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An analysis of binary microlensing event OGLE-2015-BLG-0060

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, Jaimes, RF, Horne, K, Mao, S, Menzies, J, Schmidt, R, Snodgrass, C, Steele, IA , Wambsganss, J, Mroz, P, Szymanski, MK, Soszynski, I, Skowron, J, Pietrukowicz, P, Kozlowski, S, Poleski, R, Ulaczyk, K, Pawlak, M, Jorgensen, 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, Novati, SC, 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 and Yonehara, A (2019) An analysis of binary microlensing event OGLE-2015-BLG-0060. Monthly Notices of the Royal Astronomical Society, 487 (4). pp. 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 ⋆1 =0.87±0.12M ⊙ and M ⋆2 =0.77±0.11M ⊙. 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 article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2019 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
Uncontrolled Keywords: 0201 Astronomical and Space Sciences
Subjects: Q Science > QB Astronomy
Q Science > QC Physics
Divisions: Astrophysics Research Institute
Publisher: Oxford University Press
Related URLs:
Date Deposited: 06 Aug 2019 09:54
Last Modified: 06 Aug 2019 10:00
DOI or Identification number: 10.1093/mnras/stz1404
URI: http://researchonline.ljmu.ac.uk/id/eprint/11145

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