The EROS2 search for microlensing events towards the spiral arms: the complete seven season results
Y. R. Rahal, C. Afonso, J. -N. Albert, J. Andersen, R. Ansari, E. Aubourg, P. Bareyre, J. -P. Beaulieu, X. Charlot, F. Couchot, C. Coutures, F. Derue, R. Ferlet… 展开作者
Y. R. Rahal, C. Afonso, J. -N. Albert, J. Andersen, R. Ansari, E. Aubourg, P. Bareyre, J. -P. Beaulieu, X. Charlot, F. Couchot, C. Coutures, F. Derue, R. Ferlet, P. Fouqué, J. -F. Glicenstein, B. Goldman, A. Gould, D. Graff, M. Gros, J. Haissinski, C. Hamadache, J. de Kat, E. Lesquoy, C. Loup, L. Le Guillou, C. Magneville, B. Mansoux, J. -B. Marquette, E. Maurice, A. Maury, A. Milsztajn, M. Moniez, N. Palanque-Delabrouille, O. Perdereau, S. Rahvar, J. Rich, M. Spiro, P. Tisserand, A. Vidal-Madjar
The EROS-2 project has been designed to search for microlensing events towards any dense stellar field. The densest parts of the Galactic spiral arms have been monitored to maximize the microlensing signal expected from the stars of the Galactic disk and bulge. 12.9 million stars have been monitored during 7 seasons towards 4 directions in the Galactic plane, away from the Galactic center. A total of 27 microlensing event candidates have been found. Estimates of the optical depths from the 22 best events are provided. A first order interpretation shows that simple Galactic models with a standard disk and an elongated bulge are in agreement with our observations. We find that the average microlensing optical depth towards the complete EROS-cataloged stars of the spiral arms is $\barτ =0.51\pm .13\times 10^{-6}$, a number that is stable when the selection criteria are moderately varied. As the EROS catalog is almost complete up to $I_C=18.5$, the optical depth estimated for the sub-sample of bright target stars with $I_C<18.5$ ($\barτ=0.39\pm >.11\times 10^{-6}$) is easier to interpret. The set of microlensing events that we have observed is consistent with a simple Galactic model. A more precise interpretation would require either a better knowledge of the distance distribution of the target stars, or a simulation based on a Galactic model. For this purpose, we define and discuss the concept of optical depth for a given catalog or for a limiting magnitude.
Systematic KMTNet Planetary Anomaly Search. XIII. Complete Sample of 2021 Prime Field Planets
Westlake University（西湖大学）；Chungbuk National University（忠北国立大学）；Ohio State University（俄亥俄州立大学）；Korea Astronomy and Space Science Institute（韩国天文和空间科学研究所）；Massey University（梅西大学）；Osaka University（大阪大学）
Mass Production of 2023 KMTNet Microlensing Planets I: Low Mass Ratio
Korea Astronomy and Space Science Institute（韩国天文与空间科学研究所）；Astronomical Observatory, University of Warsaw（华沙大学天文台）；Westlake University（西湖大学）；Tsinghua University（清华大学）；University of Chinese Academy of Sciences（中国科学院大学）；Ohio State University（俄亥俄州立大学）；University of Canterbury（坎特伯雷大学）
KMT-2025-BLG-0975Lb and KMT-2025-BLG-1160Lb: Two Uranus-Mass Planets Beyond the Snow Line Discovered by Microlensing
Chungbuk National University（忠北国立大学）；Korea Astronomy and Space Science Institute（韩国天体宇宙科学研究所）；University of Warsaw（华沙大学）；Ohio State University（俄亥俄州立大学）；University of Canterbury（坎特伯雷大学）；University of Science and Technology（科学技术大学）
IRFU, CEA, Universite de Paris-Saclay（萨克雷大学CEA IRFU）；Université Paris-Saclay, CNRS/IN2P3, IJCLab（巴黎萨克莱大学CNRS/IN2P3 IJCLab）；Université Paris-Saclay, Université Paris Cité, CEA, CNRS, AIM（巴黎萨克莱大学、巴黎西岱大学、CEA、CNRS AIM）；Université de Paris, CNRS, Astroparticule et Cosmologie（巴黎大学CNRS 粒子天体物理学）；Sorbonne Universités, UPMC Univ Paris 6 et CNRS, UMR 7095, Institut d’Astrophysique de Paris, IAP（索邦大学、巴黎第六大学及CNRS 巴黎天文台）；Sorbonne Université, CNRS/IN2P3, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE)（索邦大学CNRS/IN2P3 核与高能物理实验室）；Université de Strasbourg, CNRS, Observatoire Astronomique, CNRS, UMR 7550（斯特拉斯堡大学CNRS 天文观测站）
The X-Ray Continuum Emission Region in the Lensed Quasar SDSS J133907.23+131038.6 is Much Smaller than the Accretion Disk
United States Naval Academy（美国海军学院）；The University of Oklahoma（俄克拉荷马大学）；Instituto de Física de Cantabria (CSIC-UC)（坎塔布里亚物理研究所（西班牙国家研究委员会-坎塔布里亚大学））；O.Ya. Usikov Institute for Radiophysics and Electronics（O.Ya.乌西科夫无线电物理与电子研究所）；College of Charleston（查尔斯顿学院）
