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Dominik, M, Bachelet, E, Bozza, V, Street, RA, Han, C, Hundertmark, M, Udalski, A, Bramich, DM, Alsubai, KA, Novati, SC, Ciceri, S, D'Ago, G, Jaimes, RF, Haugbolle, T, Hinse, TC, Horne, K, Jorgensen, UG, 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, IA, Surdej, J, Tsapras, Y, Wambsganss, J, Wertz, O, Pietrukowicz, P, Szymanski, MK, Mroz, P, Skowron, J, Soszynski, I, Ulaczyk, K, Poleski, R, Wyrzykowski, L and Kozlowski, S (2019) OGLE-2014-BLG-1186: gravitational microlensing providing evidence for a planet orbiting the foreground star or for a close binary source? Monthly Notices of the Royal Astronomical Society, 484 (4). pp. 5608-5632. ISSN 0035-8711
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OGLE-2014-BLG-1186 gravitational microlensing providing evidence for a planet orbiting the foreground star or for a close binary source.pdf - Published Version Download (6MB) | Preview |
Abstract
Discussing the particularly long gravitational microlensing event OGLE-2014-BLG-1186 with a time-scale tE ∼ 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 M2 = (45 ± 9) M⊕, orbiting a star of mass M1 = (0.35 ± 0.06) M⊙, located at a distance DL = (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 DL = (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.
| Item Type: | Article |
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| Additional Information: | This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2019 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. |
| Uncontrolled Keywords: | 0201 Astronomical and Space Sciences |
| Subjects: | Q Science > QB Astronomy Q Science > QC Physics |
| Divisions: | Astrophysics Research Institute |
| Publisher: | Oxford University Press |
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| Date Deposited: | 06 Aug 2019 10:28 |
| Last Modified: | 04 Sep 2021 09:03 |
| DOI or ID number: | 10.1093/mnras/stz306 |
| URI: | https://researchonline.ljmu.ac.uk/id/eprint/11149 |
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