/lpv/ for Miras located in the Galactic bulge fields, and http://www.astrouw.edu.pl/ogle/ogle4/OCVS/gd/lpv/ for Miras located in the Galactic disk fields</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.04034">arXiv:2203.04034</a> <span> [<a href="https://arxiv.org/pdf/2203.04034">pdf</a>, <a href="https://arxiv.org/format/2203.04034">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/10.1051/0004-6361/202243490">10.1051/0004-6361/202243490 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Precision measurement of a brown dwarf mass in a binary system in the microlensing event OGLE-2019-BLG-0033/MOA-2019-BLG-035 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Herald%2C+A">A. Herald</a>, <a href="/search/astro-ph?searchtype=author&query=Udalski%2C+A">A. Udalski</a>, <a href="/search/astro-ph?searchtype=author&query=Bozza%2C+V">V. Bozza</a>, <a href="/search/astro-ph?searchtype=author&query=Rota%2C+P">P. Rota</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+I+A">I. A. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Yee%2C+J+C">J. C. Yee</a>, <a href="/search/astro-ph?searchtype=author&query=Sajadian%2C+S">S. Sajadian</a>, <a href="/search/astro-ph?searchtype=author&query=Mroz%2C+P">P. Mroz</a>, <a href="/search/astro-ph?searchtype=author&query=Poleski%2C+R">R. Poleski</a>, <a href="/search/astro-ph?searchtype=author&query=Skowron%2C+J">J. Skowron</a>, <a href="/search/astro-ph?searchtype=author&query=Szymanski%2C+M+K">M. K. Szymanski</a>, <a href="/search/astro-ph?searchtype=author&query=Soszynski%2C+I">I. Soszynski</a>, <a href="/search/astro-ph?searchtype=author&query=Pietrukowicz%2C+P">P. Pietrukowicz</a>, <a href="/search/astro-ph?searchtype=author&query=Kozlowski%2C+S">S. Kozlowski</a>, <a href="/search/astro-ph?searchtype=author&query=Ulaczyk%2C+K">K. Ulaczyk</a>, <a href="/search/astro-ph?searchtype=author&query=Rybicki%2C+K+A">K. A. Rybicki</a>, <a href="/search/astro-ph?searchtype=author&query=Iwanek%2C+P">P. Iwanek</a>, <a href="/search/astro-ph?searchtype=author&query=Wrona%2C+M">M. Wrona</a>, <a href="/search/astro-ph?searchtype=author&query=Gromadzki%2C+M">M. Gromadzki</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+F">F. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Barry%2C+R">R. Barry</a>, <a href="/search/astro-ph?searchtype=author&query=Bennett%2C+D+P">D. P. Bennett</a>, <a href="/search/astro-ph?searchtype=author&query=Bhattacharya%2C+A">A. Bhattacharya</a>, <a href="/search/astro-ph?searchtype=author&query=Fukui%2C+A">A. Fukui</a>, <a href="/search/astro-ph?searchtype=author&query=Fujii%2C+H">H. Fujii</a> , et al. (67 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="2203.04034v3-abstract-short" style="display: inline;"> Context. Brown dwarfs are poorly understood transition objects between stars and planets, with several competing mechanisms having been proposed for their formation. Mass measurements are generally difficult for isolated objects but also for brown dwarfs orbiting low-mass stars, which are often too faint for spectroscopic follow-up. Aims. Microlensing provides an alternative tool for the discovery… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.04034v3-abstract-full').style.display = 'inline'; document.getElementById('2203.04034v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.04034v3-abstract-full" style="display: none;"> Context. Brown dwarfs are poorly understood transition objects between stars and planets, with several competing mechanisms having been proposed for their formation. Mass measurements are generally difficult for isolated objects but also for brown dwarfs orbiting low-mass stars, which are often too faint for spectroscopic follow-up. Aims. Microlensing provides an alternative tool for the discovery and investigation of such faint systems. Here we present the analysis of the microlensing event OGLE-2019-BLG-0033/MOA-2019-BLG-035, which is due to a binary system composed of a brown dwarf orbiting a red dwarf. Methods. Thanks to extensive ground observations and the availability of space observations from Spitzer, it has been possible to obtain accurate estimates of all microlensing parameters, including parallax, source radius and orbital motion of the binary lens. Results. After accurate modeling, we find that the lens is composed of a red dwarf with mass $M_1 = 0.149 \pm 0.010M_\odot$ and a brown dwarf with mass $M_2 = 0.0463 \pm 0.0031M_\odot$, at a projected separation of $a_\perp = 0.585$ au. The system has a peculiar velocity that is typical of old metal-poor populations in the thick disk. Percent precision in the mass measurement of brown dwarfs has been achieved only in a few microlensing events up to now, but will likely become common with the Roman space telescope. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.04034v3-abstract-full').style.display = 'none'; document.getElementById('2203.04034v3-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 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">13 pages, 6 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 663, A100 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2112.02414">arXiv:2112.02414</a> <span> [<a href="https://arxiv.org/pdf/2112.02414">pdf</a>, <a href="https://arxiv.org/format/2112.02414">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/10.1093/mnras/stab3581">10.1093/mnras/stab3581 <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 III: One Wide-Orbit Planet And Two Stellar Binaries </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Wang%2C+H">Hanyue Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Zang%2C+W">Weicheng Zang</a>, <a href="/search/astro-ph?searchtype=author&query=Zhu%2C+W">Wei Zhu</a>, <a href="/search/astro-ph?searchtype=author&query=Hwang%2C+K">Kyu-Ha Hwang</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=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=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=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>, <a href="/search/astro-ph?searchtype=author&query=Poleski%2C+R">Radoslaw Poleski</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="2112.02414v1-abstract-short" style="display: inline;"> Only a few wide-orbit planets around old stars have been detected, which limits our statistical understanding of this planet population. Following the systematic search for planetary anomalies in microlensing events found by the Korea Microlensing Telescope Network (KMTNet), we present the discovery and analysis of three events that were initially thought to contain wide-orbit planets. The anomalo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.02414v1-abstract-full').style.display = 'inline'; document.getElementById('2112.02414v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2112.02414v1-abstract-full" style="display: none;"> Only a few wide-orbit planets around old stars have been detected, which limits our statistical understanding of this planet population. Following the systematic search for planetary anomalies in microlensing events found by the Korea Microlensing Telescope Network (KMTNet), we present the discovery and analysis of three events that were initially thought to contain wide-orbit planets. The anomalous feature in the light curve of OGLE-2018-BLG-0383 is caused by a planet with mass ratio $q=2.1\times 10^{-4}$ and a projected separation $s=2.45$. This makes it the lowest mass-ratio microlensing planet at such wide orbits. The other two events, KMT-2018-BLG-0998 and OGLE-2018-BLG-0271, are shown to be stellar binaries ($q>0.1$) with rather close ($s<1$) separations. We briefly discuss the properties of known wide-orbit microlensing planets and show that the survey observations are crucial in discovering and further statistically constraining such a planet population. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.02414v1-abstract-full').style.display = 'none'; document.getElementById('2112.02414v1-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 December, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2021. </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 by 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/2112.01613">arXiv:2112.01613</a> <span> [<a href="https://arxiv.org/pdf/2112.01613">pdf</a>, <a href="https://arxiv.org/format/2112.01613">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 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/10.1051/0004-6361/202039542">10.1051/0004-6361/202039542 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Single-lens mass measurement in the high-magnification microlensing event Gaia19bld located in the Galactic disc </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Rybicki%2C+K+A">K. A. Rybicki</a>, <a href="/search/astro-ph?searchtype=author&query=Wyrzykowski%2C+%C5%81">艁. Wyrzykowski</a>, <a href="/search/astro-ph?searchtype=author&query=Bachelet%2C+E">E. Bachelet</a>, <a href="/search/astro-ph?searchtype=author&query=Cassan%2C+A">A. Cassan</a>, <a href="/search/astro-ph?searchtype=author&query=Zieli%C5%84ski%2C+P">P. Zieli艅ski</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+A">A. Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Novati%2C+S+C">S. Calchi Novati</a>, <a href="/search/astro-ph?searchtype=author&query=Yee%2C+J+C">J. C. Yee</a>, <a href="/search/astro-ph?searchtype=author&query=Ryu%2C+Y+-">Y. -H. Ryu</a>, <a href="/search/astro-ph?searchtype=author&query=Gromadzki%2C+M">M. Gromadzki</a>, <a href="/search/astro-ph?searchtype=author&query=Miko%C5%82ajczyk%2C+P">P. Miko艂ajczyk</a>, <a href="/search/astro-ph?searchtype=author&query=Ihanec%2C+N">N. Ihanec</a>, <a href="/search/astro-ph?searchtype=author&query=Kruszy%C5%84ska%2C+K">K. Kruszy艅ska</a>, <a href="/search/astro-ph?searchtype=author&query=Hambsch%2C+F+-">F. -J. Hambsch</a>, <a href="/search/astro-ph?searchtype=author&query=Zo%C5%82a%2C+S">S. Zo艂a</a>, <a href="/search/astro-ph?searchtype=author&query=Fossey%2C+S+J">S. J. Fossey</a>, <a href="/search/astro-ph?searchtype=author&query=Awiphan%2C+S">S. Awiphan</a>, <a href="/search/astro-ph?searchtype=author&query=Nakharutai%2C+N">N. Nakharutai</a>, <a href="/search/astro-ph?searchtype=author&query=Lewis%2C+F">F. Lewis</a>, <a href="/search/astro-ph?searchtype=author&query=E.%2C+F+O">F. Olivares E.</a>, <a href="/search/astro-ph?searchtype=author&query=Hodgkin%2C+S">S. Hodgkin</a>, <a href="/search/astro-ph?searchtype=author&query=Delgado%2C+A">A. Delgado</a>, <a href="/search/astro-ph?searchtype=author&query=Breedt%2C+E">E. Breedt</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+D+L">D. L. Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=vanLeeuwen%2C+M">M. vanLeeuwen</a> , et al. (44 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="2112.01613v1-abstract-short" style="display: inline;"> We present the photometric analysis of Gaia19bld, a high-magnification ($A\approx60$) microlensing event located in the southern Galactic plane, which exhibited finite source and microlensing parallax effects. Due to a prompt detection by the Gaia satellite and the very high brightness of $I = 9.05~$mag at the peak, it was possible to collect a complete and unique set of multi-channel follow-up ob… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.01613v1-abstract-full').style.display = 'inline'; document.getElementById('2112.01613v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2112.01613v1-abstract-full" style="display: none;"> We present the photometric analysis of Gaia19bld, a high-magnification ($A\approx60$) microlensing event located in the southern Galactic plane, which exhibited finite source and microlensing parallax effects. Due to a prompt detection by the Gaia satellite and the very high brightness of $I = 9.05~$mag at the peak, it was possible to collect a complete and unique set of multi-channel follow-up observations, which allowed us to determine all parameters vital for the characterisation of the lens and the source in the microlensing event. Gaia19bld was discovered by the Gaia satellite and was subsequently intensively followed up with a network of ground-based observatories and the Spitzer Space Telescope. We collected multiple high-resolution spectra with Very Large Telescope (VLT)/X-Shooter to characterise the source star. The event was also observed with VLT Interferometer (VLTI)/PIONIER during the peak. Here we focus on the photometric observations and model the light curve composed of data from Gaia, Spitzer, and multiple optical, ground-based observatories. We find the best-fitting solution with parallax and finite source effects. We derived the limit on the luminosity of the lens based on the blended light model and spectroscopic distance. We compute the mass of the lens to be $1.13 \pm 0.03~M_{\odot}$ and derive its distance to be $5.52^{+0.35}_{-0.64}~\mathrm{kpc}$. The lens is likely a main sequence star, however its true nature has yet to be verified by future high-resolution observations. Our results are consistent with interferometric measurements of the angular Einstein radius, emphasising that interferometry can be a new channel for determining the masses of objects that would otherwise remain undetectable, including stellar-mass black holes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.01613v1-abstract-full').style.display = 'none'; document.getElementById('2112.01613v1-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, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2021. </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 to Astronomy&Astrophysics</span> </p> </li> </ol> <nav class="pagination is-small is-centered breathe-horizontal" 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