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The first circumbinary planet found by microlensing: OGLE-2007-BLG-349L(AB)c

Citation

Bennett, DP and Rhie, SH and Udalski, A and Gould, A and Tsapras, Y and Kubas, D and Bond, IA and Greenhill, J and Cassan, A and Rattenbury, NJ and Boyajian, TS and Luhn, J and Penny, MT and Anderson, J and Abe, F and Bhattacharya, A and Botzler, CS and Donachie, M and Freeman, M and Fukui, A and Hirao, Y and Itow, Y and Koshimoto, N and Li, MCA and Ling, CH and Masuda, K and Matsubara, Y and Muraki, Y and Nagakane, M and Ohnishi, K and Oyokawa, H and Perrott, YC and Saito, T and Sharan, A and Sullivan, DJ and Sumi, T and Suzuki, D and Tristram, PJ and Yonehara, A and Yock, PCM and Szymanski, MK and Soszynski, I and Ulaczyk, K and Wyrzykowski, L and Allen, W and DePoy, D and Gal-Yam, A and Gaudi, BS and Han, C and Monard, IAG and Ofek, E and Pogge, RW and Street, RA and Bramich, DM and Dominik, M and Horne, K and Snodgrass, C and Steele, IA and Albrow, MD and Bachelet, E and Batista, V and Beaulieu, JP and Brillant, S and Caldwell, JAR and Cole, A and Coutures, C and Dieters, S and Prester, DD and Donatowicz, J and Fouque, P and Hundertmark, M and Jorgensen, UG and Kains, N and Kane, SR and Marquette, JB and Menzies, J and Pollard, KR and Ranc, C and Sahu, KC and Wambsganss, J and Williams, A and Zub, M, The first circumbinary planet found by microlensing: OGLE-2007-BLG-349L(AB)c, Astronomical Journal, 152, (5) Article 125. ISSN 0004-6256 (2016) [Refereed Article]


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Copyright 2016 The American Astronomical Society

DOI: doi:10.3847/0004-6256/152/5/125

Abstract

We present the analysis of the first circumbinary planet microlensing event, OGLE-2007-BLG-349. This event has a strong planetary signal that is best fit with a mass ratio of q ≈ 3.4 × 10-4, but there is an additional signal due to an additional lens mass, either another planet or another star. We find acceptable light-curve fits with two classes of models: two-planet models (with a single host star) and circumbinary planet models. The light curve also reveals a significant microlensing parallax effect, which constrains the mass of the lens system to be ML ≈ 0.7 M⊙. Hubble Space Telescope (HST) images resolve the lens and source stars from their neighbors and indicate excess flux due to the star(s) in the lens system. This is consistent with the predicted flux from the circumbinary models, where the lens mass is shared between two stars, but there is not enough flux to be consistent with the two-planet, one-star models. So, only the circumbinary models are consistent with the HST data. They indicate a planet of mass mc = 80 ± 13 M⊙, orbiting a pair of M dwarfs with masses of MA = 0.41 ± 0.07 and MB = 0.30 ± 0.07, which makes this the lowest-mass circumbinary planet system known. The ratio of the separation between the planet and the center of mass to the separation of the two stars is ∼40, so unlike most of the circumbinary planets found by Kepler, the planet does not orbit near the stability limit.

Item Details

Item Type:Refereed Article
Keywords:gravitational lensing: micro, planetary systems
Research Division:Physical Sciences
Research Group:Astronomical and Space Sciences
Research Field:Stellar Astronomy and Planetary Systems
Objective Division:Expanding Knowledge
Objective Group:Expanding Knowledge
Objective Field:Expanding Knowledge in the Physical Sciences
UTAS Author:Greenhill, J (Dr John Greenhill)
UTAS Author:Cole, A (Associate Professor Andrew Cole)
UTAS Author:Dieters, S (Dr Stefan Dieters)
ID Code:112824
Year Published:2016
Web of Science® Times Cited:27
Deposited By:Mathematics and Physics
Deposited On:2016-11-30
Last Modified:2017-11-03
Downloads:96 View Download Statistics

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