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Udalski, A, Han, C, Bozza, V, Gould, A, Bond, IA, Mroz, P, Skowron, J, Wyrzykowski, L, Szymanski, MK, Soszynski, I, Ulaczyk, K, Poleski, R, Pietrukowicz, P, Kozlowski, S, Abe, F, Barry, R, 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, Miyazaki, S, Munakata, H, Muraki, Y, Nagakane, M, Ohnishi, K, Ranc, C, Rattenbury, N, Saito, T, Sharan, A, Sullivan, DJ, Sumi, T, Suzuki, D, Tristram, PJ, Yamada, T, Yonehara, A, Bachelet, E, Bramich, DM, DAgo, G, Dominik, M, Jaimes, RF, Horne, K, Hundertmark, M, Kains, N, Menzies, J, Schmidt, R, Snodgrass, C, Steele, IA, Wambsganss, J, Pogge, RW, Jung, YK, Shin, I-G, Yee, JC, Kim, W-T, Beichman, C, Carey, S, Novati, SC and Zhu, W (2018) OGLE-2014-BLG-0289: Precise Characterization of a Quintuple-peak Gravitational Microlensing Event. Astrophysical Journal, 853 (1). ISSN 0004-637X
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OGLE-2014-BLG-0289 Precise Characterization of a Quintuple-peak Gravitational Microlensing Event.pdf - Accepted Version Download (1MB) | Preview |
Abstract
We 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 ${\pi }_{{\rm{E}}}$. Furthermore, the three resolved caustics allow us to measure the angular Einstein radius ${\theta }_{{\rm{E}}}$. From the combination of ${\pi }_{{\rm{E}}}$ and ${\theta }_{{\rm{E}}}$, the physical lens parameters are uniquely determined. It is found that the lens is a binary composed of two M dwarfs with masses ${M}_{1}=0.52\pm 0.04\ {M}_{\odot }$ and ${M}_{2}=0.42\pm 0.03\ {M}_{\odot }$ separated in projection by ${a}_{\perp }=6.4\pm 0.5\,\mathrm{au}$. The lens is located in the disk with a distance of ${D}_{{\rm{L}}}=3.3\pm 0.3\,\mathrm{kpc}$. 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.
| Item Type: | Article |
|---|---|
| Uncontrolled Keywords: | 0201 Astronomical And Space Sciences, 0305 Organic Chemistry, 0306 Physical Chemistry (Incl. Structural) |
| Subjects: | Q Science > QB Astronomy Q Science > QC Physics |
| Divisions: | Astrophysics Research Institute |
| Publisher: | American Astronomical Society; IOP Publishing |
| Related URLs: | |
| Date Deposited: | 23 Mar 2018 12:37 |
| Last Modified: | 04 Sep 2021 10:37 |
| DOI or ID number: | 10.3847/1538-4357/aaa295 |
| URI: | https://researchonline.ljmu.ac.uk/id/eprint/8362 |
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