MOA-2009-BLG-387Lb

A massive planet orbiting an M dwarf

V. Batista, A. Gould, S. Dieters, S. Dong, I. Bond, J. P. Beaulieu, D. Maoz, B. Monard, G. W. Christie, J. McCormick, M. D. Albrow, K. Horne, Y. Tsapras, M. J. Burgdorf, S. Calchi Novati, J. Skottfelt, J. Caldwell, S. Kozłowski, D. Kubas, B. S. Gaudi & 115 others C. Han, D. P. Bennett, J. An, F. Abe, C. S. Botzler, D. Douchin, M. Freeman, A. Fukui, K. Furusawa, J. B. Hearnshaw, S. Hosaka, Y. Itow, K. Kamiya, P. M. Kilmartin, A. Korpela, W. Lin, C. H. Ling, S. Makita, K. Masuda, Y. Matsubara, N. Miyake, Y. Muraki, M. Nagaya, K. Nishimoto, K. Ohnishi, T. Okumura, Y. C. Perrott, N. Rattenbury, To Saito, D. J. Sullivan, T. Sumi, W. L. Sweatman, P. J. Tristram, E. Von Seggern, P. C M Yock, S. Brillant, J. J. Calitz, A. Cassan, A. Cole, K. Cook, C. Coutures, D. Dominis Prester, J. Donatowicz, J. Greenhill, M. Hoffman, F. Jablonski, S. R. Kane, N. Kains, J. B. Marquette, R. Martin, E. Martioli, P. Meintjes, J. Menzies, E. Pedretti, K. Pollard, K. C. Sahu, C. Vinter, J. Wambsganss, R. Watson, A. Williams, M. Zub, W. Allen, G. Bolt, M. Bos, D. L. Depoy, J. Drummond, J. D. Eastman, A. Gal-Yam, E. Gorbikov, D. Higgins, J. Janczak, S. Kaspi, C. U. Lee, F. Mallia, A. Maury, L. A G Monard, D. Moorhouse, N. Morgan, T. Natusch, E. O. Ofek, B. G. Park, R. W. Pogge, D. Polishook, R. Santallo, A. Shporer, O. Spector, G. Thornley, J. C. Yee, V. Bozza, P. Browne, M. Dominik, S. Dreizler, F. Finet, M. Glitrup, F. Grundahl, K. Harpsøe, F. V. Hessman, T. C. Hinse, M. Hundertmark, U. G. Jørgensen, C. Liebig, G. Maier, L. Mancini, M. Mathiasen, S. Rahvar, D. Ricci, G. Scarpetta, J. Southworth, J. Surdej, F. Zimmer, A. Allan, D. M. Bramich, C. Snodgrass, I. A. Steele, R. A. Street

Research output: Contribution to journalArticle

84 Citations (Scopus)

Abstract

Aims. We report the discovery of a planet with a high planet-to-star mass ratio in the microlensing event MOA-2009-BLG-387, which exhibited pronounced deviations over a 12-day interval, one of the longest for any planetary event. The host is an M dwarf, with a mass in the range 0.07 M ⊙ < Mhost < 0.49 M1 at 90% confidence. The planet-star mass ratio q = 0.0132 ± 0.003 has been measured extremely well, so at the best-estimated host mass, the planet mass is mp = 2.6 Jupiter masses for the median host mass, M = 0.19 M ⊙. Methods. The host mass is determined from two "higher order" microlensing parameters. One of these, the angular Einstein radius θE = 0.31 ± 0.03 mas has been accurately measured, but the other (the microlens parallax πE, which is due to the Earth's orbital motion) is highly degenerate with the orbital motion of the planet. We statistically resolve the degeneracy between Earth and planet orbital effects by imposing priors from a Galactic model that specifies the positions and velocities of lenses and sources and a Kepler model of orbits. Results. The 90% confidence intervals for the distance, semi-major axis, and period of the planet are 3.5 kpc < DL < 7.9 kpc, 1.1 AU < a < 2.7 AU, and 3.8 yr < P < 7.6 yr, respectively.

Original languageEnglish
Article numberA102
JournalAstronomy and Astrophysics
Volume529
DOIs
Publication statusPublished - 18 Apr 2011
Externally publishedYes

Fingerprint

planets
planet
orbits
mass ratios
confidence
intervals
stars
parallax
Jupiter (planet)
Jupiter
confidence interval
lenses
deviation
orbitals
radii

Keywords

  • gravitational lensing: micro
  • instrumentation: adaptive optics
  • instrumentation: photometers
  • methods: data analysis
  • methods: numerical
  • planets and satellites: detection

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Batista, V., Gould, A., Dieters, S., Dong, S., Bond, I., Beaulieu, J. P., ... Street, R. A. (2011). MOA-2009-BLG-387Lb: A massive planet orbiting an M dwarf. Astronomy and Astrophysics, 529, [A102]. https://doi.org/10.1051/0004-6361/201016111

MOA-2009-BLG-387Lb : A massive planet orbiting an M dwarf. / Batista, V.; Gould, A.; Dieters, S.; Dong, S.; Bond, I.; Beaulieu, J. P.; Maoz, D.; Monard, B.; Christie, G. W.; McCormick, J.; Albrow, M. D.; Horne, K.; Tsapras, Y.; Burgdorf, M. J.; Calchi Novati, S.; Skottfelt, J.; Caldwell, J.; Kozłowski, S.; Kubas, D.; Gaudi, B. S.; Han, C.; Bennett, D. P.; An, J.; Abe, F.; Botzler, C. S.; Douchin, D.; Freeman, M.; Fukui, A.; Furusawa, K.; Hearnshaw, J. B.; Hosaka, S.; Itow, Y.; Kamiya, K.; Kilmartin, P. M.; Korpela, A.; Lin, W.; Ling, C. H.; Makita, S.; Masuda, K.; Matsubara, Y.; Miyake, N.; Muraki, Y.; Nagaya, M.; Nishimoto, K.; Ohnishi, K.; Okumura, T.; Perrott, Y. C.; Rattenbury, N.; Saito, To; Sullivan, D. J.; Sumi, T.; Sweatman, W. L.; Tristram, P. J.; Von Seggern, E.; Yock, P. C M; Brillant, S.; Calitz, J. J.; Cassan, A.; Cole, A.; Cook, K.; Coutures, C.; Dominis Prester, D.; Donatowicz, J.; Greenhill, J.; Hoffman, M.; Jablonski, F.; Kane, S. R.; Kains, N.; Marquette, J. B.; Martin, R.; Martioli, E.; Meintjes, P.; Menzies, J.; Pedretti, E.; Pollard, K.; Sahu, K. C.; Vinter, C.; Wambsganss, J.; Watson, R.; Williams, A.; Zub, M.; Allen, W.; Bolt, G.; Bos, M.; Depoy, D. L.; Drummond, J.; Eastman, J. D.; Gal-Yam, A.; Gorbikov, E.; Higgins, D.; Janczak, J.; Kaspi, S.; Lee, C. U.; Mallia, F.; Maury, A.; Monard, L. A G; Moorhouse, D.; Morgan, N.; Natusch, T.; Ofek, E. O.; Park, B. G.; Pogge, R. W.; Polishook, D.; Santallo, R.; Shporer, A.; Spector, O.; Thornley, G.; Yee, J. C.; Bozza, V.; Browne, P.; Dominik, M.; Dreizler, S.; Finet, F.; Glitrup, M.; Grundahl, F.; Harpsøe, K.; Hessman, F. V.; Hinse, T. C.; Hundertmark, M.; Jørgensen, U. G.; Liebig, C.; Maier, G.; Mancini, L.; Mathiasen, M.; Rahvar, S.; Ricci, D.; Scarpetta, G.; Southworth, J.; Surdej, J.; Zimmer, F.; Allan, A.; Bramich, D. M.; Snodgrass, C.; Steele, I. A.; Street, R. A.

In: Astronomy and Astrophysics, Vol. 529, A102, 18.04.2011.

Research output: Contribution to journalArticle

Batista, V, Gould, A, Dieters, S, Dong, S, Bond, I, Beaulieu, JP, Maoz, D, Monard, B, Christie, GW, McCormick, J, Albrow, MD, Horne, K, Tsapras, Y, Burgdorf, MJ, Calchi Novati, S, Skottfelt, J, Caldwell, J, Kozłowski, S, Kubas, D, Gaudi, BS, Han, C, Bennett, DP, An, J, Abe, F, Botzler, CS, Douchin, D, Freeman, M, Fukui, A, Furusawa, K, Hearnshaw, JB, Hosaka, S, Itow, Y, Kamiya, K, Kilmartin, PM, Korpela, A, Lin, W, Ling, CH, Makita, S, Masuda, K, Matsubara, Y, Miyake, N, Muraki, Y, Nagaya, M, Nishimoto, K, Ohnishi, K, Okumura, T, Perrott, YC, Rattenbury, N, Saito, T, Sullivan, DJ, Sumi, T, Sweatman, WL, Tristram, PJ, Von Seggern, E, Yock, PCM, Brillant, S, Calitz, JJ, Cassan, A, Cole, A, Cook, K, Coutures, C, Dominis Prester, D, Donatowicz, J, Greenhill, J, Hoffman, M, Jablonski, F, Kane, SR, Kains, N, Marquette, JB, Martin, R, Martioli, E, Meintjes, P, Menzies, J, Pedretti, E, Pollard, K, Sahu, KC, Vinter, C, Wambsganss, J, Watson, R, Williams, A, Zub, M, Allen, W, Bolt, G, Bos, M, Depoy, DL, Drummond, J, Eastman, JD, Gal-Yam, A, Gorbikov, E, Higgins, D, Janczak, J, Kaspi, S, Lee, CU, Mallia, F, Maury, A, Monard, LAG, Moorhouse, D, Morgan, N, Natusch, T, Ofek, EO, Park, BG, Pogge, RW, Polishook, D, Santallo, R, Shporer, A, Spector, O, Thornley, G, Yee, JC, Bozza, V, Browne, P, Dominik, M, Dreizler, S, Finet, F, Glitrup, M, Grundahl, F, Harpsøe, K, Hessman, FV, Hinse, TC, Hundertmark, M, Jørgensen, UG, Liebig, C, Maier, G, Mancini, L, Mathiasen, M, Rahvar, S, Ricci, D, Scarpetta, G, Southworth, J, Surdej, J, Zimmer, F, Allan, A, Bramich, DM, Snodgrass, C, Steele, IA & Street, RA 2011, 'MOA-2009-BLG-387Lb: A massive planet orbiting an M dwarf', Astronomy and Astrophysics, vol. 529, A102. https://doi.org/10.1051/0004-6361/201016111
Batista V, Gould A, Dieters S, Dong S, Bond I, Beaulieu JP et al. MOA-2009-BLG-387Lb: A massive planet orbiting an M dwarf. Astronomy and Astrophysics. 2011 Apr 18;529. A102. https://doi.org/10.1051/0004-6361/201016111
Batista, V. ; Gould, A. ; Dieters, S. ; Dong, S. ; Bond, I. ; Beaulieu, J. P. ; Maoz, D. ; Monard, B. ; Christie, G. W. ; McCormick, J. ; Albrow, M. D. ; Horne, K. ; Tsapras, Y. ; Burgdorf, M. J. ; Calchi Novati, S. ; Skottfelt, J. ; Caldwell, J. ; Kozłowski, S. ; Kubas, D. ; Gaudi, B. S. ; Han, C. ; Bennett, D. P. ; An, J. ; Abe, F. ; Botzler, C. S. ; Douchin, D. ; Freeman, M. ; Fukui, A. ; Furusawa, K. ; Hearnshaw, J. B. ; Hosaka, S. ; Itow, Y. ; Kamiya, K. ; Kilmartin, P. M. ; Korpela, A. ; Lin, W. ; Ling, C. H. ; Makita, S. ; Masuda, K. ; Matsubara, Y. ; Miyake, N. ; Muraki, Y. ; Nagaya, M. ; Nishimoto, K. ; Ohnishi, K. ; Okumura, T. ; Perrott, Y. C. ; Rattenbury, N. ; Saito, To ; Sullivan, D. J. ; Sumi, T. ; Sweatman, W. L. ; Tristram, P. J. ; Von Seggern, E. ; Yock, P. C M ; Brillant, S. ; Calitz, J. J. ; Cassan, A. ; Cole, A. ; Cook, K. ; Coutures, C. ; Dominis Prester, D. ; Donatowicz, J. ; Greenhill, J. ; Hoffman, M. ; Jablonski, F. ; Kane, S. R. ; Kains, N. ; Marquette, J. B. ; Martin, R. ; Martioli, E. ; Meintjes, P. ; Menzies, J. ; Pedretti, E. ; Pollard, K. ; Sahu, K. C. ; Vinter, C. ; Wambsganss, J. ; Watson, R. ; Williams, A. ; Zub, M. ; Allen, W. ; Bolt, G. ; Bos, M. ; Depoy, D. L. ; Drummond, J. ; Eastman, J. D. ; Gal-Yam, A. ; Gorbikov, E. ; Higgins, D. ; Janczak, J. ; Kaspi, S. ; Lee, C. U. ; Mallia, F. ; Maury, A. ; Monard, L. A G ; Moorhouse, D. ; Morgan, N. ; Natusch, T. ; Ofek, E. O. ; Park, B. G. ; Pogge, R. W. ; Polishook, D. ; Santallo, R. ; Shporer, A. ; Spector, O. ; Thornley, G. ; Yee, J. C. ; Bozza, V. ; Browne, P. ; Dominik, M. ; Dreizler, S. ; Finet, F. ; Glitrup, M. ; Grundahl, F. ; Harpsøe, K. ; Hessman, F. V. ; Hinse, T. C. ; Hundertmark, M. ; Jørgensen, U. G. ; Liebig, C. ; Maier, G. ; Mancini, L. ; Mathiasen, M. ; Rahvar, S. ; Ricci, D. ; Scarpetta, G. ; Southworth, J. ; Surdej, J. ; Zimmer, F. ; Allan, A. ; Bramich, D. M. ; Snodgrass, C. ; Steele, I. A. ; Street, R. A. / MOA-2009-BLG-387Lb : A massive planet orbiting an M dwarf. In: Astronomy and Astrophysics. 2011 ; Vol. 529.
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title = "MOA-2009-BLG-387Lb: A massive planet orbiting an M dwarf",
abstract = "Aims. We report the discovery of a planet with a high planet-to-star mass ratio in the microlensing event MOA-2009-BLG-387, which exhibited pronounced deviations over a 12-day interval, one of the longest for any planetary event. The host is an M dwarf, with a mass in the range 0.07 M {\^a}Š™ < Mhost < 0.49 M1 at 90{\%} confidence. The planet-star mass ratio q = 0.0132 ± 0.003 has been measured extremely well, so at the best-estimated host mass, the planet mass is mp = 2.6 Jupiter masses for the median host mass, M = 0.19 M {\^a}Š™. Methods. The host mass is determined from two {"}higher order{"} microlensing parameters. One of these, the angular Einstein radius θE = 0.31 ± 0.03 mas has been accurately measured, but the other (the microlens parallax πE, which is due to the Earth's orbital motion) is highly degenerate with the orbital motion of the planet. We statistically resolve the degeneracy between Earth and planet orbital effects by imposing priors from a Galactic model that specifies the positions and velocities of lenses and sources and a Kepler model of orbits. Results. The 90{\%} confidence intervals for the distance, semi-major axis, and period of the planet are 3.5 kpc < DL < 7.9 kpc, 1.1 AU < a < 2.7 AU, and 3.8 yr < P < 7.6 yr, respectively.",
keywords = "gravitational lensing: micro, instrumentation: adaptive optics, instrumentation: photometers, methods: data analysis, methods: numerical, planets and satellites: detection",
author = "V. Batista and A. Gould and S. Dieters and S. Dong and I. Bond and Beaulieu, {J. P.} and D. Maoz and B. Monard and Christie, {G. W.} and J. McCormick and Albrow, {M. D.} and K. Horne and Y. Tsapras and Burgdorf, {M. J.} and {Calchi Novati}, S. and J. Skottfelt and J. Caldwell and S. Kozłowski and D. Kubas and Gaudi, {B. S.} and C. Han and Bennett, {D. P.} and J. An and F. Abe and Botzler, {C. S.} and D. Douchin and M. Freeman and A. Fukui and K. Furusawa and Hearnshaw, {J. B.} and S. Hosaka and Y. Itow and K. Kamiya and Kilmartin, {P. M.} and A. Korpela and W. Lin and Ling, {C. H.} and S. Makita and K. Masuda and Y. Matsubara and N. Miyake and Y. Muraki and M. Nagaya and K. Nishimoto and K. Ohnishi and T. Okumura and Perrott, {Y. C.} and N. Rattenbury and To Saito and Sullivan, {D. J.} and T. Sumi and Sweatman, {W. L.} and Tristram, {P. J.} and {Von Seggern}, E. and Yock, {P. C M} and S. Brillant and Calitz, {J. J.} and A. Cassan and A. Cole and K. Cook and C. Coutures and {Dominis Prester}, D. and J. Donatowicz and J. Greenhill and M. Hoffman and F. Jablonski and Kane, {S. R.} and N. Kains and Marquette, {J. B.} and R. Martin and E. Martioli and P. Meintjes and J. Menzies and E. Pedretti and K. Pollard and Sahu, {K. C.} and C. Vinter and J. Wambsganss and R. Watson and A. Williams and M. Zub and W. Allen and G. Bolt and M. Bos and Depoy, {D. L.} and J. Drummond and Eastman, {J. D.} and A. Gal-Yam and E. Gorbikov and D. Higgins and J. Janczak and S. Kaspi and Lee, {C. U.} and F. Mallia and A. Maury and Monard, {L. A G} and D. Moorhouse and N. Morgan and T. Natusch and Ofek, {E. O.} and Park, {B. G.} and Pogge, {R. W.} and D. Polishook and R. Santallo and A. Shporer and O. Spector and G. Thornley and Yee, {J. C.} and V. Bozza and P. Browne and M. Dominik and S. Dreizler and F. Finet and M. Glitrup and F. Grundahl and K. Harps{\o}e and Hessman, {F. V.} and Hinse, {T. C.} and M. Hundertmark and J{\o}rgensen, {U. G.} and C. Liebig and G. Maier and L. Mancini and M. Mathiasen and S. Rahvar and D. Ricci and G. Scarpetta and J. Southworth and J. Surdej and F. Zimmer and A. Allan and Bramich, {D. M.} and C. Snodgrass and Steele, {I. A.} and Street, {R. A.}",
year = "2011",
month = "4",
day = "18",
doi = "10.1051/0004-6361/201016111",
language = "English",
volume = "529",
journal = "Astronomy and Astrophysics",
issn = "0004-6361",
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TY - JOUR

T1 - MOA-2009-BLG-387Lb

T2 - A massive planet orbiting an M dwarf

AU - Batista, V.

AU - Gould, A.

AU - Dieters, S.

AU - Dong, S.

AU - Bond, I.

AU - Beaulieu, J. P.

AU - Maoz, D.

AU - Monard, B.

AU - Christie, G. W.

AU - McCormick, J.

AU - Albrow, M. D.

AU - Horne, K.

AU - Tsapras, Y.

AU - Burgdorf, M. J.

AU - Calchi Novati, S.

AU - Skottfelt, J.

AU - Caldwell, J.

AU - Kozłowski, S.

AU - Kubas, D.

AU - Gaudi, B. S.

AU - Han, C.

AU - Bennett, D. P.

AU - An, J.

AU - Abe, F.

AU - Botzler, C. S.

AU - Douchin, D.

AU - Freeman, M.

AU - Fukui, A.

AU - Furusawa, K.

AU - Hearnshaw, J. B.

AU - Hosaka, S.

AU - Itow, Y.

AU - Kamiya, K.

AU - Kilmartin, P. M.

AU - Korpela, A.

AU - Lin, W.

AU - Ling, C. H.

AU - Makita, S.

AU - Masuda, K.

AU - Matsubara, Y.

AU - Miyake, N.

AU - Muraki, Y.

AU - Nagaya, M.

AU - Nishimoto, K.

AU - Ohnishi, K.

AU - Okumura, T.

AU - Perrott, Y. C.

AU - Rattenbury, N.

AU - Saito, To

AU - Sullivan, D. J.

AU - Sumi, T.

AU - Sweatman, W. L.

AU - Tristram, P. J.

AU - Von Seggern, E.

AU - Yock, P. C M

AU - Brillant, S.

AU - Calitz, J. J.

AU - Cassan, A.

AU - Cole, A.

AU - Cook, K.

AU - Coutures, C.

AU - Dominis Prester, D.

AU - Donatowicz, J.

AU - Greenhill, J.

AU - Hoffman, M.

AU - Jablonski, F.

AU - Kane, S. R.

AU - Kains, N.

AU - Marquette, J. B.

AU - Martin, R.

AU - Martioli, E.

AU - Meintjes, P.

AU - Menzies, J.

AU - Pedretti, E.

AU - Pollard, K.

AU - Sahu, K. C.

AU - Vinter, C.

AU - Wambsganss, J.

AU - Watson, R.

AU - Williams, A.

AU - Zub, M.

AU - Allen, W.

AU - Bolt, G.

AU - Bos, M.

AU - Depoy, D. L.

AU - Drummond, J.

AU - Eastman, J. D.

AU - Gal-Yam, A.

AU - Gorbikov, E.

AU - Higgins, D.

AU - Janczak, J.

AU - Kaspi, S.

AU - Lee, C. U.

AU - Mallia, F.

AU - Maury, A.

AU - Monard, L. A G

AU - Moorhouse, D.

AU - Morgan, N.

AU - Natusch, T.

AU - Ofek, E. O.

AU - Park, B. G.

AU - Pogge, R. W.

AU - Polishook, D.

AU - Santallo, R.

AU - Shporer, A.

AU - Spector, O.

AU - Thornley, G.

AU - Yee, J. C.

AU - Bozza, V.

AU - Browne, P.

AU - Dominik, M.

AU - Dreizler, S.

AU - Finet, F.

AU - Glitrup, M.

AU - Grundahl, F.

AU - Harpsøe, K.

AU - Hessman, F. V.

AU - Hinse, T. C.

AU - Hundertmark, M.

AU - Jørgensen, U. G.

AU - Liebig, C.

AU - Maier, G.

AU - Mancini, L.

AU - Mathiasen, M.

AU - Rahvar, S.

AU - Ricci, D.

AU - Scarpetta, G.

AU - Southworth, J.

AU - Surdej, J.

AU - Zimmer, F.

AU - Allan, A.

AU - Bramich, D. M.

AU - Snodgrass, C.

AU - Steele, I. A.

AU - Street, R. A.

PY - 2011/4/18

Y1 - 2011/4/18

N2 - Aims. We report the discovery of a planet with a high planet-to-star mass ratio in the microlensing event MOA-2009-BLG-387, which exhibited pronounced deviations over a 12-day interval, one of the longest for any planetary event. The host is an M dwarf, with a mass in the range 0.07 M ⊙ < Mhost < 0.49 M1 at 90% confidence. The planet-star mass ratio q = 0.0132 ± 0.003 has been measured extremely well, so at the best-estimated host mass, the planet mass is mp = 2.6 Jupiter masses for the median host mass, M = 0.19 M ⊙. Methods. The host mass is determined from two "higher order" microlensing parameters. One of these, the angular Einstein radius θE = 0.31 ± 0.03 mas has been accurately measured, but the other (the microlens parallax πE, which is due to the Earth's orbital motion) is highly degenerate with the orbital motion of the planet. We statistically resolve the degeneracy between Earth and planet orbital effects by imposing priors from a Galactic model that specifies the positions and velocities of lenses and sources and a Kepler model of orbits. Results. The 90% confidence intervals for the distance, semi-major axis, and period of the planet are 3.5 kpc < DL < 7.9 kpc, 1.1 AU < a < 2.7 AU, and 3.8 yr < P < 7.6 yr, respectively.

AB - Aims. We report the discovery of a planet with a high planet-to-star mass ratio in the microlensing event MOA-2009-BLG-387, which exhibited pronounced deviations over a 12-day interval, one of the longest for any planetary event. The host is an M dwarf, with a mass in the range 0.07 M ⊙ < Mhost < 0.49 M1 at 90% confidence. The planet-star mass ratio q = 0.0132 ± 0.003 has been measured extremely well, so at the best-estimated host mass, the planet mass is mp = 2.6 Jupiter masses for the median host mass, M = 0.19 M ⊙. Methods. The host mass is determined from two "higher order" microlensing parameters. One of these, the angular Einstein radius θE = 0.31 ± 0.03 mas has been accurately measured, but the other (the microlens parallax πE, which is due to the Earth's orbital motion) is highly degenerate with the orbital motion of the planet. We statistically resolve the degeneracy between Earth and planet orbital effects by imposing priors from a Galactic model that specifies the positions and velocities of lenses and sources and a Kepler model of orbits. Results. The 90% confidence intervals for the distance, semi-major axis, and period of the planet are 3.5 kpc < DL < 7.9 kpc, 1.1 AU < a < 2.7 AU, and 3.8 yr < P < 7.6 yr, respectively.

KW - gravitational lensing: micro

KW - instrumentation: adaptive optics

KW - instrumentation: photometers

KW - methods: data analysis

KW - methods: numerical

KW - planets and satellites: detection

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U2 - 10.1051/0004-6361/201016111

DO - 10.1051/0004-6361/201016111

M3 - Article

VL - 529

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

SN - 0004-6361

M1 - A102

ER -