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Tsapras, Y, Cassan, A, Ranc, C, Bachelet, E, Street, R, Udalski, A, Hundertmark, M, Bozza, V, Beaulieu, JP, Marquette, JB, Euteneuer, E, Bramich, DM, Dominik, M, Figuera Jaimes, R, Horne, K, Mao, S, Menzies, J, Schmidt, R, Snodgrass, C, Steele, IA, Wambsganss, J, Mróz, P, Szymański, MK, Soszyński, I, Skowron, J, Pietrukowicz, P, Kozłowski, S, Poleski, R, Ulaczyk, K, Pawlak, M, Jørgensen, UG, Skottfelt, J, Popovas, A, Ciceri, S, Korhonen, H, Kuffmeier, M, Evans, DF, Peixinho, N, Hinse, TC, Burgdorf, MJ, Southworth, J, Tronsgaard, R, Kerins, E, Andersen, MI, Rahvar, S, Wang, Y, Wertz, O, Rabus, M, Calchi Novati, S, D’Ago, G, Scarpetta, G, Mancini, L, Abe, F, Asakura, Y, Bennett, DP, Bhattacharya, A, Donachie, M, Evans, P, Fukui, A, Hirao, Y, Itow, Y, Kawasaki, K, Koshimoto, N, Li, MCA, Ling, CH, Masuda, K, Matsubara, Y, Muraki, Y, Miyazaki, S, Nagakane, M, Ohnishi, K, Rattenbury, N, Saito, T, Sharan, A, Shibai, H, Sullivan, DJ, Sumi, T, Suzuki, D, Tristram, PJ, Yamada, T, Yonehara, A, team, TR, collaboration, TOGLE, collaboration, TM and collaboration, TMOA (2019) An analysis of binary microlensing event OGLE-2015-BLG-0060. Monthly Notices of the Royal Astronomical Society, 487 (4). 4603 - 4614. ISSN 0035-8711

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Abstract

We present the analysis of stellar binary microlensing event OGLE-2015-BLG-0060 based on observations obtained from 13 different telescopes. Intensive coverage of the anomalous parts of the light curve was achieved by automated follow-up observations from the robotic telescopes of the Las Cumbres Observatory. We show that, for the first time, all main features of an anomalous microlensing event are well covered by follow-up data, allowing us to estimate the physical parameters of the lens. The strong detection of second-order effects in the event light curve necessitates the inclusion of longer-baseline survey data in order to constrain the parallax vector. We find that the event was most likely caused by a stellar binary-lens with masses $M_\star 1 = 0.87 \pm 0.12 \, \mathrmM_ødot $ and $M_\star 2 = 0.77 \pm 0.11 \, \mathrmM_ødot $. The distance to the lensing system is 6.41 ± 0.14 kpc and the projected separation between the two components is 13.85 ± 0.16 au. Alternative interpretations are also considered.

Item Type: Article
Additional Information: This is the final published version of the article (version of record). It first appeared online via Oxford University Press at https://doi.org/10.1093/mnras/stz1404 - please refer to any applicable terms of use of the publisher.
Uncontrolled Keywords: gravitational lensing, micro, methods, observational, techniques, photometric, Galaxy, bulge
Subjects: Q Science > QB Astronomy > QB799 Stars
Divisions: Faculty of Natural Sciences > School of Chemical and Physical Sciences
Depositing User: Symplectic
Date Deposited: 02 Aug 2019 08:55
Last Modified: 13 Aug 2019 10:51
URI: https://eprints.keele.ac.uk/id/eprint/6614

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