OGLE-2013-BLG-0102LA,B: MICROLENSING BINARY WITH COMPONENTS AT STAR/BROWN DWARF AND BROWN DWARF/PLANET BOUNDARIES

Journal Article · Sat Jan 10 00:00:00 EST 2015 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/798/2/123· OSTI ID:22364605

Jung, Y. K.; Han, C. ^[1]; Udalski, A.; Skowron, J.; Kozłowski, S.; Poleski, R.; Wyrzykowski, Ł.; Szymański, M. K.; Pietrzyński, G.; Soszyński, I.; Ulaczyk, K.; Pietrukowicz, P.; Mróz, P.; Kubiak, M. ^[2]; Sumi, T. ^[3]; Gould, A. ^[4]; Abe, F. ^[5]; Bennett, D. P. ^[6]; Bond, I. A. ^[7]; others, and

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1. Department of Physics, Chungbuk National University, Cheongju 371-763 (Korea, Republic of)
2. Warsaw University Observatory, Al. Ujazdowskie 4, 00-478 Warszawa (Poland)
3. Department of Earth and Space Science, Osaka University, Osaka 560-0043 (Japan)
4. Department of Astronomy, Ohio State University, 140 West 18th Avenue, Columbus, OH 43210 (United States)
5. Solar-Terrestrial Environment Laboratory, Nagoya University, Nagoya 464-8601 (Japan)
6. Department of Physics, University of Notre Dame, 225 Nieuwland Science Hall, Notre Dame, IN 46556-5670 (United States)
7. Institute of Information and Mathematical Sciences, Massey University, Private Bag 102-904, North Shore Mail Centre, Auckland (New Zealand)

We present an analysis of the gravitational microlensing event OGLE-2013-BLG-0102. The light curve of the event is characterized by a strong short-term anomaly superposed on a smoothly varying lensing curve with a moderate magnification A {sub max} ∼ 1.5. It is found that the event was produced by a binary lens with a mass ratio between the components of q = 0.13 and the anomaly was caused by the passage of the source trajectory over a caustic located away from the barycenter of the binary. Based on the analysis of the effects on the light curve due to the finite size of the source and the parallactic motion of the Earth, we determine the physical parameters of the lens system. The measured masses of the lens components are M {sub 1} = 0.096 ± 0.013 M {sub ☉} and M {sub 2} = 0.012 ± 0.002 M {sub ☉}, which correspond to near the hydrogen-burning and deuterium-burning mass limits, respectively. The distance to the lens is 3.04 ± 0.31 kpc and the projected separation between the lens components is 0.80 ± 0.08 AU.

• OSTI ID: 22364605
• Journal Information: Astrophysical Journal, Vol. 798, Issue 2; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
BINARY STARS
DEUTERIUM
DIAGRAMS
DISTANCE
DWARF STARS
GRAVITATIONAL LENSES
HYDROGEN BURNING
MASS
PLANETS
TRAJECTORIES
VISIBLE RADIATION