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

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posted on 2023-05-18, 23:58 authored by Bennett, DP, Rhie, SH, Udalski, A, Gould, A, Tsapras, Y, Kubas, D, Bond, IA, Greenhill, J, Cassan, A, Rattenbury, NJ, Boyajian, TS, Luhn, J, Penny, MT, Anderson, J, Abe, F, Bhattacharya, A, Botzler, CS, Donachie, M, Freeman, M, Fukui, A, Hirao, Y, Itow, Y, Koshimoto, N, Li, MCA, Ling, CH, Masuda, K, Matsubara, Y, Muraki, Y, Nagakane, M, Ohnishi, K, Oyokawa, H, Perrott, YC, Saito, T, Sharan, A, Sullivan, DJ, Sumi, T, Suzuki, D, Tristram, PJ, Yonehara, A, Yock, PCM, Szymanski, MK, Soszynski, I, Ulaczyk, K, Wyrzykowski, L, Allen, W, DePoy, D, Gal-Yam, A, Gaudi, BS, Han, C, Monard, IAG, Ofek, E, Pogge, RW, Street, RA, Bramich, DM, Dominik, M, Horne, K, Snodgrass, C, Steele, IA, Albrow, MD, Bachelet, E, Batista, V, Jean-Philippe BeaulieuJean-Philippe Beaulieu, Brillant, S, Caldwell, JAR, Andrew ColeAndrew Cole, Coutures, C, Dieters, S, Prester, DD, Donatowicz, J, Fouque, P, Hundertmark, M, Jorgensen, UG, Kains, N, Kane, SR, Marquette, JB, Menzies, J, Pollard, KR, Ranc, C, Sahu, KC, Wambsganss, J, Williams, A, Zub, M
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.

History

Publication title

Astronomical Journal

Volume

152

Issue

5

Article number

125

Number

125

Pagination

1-14

ISSN

0004-6256

Department/School

School of Natural Sciences

Publisher

Univ Chicago Press

Place of publication

1427 E 60Th St, Chicago, USA, Il, 60637-2954

Rights statement

Copyright 2016 The American Astronomical Society

Repository Status

  • Open

Socio-economic Objectives

Expanding knowledge in the physical sciences

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