Li, S-S, Zang, W, Udalski, A, Shvartzvald, Y, Huber, D, Lee, C-U, Sumi, T, Gould, A, Mao, S, Fouque, P, Wang, T, Dong, S, Jorgensen, UG, Cole, A, Mroz, P, Szymanski, MK, Skowron, J, Poleski, R, Soszynski, I, Pietrukowicz, P, Kozlowski, S, Ulaczyk, K, Rybicki, KA, Iwanek, P, Yee, JC, Novati, SC, Beichman, CA, Bryden, G, Carey, S, Gaudi, BS, Henderson, CB, Zhu, W, Albrow, MD, Chung, S-J, Han, C, Hwang, K-H, Jung, YK, Ryu, Y-H, Shin, I-G, Cha, S-M, Kim, D-J, Kim, H-W, Kim, S-L, Lee, D-J, Lee, Y, Park, B-G, Pogge, RW, Bond, IA, Abe, F, Barry, R, Bennett, DP, Bhattacharya, A, Donachie, M, Fukui, A, Hirao, Y, Itow, Y, Kondo, I, Koshimoto, N, Li, MCA, Matsubara, Y, Muraki, Y, Miyazaki, S, Nagakane, M, Ranc, C, Rattenbury, NJ, Suematsu, H, Sullivan, DJ, Suzuki, D, Tristram, PJ, Yonehara, A, Christie, G, Drummond, J, Green, J, Hennerley, S, Natusch, T, Porritt, I, Bachelet, E, Maoz, D, Street, RA, Tsapras, Y, Bozza, V, Dominik, M, Hundertmark, M, Peixinho, N, Sajadian, S, Burgdorf, MJ, Evans, DF, Jaimes, RF, Fujii, YI, Haikala, LK, Helling, C, Henning, T, Hinse, TC, Mancini, L, Longa-Pena, P, Rahvar, S, Rabus, M, Skottfelt, J, Snodgrass, C, Southworth, J, Unda-Sanzana, E, von Essen, C, Beaulieu, J-P, Blackman, J and Hill, K (2019) OGLE-2017-BLG-1186: first application of asteroseismology and Gaussian processes to microlensing. Monthly Notices of the Royal Astronomical Society, 488 (3). 3308 - 3323. ISSN 1365-2966

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We present the analysis of the event OGLE-2017-BLG-1186 from the 2017 Spitzer microlensing campaign. This is a remarkable microlensing event because its source is photometrically bright and variable, which makes it possible to perform an asteroseismic analysis using ground-based data. We find that the source star is an oscillating red giant with average time-scale of ∼9 d. The asteroseismic analysis also provides us source properties including the source angular size (∼27 μas) and distance (∼11.5 kpc), which are essential for inferring the properties of the lens. When fitting the light curve, we test the feasibility of Gaussian processes (GPs) in handling the correlated noise caused by the variable source. We find that the parameters from the GP model are generally more loosely constrained than those from the traditional χ2 minimization method. We note that this event is the first microlensing system for which asteroseismology and GPs have been used to account for the variable source. With both finite-source effect and microlens parallax measured, we find that the lens is likely a ∼0.045 M⊙ brown dwarf at distance ∼9.0 kpc, or a ∼0.073 M⊙ ultracool dwarf at distance ∼9.8 kpc. Combining the estimated lens properties with a Bayesian analysis using a Galactic model, we find a ∼35 per cent probability for the lens to be a bulge object and ∼65 per cent to be a background disc object.

Item Type: Article
Uncontrolled Keywords: asteroseismology, gravitational lensing, micro, stars, fundamental parameters, oscillations
Subjects: Q Science > QB Astronomy > QB799 Stars
Divisions: Faculty of Natural Sciences > School of Chemical and Physical Sciences
Related URLs:
Depositing User: Symplectic
Date Deposited: 04 Oct 2019 09:47
Last Modified: 26 Feb 2021 15:01

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