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26 April 2024

» arxiv » 1906.2630

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An analysis of binary microlensing event OGLE-2015-BLG-0060
Y. Tsapras ; A. Cassan ; C. Ranc ; E. Bachelet ; R. Street ; A. Udalski ; M. Hundertmark ; V. Bozza ; J. P. Beaulieu ; J. B. Marquette ; E. Euteneuer ; RoboNet team ; D. M. Bramich ; M. Dominik ; R. Figuera Jaimes ; K. Horne ; S. Mao ; J. Menzies ; R. Schmidt ; C. Snodgrass ; I. A. Steele ; J. Wambsganss ; OGLE collaboration ; P. Mróz ; M. K. Szymański ; I. Soszyński ; J. Skowron ; P. Pietrukowicz ; S. Kozłowski ; R. Poleski ; K. Ulaczyk ; M. Pawlak ; MiNDSTEp collaboration ; U. G. Jørgensen ; J. Skottfelt ; A. Popovas ; S. Ciceri ; H. Korhonen ; M. Kuffmeier ; D. F. Evans ; N. Peixinho ; T. C. Hinse ; M. J. Burgdorf ; J. Southworth ; R. Tronsgaard ; E. Kerins ; M. I. Andersen ; S. Rahvar ; Y. Wang ; O. Wertz ; M. Rabus ; S. Calchi Novati ; G. D'Ago ; G. Scarpetta ; L. Mancini ; MOA collaboration ; F. Abe ; Y. Asakura ; D. P. Bennett ; A. Bhattacharya ; M. Donachie ; P. Evans ; A. Fukui ; Y. Hirao ; Y. Itow ; K. Kawasaki ; N. Koshimoto ; M. C. A. Li ; C. H. Ling ; K. Masuda ; Y. Matsubara ; Y. Muraki ; S. Miyazaki ; M. Nagakane ; K. Ohnishi ; N. Rattenbury ; To. Saito ; A. Sharan ; H. Shibai ; D. J. Sullivan ; T. Sumi ; D. Suzuki ; P. J. Tristram ; T. Yamada ; A. Yonehara ;
Date:	6 Jun 2019
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 $M_{star1} = 0.87 pm 0.12 M_{odot}$ and $M_{star2} = 0.77 pm 0.11 M_{odot}$. The distance to the lensing system is 6.41 $pm 0.14$ kpc and the projected separation between the two components is 13.85 $pm 0.16$ AU. Alternative interpretations are also considered.
Source:	arXiv, 1906.2630
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