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. Szymański; I. Soszyński; K. Ulaczyk; Ł. 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. Fouqué; M. Hundertmark; U. G. Jørgensen; N. Kains; S. R. Kane; J.-B. Marquette; J. Menzies; K. R. Pollard; C. Ranc; K. C. Sahu; J. Wambsganss; A. Williams; M. Zub

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

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. FukuiY. 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. Szymański, I. Soszyński, K. Ulaczyk, Ł. 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. Fouqué, M. Hundertmark, U. G. Jørgensen, N. Kains, S. R. Kane, J.-B. Marquette, J. Menzies, K. R. Pollard, C. Ranc, K. C. Sahu, J. Wambsganss, A. Williams, M. Zub

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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 M_L ≈0.7 M_sun. 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 m_c = 80 ± 13 M_earth, orbiting a pair of M dwarfs with masses of M_A = 0.41 ± 0.07 and M_B = 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.

Original language	English
Article number	125
Number of pages	14
Journal	Astronomical Journal
Volume	152
Issue number	5
Early online date	21 Oct 2016
DOIs	https://doi.org/10.3847/0004-6256/152/5/125
Publication status	Published - Nov 2016

Keywords

Gravitational lensing: micro
Planetary systems

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10.3847/0004-6256/152/5/125

Bennett_2016_AJ_152_125
© 2016, Astronomical Society of America. This work has been made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at iopscience.iop.org / http://dx.doi.org/10.3847/0004-6256/152/5/125
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Bennett, D. P., Rhie, S. H., Udalski, A., Gould, A., Tsapras, Y., Kubas, D., Bond, I. A., Greenhill, J., Cassan, A., Rattenbury, N. J., Boyajian, T. S., Luhn, J., Penny, M. T., Anderson, J., Abe, F., Bhattacharya, A., Botzler, C. S., Donachie, M., Freeman, M., ... Zub, M. (2016). The first circumbinary planet found by microlensing: OGLE-2007-BLG-349L(AB)c. Astronomical Journal, 152(5), Article 125. https://doi.org/10.3847/0004-6256/152/5/125

@article{fb07d4e5cc9b4f1aa3c40842ab5953c7,

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

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\_sun. 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\_earth, 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.",

keywords = "Gravitational lensing: micro, Planetary systems",

author = "Bennett, \{D. P.\} and Rhie, \{S. H.\} and A. Udalski and A. Gould and Y. Tsapras and D. Kubas and Bond, \{I. A.\} and J. Greenhill and A. Cassan and Rattenbury, \{N. J.\} and Boyajian, \{T. S.\} and J. Luhn and Penny, \{M. T.\} and J. Anderson and F. Abe and A. Bhattacharya and Botzler, \{C. S.\} and M. Donachie and M. Freeman and A. Fukui and Y. Hirao and Y. Itow and N. Koshimoto and Li, \{M. C. A.\} and Ling, \{C. H.\} and K. Masuda and Y. Matsubara and Y. Muraki and M. Nagakane and K. Ohnishi and H. Oyokawa and Perrott, \{Y. C.\} and To. Saito and A. Sharan and Sullivan, \{D. J.\} and T. Sumi and D. Suzuki and Tristram, \{P. J.\} and A. Yonehara and Yock, \{P. C. M.\} and Szyma{\'n}ski, \{M. K.\} and I. Soszy{\'n}ski and K. Ulaczyk and {\L}. Wyrzykowski and W. Allen and D. DePoy and A. Gal-Yam and Gaudi, \{B. S.\} and C. Han and Monard, \{I. A. G.\} and E. Ofek and Pogge, \{R. W.\} and Street, \{R. A.\} and Bramich, \{D. M.\} and M. Dominik and K. Horne and C. Snodgrass and Steele, \{I. A.\} and Albrow, \{M. D.\} and E. Bachelet and V. Batista and J.-P. Beaulieu and S. Brillant and Caldwell, \{J. A. R.\} and A. Cole and C. Coutures and S. Dieters and \{Dominis Prester\}, D. and J. Donatowicz and P. Fouqu{\'e} and M. Hundertmark and J{\o}rgensen, \{U. G.\} and N. Kains and Kane, \{S. R.\} and J.-B. Marquette and J. Menzies and Pollard, \{K. R.\} and C. Ranc and Sahu, \{K. C.\} and J. Wambsganss and A. Williams and M. Zub",

year = "2016",

month = nov,

doi = "10.3847/0004-6256/152/5/125",

language = "English",

volume = "152",

journal = "Astronomical Journal",

issn = "0004-6256",

publisher = "American Astronomical Society",

number = "5",

}

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, Szymański, MK, Soszyński, I, Ulaczyk, K, Wyrzykowski, Ł, 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, Beaulieu, J-P, Brillant, S, Caldwell, JAR, Cole, A, Coutures, C, Dieters, S, Dominis Prester, D, Donatowicz, J, Fouqué, P, Hundertmark, M, Jørgensen, UG, Kains, N, Kane, SR, Marquette, J-B, Menzies, J, Pollard, KR, Ranc, C, Sahu, KC, Wambsganss, J, Williams, A & Zub, M 2016, 'The first circumbinary planet found by microlensing: OGLE-2007-BLG-349L(AB)c', Astronomical Journal, vol. 152, no. 5, 125. https://doi.org/10.3847/0004-6256/152/5/125

TY - JOUR

T1 - The first circumbinary planet found by microlensing: OGLE-2007-BLG-349L(AB)c

AU - Bennett, D. P.

AU - Rhie, S. H.

AU - Udalski, A.

AU - Gould, A.

AU - Tsapras, Y.

AU - Kubas, D.

AU - Bond, I. A.

AU - Greenhill, J.

AU - Cassan, A.

AU - Rattenbury, N. J.

AU - Boyajian, T. S.

AU - Luhn, J.

AU - Penny, M. T.

AU - Anderson, J.

AU - Abe, F.

AU - Bhattacharya, A.

AU - Botzler, C. S.

AU - Donachie, M.

AU - Freeman, M.

AU - Fukui, A.

AU - Hirao, Y.

AU - Itow, Y.

AU - Koshimoto, N.

AU - Li, M. C. A.

AU - Ling, C. H.

AU - Masuda, K.

AU - Matsubara, Y.

AU - Muraki, Y.

AU - Nagakane, M.

AU - Ohnishi, K.

AU - Oyokawa, H.

AU - Perrott, Y. C.

AU - Saito, To.

AU - Sharan, A.

AU - Sullivan, D. J.

AU - Sumi, T.

AU - Suzuki, D.

AU - Tristram, P. J.

AU - Yonehara, A.

AU - Yock, P. C. M.

AU - Szymański, M. K.

AU - Soszyński, I.

AU - Ulaczyk, K.

AU - Wyrzykowski, Ł.

AU - Allen, W.

AU - DePoy, D.

AU - Gal-Yam, A.

AU - Gaudi, B. S.

AU - Han, C.

AU - Monard, I. A. G.

AU - Ofek, E.

AU - Pogge, R. W.

AU - Street, R. A.

AU - Bramich, D. M.

AU - Dominik, M.

AU - Horne, K.

AU - Snodgrass, C.

AU - Steele, I. A.

AU - Albrow, M. D.

AU - Bachelet, E.

AU - Batista, V.

AU - Beaulieu, J.-P.

AU - Brillant, S.

AU - Caldwell, J. A. R.

AU - Cole, A.

AU - Coutures, C.

AU - Dieters, S.

AU - Dominis Prester, D.

AU - Donatowicz, J.

AU - Fouqué, P.

AU - Hundertmark, M.

AU - Jørgensen, U. G.

AU - Kains, N.

AU - Kane, S. R.

AU - Marquette, J.-B.

AU - Menzies, J.

AU - Pollard, K. R.

AU - Ranc, C.

AU - Sahu, K. C.

AU - Wambsganss, J.

AU - Williams, A.

AU - Zub, M.

PY - 2016/11

Y1 - 2016/11

N2 - 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_sun. 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_earth, 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.

AB - 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_sun. 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_earth, 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.

KW - Gravitational lensing: micro

KW - Planetary systems

UR - https://www.scopus.com/pages/publications/84994519967

U2 - 10.3847/0004-6256/152/5/125

DO - 10.3847/0004-6256/152/5/125

M3 - Article

SN - 0004-6256

VL - 152

JO - Astronomical Journal

JF - Astronomical Journal

IS - 5

M1 - 125

ER -

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

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Astronomy at St Andrews 2015-2018: Astronomy at St Andrews 2015-2018

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

Abstract

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Astronomy at St Andrews 2015-2018: Astronomy at St Andrews 2015-2018

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