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OGLE-2014-BLG-0289: Precise Characterization of a Quintuple-peak Gravitational Microlensing Event
journal contribution
posted on 2019-08-30, 08:36 authored by A Udalski, C Han, V Bozza, A Gould, IA Bond, P Mróz, J Skowron, Wyrzykowski, MK Szymański, I Soszyński, K Ulaczyk, R Poleski, P Pietrukowicz, S Kozłowski, F Abe, R Barry, DP Bennett, A Bhattacharya, M Donachie, P Evans, A Fukui, Y Hirao, Y Itow, K Kawasaki, N Koshimoto, MCA Li, CH Ling, K Masuda, Y Matsubara, S Miyazaki, H Munakata, Y Muraki, M Nagakane, K Ohnishi, C Ranc, N Rattenbury, T Saito, A Sharan, DJ Sullivan, T Sumi, D Suzuki, PJ Tristram, T Yamada, A Yonehara, E Bachelet, DM Bramich, G DÁgo, M Dominik, RF Jaimes, K Horne, M Hundertmark, N Kains, J Menzies, R Schmidt, C Snodgrass, IA Steele, J Wambsganss, RW Pogge, YK Jung, IG Shin, JC Yee, WT Kim, C Beichman, S Carey, SC Novati, W ZhuWe present the analysis of the binary-microlensing event OGLE-2014-BLG-0289. The event light curve exhibits five very unusual peaks, four of which were produced by caustic crossings and the other by a cusp approach. It is found that the quintuple-peak features of the light curve provide tight constraints on the source trajectory, enabling us to precisely and accurately measure the microlensing parallax πE. Furthermore, the three resolved caustics allow us to measure the angular Einstein radius θE. From the combination of πEand θE, the physical lens parameters are uniquely determined. It is found that the lens is a binary composed of two M dwarfs with masses M1= 0.52 ± 0.04 Moand M2= 0.42 ± 0.03 Moseparated in projection by aτ = 6.4 ± 0.5 au. The lens is located in the disk with a distance of DL= 3.3 ± 0.3 kpc. The reason for the absence of a lensing signal in the Spitzer data is that the time of observation corresponds to the flat region of the light curve.
Funding
Work by C. Han was supported by the grant (2017R1A4A1015178) of National Research Foundation of Korea. The OGLE project has received funding from the National Science Centre, Poland, grant MAESTRO 2014/14/A/ST9/00121 to A. Udalski. OGLE Team thanks Profs. M. Kubiak and G. Pietrzyński for their contribution to the OGLE photometric data set presented in this paper. The MOA project is supported by JSPS KAKENHI grant Nos. JSPS24253004, JSPS26247023, JSPS23340064, JSPS15H00781, and JP16H06287. Work by A. Gould was supported by JPL grant 1500811. Work by J. C. Yee was performed in part under contract with the California Institute of Technology (Caltech)/Jet Propulsion Laboratory (JPL) funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. We acknowledge the high-speed internet service (KREONET) provided by Korea Institute of Science and Technology Information (KISTI). Software: OGLE pipeline (Woźniak 2000; Udalski 2003), MOA pipeline (Bond et al. 2001), the DANDIA pipeline (Bramich 2008), pySIS (Albrow et al. 2009), DoPHOT (Schechter et al. 1993).
History
Citation
Astrophysical Journal, 2018, 853 (1)Author affiliation
/Organisation/COLLEGE OF SCIENCE AND ENGINEERING/Department of Physics and AstronomyVersion
- VoR (Version of Record)
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Astrophysical JournalPublisher
American Astronomical Society, IOP Publishingissn
0004-637Xeissn
1538-4357Acceptance date
2017-12-11Copyright date
2018Available date
2019-08-30Publisher DOI
Publisher version
https://iopscience.iop.org/article/10.3847/1538-4357/aaa295Language
enAdministrator link
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