Bibcode
Bachelet, E.; Tsapras, Y.; Gould, Andrew; Street, R. A.; Bennett, David P.; Hundertmark, M. P. G.; Bozza, V.; Bramich, D. M.; Cassan, A.; Dominik, M.; Horne, K.; Mao, S.; Saha, A.; Wambsganss, J.; Zang, Weicheng; ROME/REA Collaboration; Abe, Fumio; Barry, Richard; Bennett, David P.; Bhattacharya, Aparna; Bond, Ian A.; Fukui, Akihiko; Fujii, Hirosane; Hirao, Yuki; Itow, Yoshitaka; Kirikawa, Rintaro; Kondo, Iona; Koshimoto, Naoki; Matsubara, Yutaka; Matsumoto, Sho; Miyazaki, Shota; Muraki, Yasushi; Olmschenk, Greg; Ranc, Clément; Okamura, Arisa; Rattenbury, Nicholas J.; Satoh, Yuki; Sumi, Takahiro; Suzuki, Daisuke; Silva, Stela Ishitani; Toda, Taiga; Tristram, Paul. J.; Vandorou, Aikaterini; Yama, Hibiki; MOA Collaboration; Albrow, Michael D.; Chung, Sun-Ju; Han, Cheongho; Hwang, Kyu-Ha; Jung, Youn Kil; Ryu, Yoon-Hyun; Shin, In-Gu; Shvartzvald, Yossi; Yee, Jennifer C.; Cha, Sang-Mok; Kim, Dong-Jin; Kim, Seung-Lee; Lee, Chung-Uk; Lee, Dong-Joo; Lee, Yongseok; Park, Byeong-Gon; Pogge, Richard W.; KMTNet Collaboration; Udalski, Andrzej; Mróz, Przemek; Poleski, Radosław; Skowron, Jan; Szymański, Michał K.; Soszyński, Igor; Pietrukowicz, Paweł; Kozłowski, Szymon; Ulaczyk, Krzysztof; Rybicki, Krzysztof A.; Iwanek, Patryk; Wrona, Marcin; Gromadzki, Mariusz; OGLE Collaboration
Referencia bibliográfica
The Astronomical Journal
Fecha de publicación:
9
2022
Número de citas
3
Número de citas referidas
2
Descripción
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 θ E cannot be measured from the light curve alone. However, the large event duration, t E ~ 80 days, allows a precise measurement of the microlensing parallax π E. In addition to the constraints on the angular radius θ * and the apparent brightness I s of the source, we employ the Besançon 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 M p ~ 30 M Jup, 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 ≤4 kpc. We estimate that in about 10 yr 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.