OGLE-2014-BLG-1186: gravitational microlensing providing evidence for a planet orbiting the foreground star or for a close binary source?. Issue 4 (29th January 2019)

• Record Type: Journal Article
• Authors: Dominik, M; Bachelet, E; Bozza, V; Street, R A; Han, C; Hundertmark, M; Udalski, A; Bramich, D M; Alsubai, K A; Calchi Novati, S; Ciceri, S; D'Ago, G; Figuera Jaimes, R; Haugbølle, T; Hinse, T C; Horne, K; Jørgensen, U G; Juncher, D; Kains, N; Korhonen, H; Mancini, L; Menzies, J; Popovas, A; Rabus, M; Rahvar, S; Scarpetta, G; Schmidt, R; Skottfelt, J; Snodgrass, C; Southworth, J; Starkey, D; Steele, I A; Surdej, J; Tsapras, Y; Wambsganss, J; Wertz, O; Pietrukowicz, P; Szymański, M K; Mróz, P; Skowron, J; Soszyński, I; Ulaczyk, K; Poleski, R; Wyrzykowski, Ł; Kozłowski, S;
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 484:Issue 4(2019)
• Page Start: 5608
• Page End: 5632
• Publication Date: 2019-01-29
• Subjects: gravitational lensing: micro -- methods: data analysis -- methods: statistical -- planets and satellites: detection -- (stars:) binaries: eclipsing -- Galaxy: kinematics and dynamics; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/stz306
• Languages: English
• ISSNs: 0035-8711

Abstract

ABSTRACT: Discussing the particularly long gravitational microlensing event OGLE-2014-BLG-1186 with a time-scale t E ∼ 300 d, we present a methodology for identifying the nature of localised deviations from single-lens point-source light curves, which ensures that (1) the claimed signal is substantially above the noise floor, (2) the inferred properties are robustly determined and their estimation is not subject to confusion with systematic noise in the photometry, (3) alternative viable solutions within the model framework are not missed. Annual parallax and binarity could be separated and robustly measured from the wing and the peak data, respectively. We find matching model light curves that involve either a binary lens or a binary source, and discover hitherto unknown model ambiguities. Our binary-lens models indicate a planet of mass M 2 = (45 ± 9) M⊕, orbiting a star of mass M 1 = (0.35 ± 0.06) M⊙, located at a distance D L = (1.7 ± 0.3) kpc from Earth, whereas our binary-source models suggest a brown-dwarf lens of M = (0.046 ± 0.007) M⊙, located at a distance D L = (5.7 ± 0.9) kpc, with the source potentially being a (partially) eclipsing binary involving stars predicted to be of similar colour given the ratios between the luminosities and radii. Further observations might resolve the ambiguity in the interpretation in favour of either a lens or a source binary. We experienced that close binary source stars pose a challenge for claiming the detection of planets by microlensing in events where the source passes very close to the lens star hosting the planet.