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The First Circumbinary Planet Found by Microlensing: OGLE-2007-BLG-349L(AB)c | | D.P. Bennett
; S.H. Rhie
; A. Udalski
; A. Gould
; Y. Tsapras
; D. Kubas
; I.A. Bond
; J. Greenhill
; A. Cassan
; N.J. Rattenbury
; T.S. Boyajian
; J. Luhn
; M.T. Penny
; J. Anderson
; F. Abe
; A. Bhattacharya
; C.S. Botzler
; M. Donachie
; M. Freeman
; A. Fukui
; Y. Hirao
; Y. Itow
; N. Koshimoto
; M.C.A. Li
; C.H. Ling
; K. Masuda
; Y. Matsubara
; Y. Muraki
; M. Nagakane
; K. Ohnishi
; H. Oyokawa
; Y.C. Perrott
; To. Saito
; A. Sharan
; D.J. Sullivan
; T. Sumi
; D. Suzuki
; P.J. Tristram
; A. Yonehara
; P.C.M. Yock
; M.K. Szymanski
; I. Soszynski
; K. Ulaczyk
; L. Wyrzykowski
; W. Allen
; D. DePoy
; A. Gal-Yam
; B.S. Gaudi
; C. Han
; I.A.G. Monard
; E. Ofek
; R.W. Pogge
; R.A. Street
; D.M. Bramich
; M. Dominik
; K. Horne
; C. Snodgrass
; I.A. Steele
; M.D. Albrow
; E. Bachelet
; V. Batista
; J.-P. Beaulieu
; S. Brillant
; J.A.R. Caldwell
; A. Cole
; C. Coutures
; S. Dieters
; D. Dominis Prester
; J. Donatowicz
; P. Fouque
; M. Hundertmark
; U.G. Jorgensen
; N. Kains
; S.R. Kane
; J.-B. Marquette
; J. Menzies
; K.R. Pollard
; C. Ranc
; K.C. Sahu
; J. Wambsganss
; A. Williams
; M. Zub
; | | Date: |
21 Sep 2016 | | 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 $q approx 3.4 imes 10^{-4}$, 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: 2-planet models
(with a single host star) and circumbinary planet models. The light curve also
reveals a significant microlensing parallax effect, which constraints the mass
of the lens system to be $M_L approx 0.7 M_odot$. Hubble Space Telescope
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
2-planet, 1-star models. So, only the circumbinary models are consistent with
the HST data. They indicate a planet of mass $m_c = 80pm 13 M_oplus$,
orbiting a pair of M-dwarfs with masses of $M_A = 0.41pm 0.07 M_odot$ and
$M_B = 0.30pm 0.07 M_odot$, which makes this the lowest mass circumbinary
planet system known. The ratio of the planet:center-of-mass separation to the
separations 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. | | Source: | arXiv, 1609.6720 | | Services: | Forum | Review | PDF | Favorites | |
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