| Authors |
Kruszyńska, K ; Wyrzykowski, L ; Rybicki, K. A ; Howil, K ; Jablońska, M ; Kaczmarek, Z ; Ihanec, N ; Maskoliūnas, Marius ; Bronikowski, M ; Pylypenko, U ; Udalski, A ; Mróz, P ; Poleski, R ; Skowron, J ; Szymański, M. K ; Soszyński, I ; Pietrukowicz, P ; Kozlowski, S ; Ulaczyk, K ; Iwanek, P ; Wrona, M ; Gromadzki, M ; Mróz, M. J ; Abe, F ; Bando, K ; Barry, R ; Bennett, D. P ; Bhattacharya, A ; Bond, I. A ; Fukui, A ; Hamada, R ; Hamada, S ; Hamasaki, N ; Hirao, Y ; Ishitani Silva, S ; Itow, Y ; Koshimoto, N ; Matsubara, Y ; Miyazaki, S ; Muraki, Y ; Nagai, T ; Nunota, K ; Olmschenk, G ; Ranc, C ; Rattenbury, N. J ; Satoh, Y ; Sumi, T ; Suzuki, D ; Tristram, P. J ; Vandorou, A ; Yama, H |
| Abstract [eng] |
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. |
