Dark lens candidates from Gaia Data Release 3

被引：2

作者：

Kruszyńska, K. ^{[1
,2
]}

Wyrzykowski, L. ^{[1
]}

Rybicki, K.A. ^{[3
]}

Howil, K. ^{[1
]}

Jablońska, M. ^{[1
,4
]}

Kaczmarek, Z. ^{[5
]}

Ihanec, N. ^{[1
]}

Maskoliūnas, M. ^{[6
]}

Bronikowski, M. ^{[7
]}

Pylypenko, U. ^{[1
]}

Udalski, A. ^{[1
]}

Mróz, P. ^{[1
]}

Poleski, R. ^{[1
]}

Skowron, J. ^{[1
]}

Szymański, M.K. ^{[1
]}

Soszyński, I. ^{[1
]}

Pietrukowicz, P. ^{[1
]}

Kozlowski, S. ^{[1
]}

Ulaczyk, K. ^{[8
]}

Iwanek, P. ^{[1
]}

Wrona, M. ^{[1
]}

Gromadzki, M. ^{[1
]}

Mróz, M.J. ^{[1
]}

Abe, F. ^{[9
]}

Bando, K. ^{[10
]}

Barry, R. ^{[11
]}

Bennett, D.P. ^{[11
,12
]}

Bhattacharya, A. ^{[11
,12
]}

Bond, I.A. ^{[13
]}

Fukui, A. ^{[14
]}

Hamada, R. ^{[10
]}

Hamada, S. ^{[10
]}

Hamasaki, N. ^{[10
]}

Hirao, Y. ^{[15
]}

Ishitani Silva, S. ^{[11
,16
]}

Itow, Y. ^{[9
]}

Koshimoto, N. ^{[10
]}

Matsubara, Y. ^{[9
]}

Miyazaki, S. ^{[17
]}

Muraki, Y. ^{[9
]}

Nagai, T. ^{[10
]}

Nunota, K. ^{[10
]}

Olmschenk, G. ^{[11
]}

Ranc, C. ^{[18
]}

Rattenbury, N.J. ^{[19
]}

Satoh, Y. ^{[10
]}

Sumi, T. ^{[10
]}

Suzuki, D. ^{[10
]}

Tristram, P.J. ^{[20
]}

Vandorou, A. ^{[11
,12
]}

机构：

[1] Astronomical Observatory, University of Warsaw, Al. Ujazdowskie 4, Warszawa,00-478, Poland

[2] Las Cumbres Observatory, 6740 Cortona Drive, Suite 102, Goleta,CA,93117, United States

[3] Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot,76100, Israel

[4] Research School of Astronomy and Astrophysics, Australian National University, Mount Stromlo Observatory, Cotter Road, Weston Creek,ACT,2611, Australia

[5] Zentrum für Astronomie der Universität Heidelberg, Astronomisches Rechen-Institut, Mönchhofstr. 12-14, Heidelberg,69120, Germany

[6] Institute of Theoretical Physics and Astronomy, Vilnius University, Saulėtekio al. 3, Vilnius,LT-10257, Lithuania

[7] Center for Astrophysics and Cosmology, University of Nova Gorica, Vipavska 11c, Ajdovščina,SI-5270, Slovenia

[8] Department of Physics, University of Warwick, Gibbet Hill Road, Coventry,CV4 7AL, United Kingdom

[9] Institute for Space-Earth Environmental Research, Nagoya University, Nagoya,464-8601, Japan

[10] Department of Earth and Space Science, Graduate School of Science, Osaka University, Osaka, Toyonaka,560-0043, Japan

[11] Code 667, NASA Goddard Space Flight Center, Greenbelt,MD,20771, United States

[12] Department of Astronomy, University of Maryland, College Park,MD,20742, United States

[13] Institute of Natural and Mathematical Sciences, Massey University, Auckland,0745, New Zealand

[14] Department of Earth and Planetary Science, Graduate School of Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo,113-0033, Japan

[15] Institute of Astronomy, Graduate School of Science, The University of Tokyo, 2-21-1 Osawa, Mitaka, Tokyo,181-0015, Japan

[16] Oak Ridge Associated Universities, Oak Ridge,TN,37830, United States

[17] Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo, Sagamihara, Kanagawa,252-5210, Japan

[18] Sorbonne Université, CNRS, UMR 7095, Institut d'Astrophysique de Paris, 98 bis bd Arago, Paris,75014, France

[19] Department of Physics, University of Auckland, Private Bag 92019, Auckland, New Zealand

[20] University of Canterbury Mt. John Observatory, P.O. Box 56, Lake Tekapo,8770, New Zealand

来源：

Astronomy and Astrophysics | 2024年 / 692卷

基金：

欧盟地平线“2020”; 日本学术振兴会;

关键词：

Black holes - Electromagnetic wave emission - Giant stars - Gravitational effects - Microlenses;

D O I：

10.1051/0004-6361/202449322

中图分类号：

学科分类号：

摘要：

Gravitational microlensing is a phenomenon that allows us to observe the dark remnants of stellar evolution, even if these bodies are no longer emitting 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 the 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, source star, Galactic model, and the expected parameter distributions. We found eleven candidates for dark remnants: one WDs, three NSs, three mass-gap objects, and four BHs. © The Authors 2024.

引用

共 50 条

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