MOA 2010-BLG-477Lb

Constraining the mass of a microlensing planet from microlensing parallax, orbital motion, and detection of blended light

E. Bachelet, I. G. Shin, C. Han, P. Fouqué, A. Gould, J. W. Menzies, J. P. Beaulieu, D. P. Bennett, I. A. Bond, Subo Dong, D. Heyrovsk, J. B. Marquette, J. Marshall, J. Skowron, R. A. Street, T. Sumi, A. Udalski, L. Abe, K. Agabi, M. D. Albrow & 121 others W. Allen, E. Bertin, M. Bos, D. M. Bramich, J. Chavez, G. W. Christie, A. A. Cole, N. Crouzet, S. Dieters, M. Dominik, J. Drummond, J. Greenhill, T. Guillot, C. B. Henderson, F. V. Hessman, K. Horne, M. Hundertmark, J. A. Johnson, U. G. Jorgensen, R. Kandori, C. Liebig, D. Mékarnia, J. McCormick, D. Moorhouse, T. Nagayama, D. Nataf, T. Natusch, S. Nishiyama, J. P. Rivet, K. C. Sahu, Y. Shvartzvald, G. Thornley, A. R. Tomczak, Y. Tsapras, J. C. Yee, V. Batista, C. S. Bennett, S. Brillant, J. A R Caldwell, A. Cassan, E. Corrales, C. Coutures, D. Dominis Prester, J. Donatowicz, D. Kubas, R. Martin, A. Williams, M. Zub, L. Andrade De Almeida, D. L. Depoy, B. S. Gaudi, L. W. Hung, F. Jablonski, S. Kaspi, N. Klein, C. U. Lee, Y. Lee, J. R. Koo, D. Maoz, J. A. Muñoz, R. W. Pogge, D. Polishook, A. Shporer, F. Abe, C. S. Botzler, P. Chote, M. Freeman, A. Fukui, K. Furusawa, P. Harris, Y. Itow, S. Kobara, C. H. Ling, K. Masuda, Y. Matsubara, N. Miyake, K. Ohmori, K. Ohnishi, N. J. Rattenbury, To Saito, D. J. Sullivan, D. Suzuki, W. L. Sweatman, P. J. Tristram, K. Wada, P. C M Yock, M. K. Szymański, I. Soszyński, M. Kubiak, R. Poleski, K. Ulaczyk, G. Pietrzyński, Wyrzykowski, N. Kains, C. Snodgrass, I. A. Steele, Khalid Al-Subai, V. Bozza, P. Browne, M. J. Burgdorf, S. Calchi Novati, P. Dodds, S. Dreizler, F. Finet, T. Gerner, S. Hardis, K. Harpsoe, T. C. Hinse, E. Kerins, L. Mancini, M. Mathiasen, M. T. Penny, S. Proft, S. Rahvar, D. Ricci, G. Scarpetta, S. Schäfer, F. Schönebeck, J. Southworth, J. Surdej, J. Wambsganss

Research output: Contribution to journalArticle

30 Citations (Scopus)

Abstract

Microlensing detections of cool planets are important for the construction of an unbiased sample to estimate the frequency of planets beyond the snow line, which is where giant planets are thought to form according to the core accretion theory of planet formation. In this paper, we report the discovery of a giant planet detected from the analysis of the light curve of a high-magnification microlensing event MOA 2010-BLG-477. The measured planet-star mass ratio is q = (2.181 ± 0.004) × 10-3 and the projected separation is s = 1.1228 ± 0.0006 in units of the Einstein radius. The angular Einstein radius is unusually large θE = 1.38 ± 0.11 mas. Combining this measurement with constraints on the "microlens parallax" and the lens flux, we can only limit the host mass to the range 0.13 < M/M < 1.0. In this particular case, the strong degeneracy between microlensing parallax and planet orbital motion prevents us from measuring more accurate host and planet masses. However, we find that adding Bayesian priors from two effects (Galactic model and Keplerian orbit) each independently favors the upper end of this mass range, yielding star and planet masses of M * = 0.67+0.33 - 0.13 M and mp1.5+0.8 - 0.3 M JUP at a distance of D = 2.3 ± 0.6kpc, and with a semi-major axis of a = 2 +3 - 1AU. Finally, we show that the lens mass can be determined from future high-resolution near-IR adaptive optics observations independently from two effects, photometric and astrometric.

Original languageEnglish
Article number73
JournalAstrophysical Journal
Volume754
Issue number1
DOIs
Publication statusPublished - 20 Jul 2012

Fingerprint

parallax
planets
planet
orbits
lenses
detection
stars
radii
snow
magnification
adaptive optics
mass ratios
light curve
accretion
high resolution
estimates

Keywords

  • gravitational lensing: micro
  • planetary systems

ASJC Scopus subject areas

  • Space and Planetary Science
  • Astronomy and Astrophysics

Cite this

MOA 2010-BLG-477Lb : Constraining the mass of a microlensing planet from microlensing parallax, orbital motion, and detection of blended light. / Bachelet, E.; Shin, I. G.; Han, C.; Fouqué, P.; Gould, A.; Menzies, J. W.; Beaulieu, J. P.; Bennett, D. P.; Bond, I. A.; Dong, Subo; Heyrovsk, D.; Marquette, J. B.; Marshall, J.; Skowron, J.; Street, R. A.; Sumi, T.; Udalski, A.; Abe, L.; Agabi, K.; Albrow, M. D.; Allen, W.; Bertin, E.; Bos, M.; Bramich, D. M.; Chavez, J.; Christie, G. W.; Cole, A. A.; Crouzet, N.; Dieters, S.; Dominik, M.; Drummond, J.; Greenhill, J.; Guillot, T.; Henderson, C. B.; Hessman, F. V.; Horne, K.; Hundertmark, M.; Johnson, J. A.; Jorgensen, U. G.; Kandori, R.; Liebig, C.; Mékarnia, D.; McCormick, J.; Moorhouse, D.; Nagayama, T.; Nataf, D.; Natusch, T.; Nishiyama, S.; Rivet, J. P.; Sahu, K. C.; Shvartzvald, Y.; Thornley, G.; Tomczak, A. R.; Tsapras, Y.; Yee, J. C.; Batista, V.; Bennett, C. S.; Brillant, S.; Caldwell, J. A R; Cassan, A.; Corrales, E.; Coutures, C.; Dominis Prester, D.; Donatowicz, J.; Kubas, D.; Martin, R.; Williams, A.; Zub, M.; Andrade De Almeida, L.; Depoy, D. L.; Gaudi, B. S.; Hung, L. W.; Jablonski, F.; Kaspi, S.; Klein, N.; Lee, C. U.; Lee, Y.; Koo, J. R.; Maoz, D.; Muñoz, J. A.; Pogge, R. W.; Polishook, D.; Shporer, A.; Abe, F.; Botzler, C. S.; Chote, P.; Freeman, M.; Fukui, A.; Furusawa, K.; Harris, P.; Itow, Y.; Kobara, S.; Ling, C. H.; Masuda, K.; Matsubara, Y.; Miyake, N.; Ohmori, K.; Ohnishi, K.; Rattenbury, N. J.; Saito, To; Sullivan, D. J.; Suzuki, D.; Sweatman, W. L.; Tristram, P. J.; Wada, K.; Yock, P. C M; Szymański, M. K.; Soszyński, I.; Kubiak, M.; Poleski, R.; Ulaczyk, K.; Pietrzyński, G.; Wyrzykowski; Kains, N.; Snodgrass, C.; Steele, I. A.; Al-Subai, Khalid; Bozza, V.; Browne, P.; Burgdorf, M. J.; Calchi Novati, S.; Dodds, P.; Dreizler, S.; Finet, F.; Gerner, T.; Hardis, S.; Harpsoe, K.; Hinse, T. C.; Kerins, E.; Mancini, L.; Mathiasen, M.; Penny, M. T.; Proft, S.; Rahvar, S.; Ricci, D.; Scarpetta, G.; Schäfer, S.; Schönebeck, F.; Southworth, J.; Surdej, J.; Wambsganss, J.

In: Astrophysical Journal, Vol. 754, No. 1, 73, 20.07.2012.

Research output: Contribution to journalArticle

Bachelet, E, Shin, IG, Han, C, Fouqué, P, Gould, A, Menzies, JW, Beaulieu, JP, Bennett, DP, Bond, IA, Dong, S, Heyrovsk, D, Marquette, JB, Marshall, J, Skowron, J, Street, RA, Sumi, T, Udalski, A, Abe, L, Agabi, K, Albrow, MD, Allen, W, Bertin, E, Bos, M, Bramich, DM, Chavez, J, Christie, GW, Cole, AA, Crouzet, N, Dieters, S, Dominik, M, Drummond, J, Greenhill, J, Guillot, T, Henderson, CB, Hessman, FV, Horne, K, Hundertmark, M, Johnson, JA, Jorgensen, UG, Kandori, R, Liebig, C, Mékarnia, D, McCormick, J, Moorhouse, D, Nagayama, T, Nataf, D, Natusch, T, Nishiyama, S, Rivet, JP, Sahu, KC, Shvartzvald, Y, Thornley, G, Tomczak, AR, Tsapras, Y, Yee, JC, Batista, V, Bennett, CS, Brillant, S, Caldwell, JAR, Cassan, A, Corrales, E, Coutures, C, Dominis Prester, D, Donatowicz, J, Kubas, D, Martin, R, Williams, A, Zub, M, Andrade De Almeida, L, Depoy, DL, Gaudi, BS, Hung, LW, Jablonski, F, Kaspi, S, Klein, N, Lee, CU, Lee, Y, Koo, JR, Maoz, D, Muñoz, JA, Pogge, RW, Polishook, D, Shporer, A, Abe, F, Botzler, CS, Chote, P, Freeman, M, Fukui, A, Furusawa, K, Harris, P, Itow, Y, Kobara, S, Ling, CH, Masuda, K, Matsubara, Y, Miyake, N, Ohmori, K, Ohnishi, K, Rattenbury, NJ, Saito, T, Sullivan, DJ, Suzuki, D, Sweatman, WL, Tristram, PJ, Wada, K, Yock, PCM, Szymański, MK, Soszyński, I, Kubiak, M, Poleski, R, Ulaczyk, K, Pietrzyński, G, Wyrzykowski, Kains, N, Snodgrass, C, Steele, IA, Al-Subai, K, Bozza, V, Browne, P, Burgdorf, MJ, Calchi Novati, S, Dodds, P, Dreizler, S, Finet, F, Gerner, T, Hardis, S, Harpsoe, K, Hinse, TC, Kerins, E, Mancini, L, Mathiasen, M, Penny, MT, Proft, S, Rahvar, S, Ricci, D, Scarpetta, G, Schäfer, S, Schönebeck, F, Southworth, J, Surdej, J & Wambsganss, J 2012, 'MOA 2010-BLG-477Lb: Constraining the mass of a microlensing planet from microlensing parallax, orbital motion, and detection of blended light', Astrophysical Journal, vol. 754, no. 1, 73. https://doi.org/10.1088/0004-637X/754/1/73
Bachelet, E. ; Shin, I. G. ; Han, C. ; Fouqué, P. ; Gould, A. ; Menzies, J. W. ; Beaulieu, J. P. ; Bennett, D. P. ; Bond, I. A. ; Dong, Subo ; Heyrovsk, D. ; Marquette, J. B. ; Marshall, J. ; Skowron, J. ; Street, R. A. ; Sumi, T. ; Udalski, A. ; Abe, L. ; Agabi, K. ; Albrow, M. D. ; Allen, W. ; Bertin, E. ; Bos, M. ; Bramich, D. M. ; Chavez, J. ; Christie, G. W. ; Cole, A. A. ; Crouzet, N. ; Dieters, S. ; Dominik, M. ; Drummond, J. ; Greenhill, J. ; Guillot, T. ; Henderson, C. B. ; Hessman, F. V. ; Horne, K. ; Hundertmark, M. ; Johnson, J. A. ; Jorgensen, U. G. ; Kandori, R. ; Liebig, C. ; Mékarnia, D. ; McCormick, J. ; Moorhouse, D. ; Nagayama, T. ; Nataf, D. ; Natusch, T. ; Nishiyama, S. ; Rivet, J. P. ; Sahu, K. C. ; Shvartzvald, Y. ; Thornley, G. ; Tomczak, A. R. ; Tsapras, Y. ; Yee, J. C. ; Batista, V. ; Bennett, C. S. ; Brillant, S. ; Caldwell, J. A R ; Cassan, A. ; Corrales, E. ; Coutures, C. ; Dominis Prester, D. ; Donatowicz, J. ; Kubas, D. ; Martin, R. ; Williams, A. ; Zub, M. ; Andrade De Almeida, L. ; Depoy, D. L. ; Gaudi, B. S. ; Hung, L. W. ; Jablonski, F. ; Kaspi, S. ; Klein, N. ; Lee, C. U. ; Lee, Y. ; Koo, J. R. ; Maoz, D. ; Muñoz, J. A. ; Pogge, R. W. ; Polishook, D. ; Shporer, A. ; Abe, F. ; Botzler, C. S. ; Chote, P. ; Freeman, M. ; Fukui, A. ; Furusawa, K. ; Harris, P. ; Itow, Y. ; Kobara, S. ; Ling, C. H. ; Masuda, K. ; Matsubara, Y. ; Miyake, N. ; Ohmori, K. ; Ohnishi, K. ; Rattenbury, N. J. ; Saito, To ; Sullivan, D. J. ; Suzuki, D. ; Sweatman, W. L. ; Tristram, P. J. ; Wada, K. ; Yock, P. C M ; Szymański, M. K. ; Soszyński, I. ; Kubiak, M. ; Poleski, R. ; Ulaczyk, K. ; Pietrzyński, G. ; Wyrzykowski ; Kains, N. ; Snodgrass, C. ; Steele, I. A. ; Al-Subai, Khalid ; Bozza, V. ; Browne, P. ; Burgdorf, M. J. ; Calchi Novati, S. ; Dodds, P. ; Dreizler, S. ; Finet, F. ; Gerner, T. ; Hardis, S. ; Harpsoe, K. ; Hinse, T. C. ; Kerins, E. ; Mancini, L. ; Mathiasen, M. ; Penny, M. T. ; Proft, S. ; Rahvar, S. ; Ricci, D. ; Scarpetta, G. ; Schäfer, S. ; Schönebeck, F. ; Southworth, J. ; Surdej, J. ; Wambsganss, J. / MOA 2010-BLG-477Lb : Constraining the mass of a microlensing planet from microlensing parallax, orbital motion, and detection of blended light. In: Astrophysical Journal. 2012 ; Vol. 754, No. 1.
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title = "MOA 2010-BLG-477Lb: Constraining the mass of a microlensing planet from microlensing parallax, orbital motion, and detection of blended light",
abstract = "Microlensing detections of cool planets are important for the construction of an unbiased sample to estimate the frequency of planets beyond the snow line, which is where giant planets are thought to form according to the core accretion theory of planet formation. In this paper, we report the discovery of a giant planet detected from the analysis of the light curve of a high-magnification microlensing event MOA 2010-BLG-477. The measured planet-star mass ratio is q = (2.181 ± 0.004) × 10-3 and the projected separation is s = 1.1228 ± 0.0006 in units of the Einstein radius. The angular Einstein radius is unusually large θE = 1.38 ± 0.11 mas. Combining this measurement with constraints on the {"}microlens parallax{"} and the lens flux, we can only limit the host mass to the range 0.13 < M/M < 1.0. In this particular case, the strong degeneracy between microlensing parallax and planet orbital motion prevents us from measuring more accurate host and planet masses. However, we find that adding Bayesian priors from two effects (Galactic model and Keplerian orbit) each independently favors the upper end of this mass range, yielding star and planet masses of M * = 0.67+0.33 - 0.13 M and mp1.5+0.8 - 0.3 M JUP at a distance of D = 2.3 ± 0.6kpc, and with a semi-major axis of a = 2 +3 - 1AU. Finally, we show that the lens mass can be determined from future high-resolution near-IR adaptive optics observations independently from two effects, photometric and astrometric.",
keywords = "gravitational lensing: micro, planetary systems",
author = "E. Bachelet and Shin, {I. G.} and C. Han and P. Fouqu{\'e} and A. Gould and Menzies, {J. W.} and Beaulieu, {J. P.} and Bennett, {D. P.} and Bond, {I. A.} and Subo Dong and D. Heyrovsk and Marquette, {J. B.} and J. Marshall and J. Skowron and Street, {R. A.} and T. Sumi and A. Udalski and L. Abe and K. Agabi and Albrow, {M. D.} and W. Allen and E. Bertin and M. Bos and Bramich, {D. M.} and J. Chavez and Christie, {G. W.} and Cole, {A. A.} and N. Crouzet and S. Dieters and M. Dominik and J. Drummond and J. Greenhill and T. Guillot and Henderson, {C. B.} and Hessman, {F. V.} and K. Horne and M. Hundertmark and Johnson, {J. A.} and Jorgensen, {U. G.} and R. Kandori and C. Liebig and D. M{\'e}karnia and J. McCormick and D. Moorhouse and T. Nagayama and D. Nataf and T. Natusch and S. Nishiyama and Rivet, {J. P.} and Sahu, {K. C.} and Y. Shvartzvald and G. Thornley and Tomczak, {A. R.} and Y. Tsapras and Yee, {J. C.} and V. Batista and Bennett, {C. S.} and S. Brillant and Caldwell, {J. A R} and A. Cassan and E. Corrales and C. Coutures and {Dominis Prester}, D. and J. Donatowicz and D. Kubas and R. Martin and A. Williams and M. Zub and {Andrade De Almeida}, L. and Depoy, {D. L.} and Gaudi, {B. S.} and Hung, {L. W.} and F. Jablonski and S. Kaspi and N. Klein and Lee, {C. U.} and Y. Lee and Koo, {J. R.} and D. Maoz and Mu{\~n}oz, {J. A.} and Pogge, {R. W.} and D. Polishook and A. Shporer and F. Abe and Botzler, {C. S.} and P. Chote and M. Freeman and A. Fukui and K. Furusawa and P. Harris and Y. Itow and S. Kobara and Ling, {C. H.} and K. Masuda and Y. Matsubara and N. Miyake and K. Ohmori and K. Ohnishi and Rattenbury, {N. J.} and To Saito and Sullivan, {D. J.} and D. Suzuki and Sweatman, {W. L.} and Tristram, {P. J.} and K. Wada and Yock, {P. C M} and Szymański, {M. K.} and I. Soszyński and M. Kubiak and R. Poleski and K. Ulaczyk and G. Pietrzyński and Wyrzykowski and N. Kains and C. Snodgrass and Steele, {I. A.} and Khalid Al-Subai and V. Bozza and P. Browne and Burgdorf, {M. J.} and {Calchi Novati}, S. and P. Dodds and S. Dreizler and F. Finet and T. Gerner and S. Hardis and K. Harpsoe and Hinse, {T. C.} and E. Kerins and L. Mancini and M. Mathiasen and Penny, {M. T.} and S. Proft and S. Rahvar and D. Ricci and G. Scarpetta and S. Sch{\"a}fer and F. Sch{\"o}nebeck and J. Southworth and J. Surdej and J. Wambsganss",
year = "2012",
month = "7",
day = "20",
doi = "10.1088/0004-637X/754/1/73",
language = "English",
volume = "754",
journal = "Astrophysical Journal",
issn = "0004-637X",
publisher = "IOP Publishing Ltd.",
number = "1",

}

TY - JOUR

T1 - MOA 2010-BLG-477Lb

T2 - Constraining the mass of a microlensing planet from microlensing parallax, orbital motion, and detection of blended light

AU - Bachelet, E.

AU - Shin, I. G.

AU - Han, C.

AU - Fouqué, P.

AU - Gould, A.

AU - Menzies, J. W.

AU - Beaulieu, J. P.

AU - Bennett, D. P.

AU - Bond, I. A.

AU - Dong, Subo

AU - Heyrovsk, D.

AU - Marquette, J. B.

AU - Marshall, J.

AU - Skowron, J.

AU - Street, R. A.

AU - Sumi, T.

AU - Udalski, A.

AU - Abe, L.

AU - Agabi, K.

AU - Albrow, M. D.

AU - Allen, W.

AU - Bertin, E.

AU - Bos, M.

AU - Bramich, D. M.

AU - Chavez, J.

AU - Christie, G. W.

AU - Cole, A. A.

AU - Crouzet, N.

AU - Dieters, S.

AU - Dominik, M.

AU - Drummond, J.

AU - Greenhill, J.

AU - Guillot, T.

AU - Henderson, C. B.

AU - Hessman, F. V.

AU - Horne, K.

AU - Hundertmark, M.

AU - Johnson, J. A.

AU - Jorgensen, U. G.

AU - Kandori, R.

AU - Liebig, C.

AU - Mékarnia, D.

AU - McCormick, J.

AU - Moorhouse, D.

AU - Nagayama, T.

AU - Nataf, D.

AU - Natusch, T.

AU - Nishiyama, S.

AU - Rivet, J. P.

AU - Sahu, K. C.

AU - Shvartzvald, Y.

AU - Thornley, G.

AU - Tomczak, A. R.

AU - Tsapras, Y.

AU - Yee, J. C.

AU - Batista, V.

AU - Bennett, C. S.

AU - Brillant, S.

AU - Caldwell, J. A R

AU - Cassan, A.

AU - Corrales, E.

AU - Coutures, C.

AU - Dominis Prester, D.

AU - Donatowicz, J.

AU - Kubas, D.

AU - Martin, R.

AU - Williams, A.

AU - Zub, M.

AU - Andrade De Almeida, L.

AU - Depoy, D. L.

AU - Gaudi, B. S.

AU - Hung, L. W.

AU - Jablonski, F.

AU - Kaspi, S.

AU - Klein, N.

AU - Lee, C. U.

AU - Lee, Y.

AU - Koo, J. R.

AU - Maoz, D.

AU - Muñoz, J. A.

AU - Pogge, R. W.

AU - Polishook, D.

AU - Shporer, A.

AU - Abe, F.

AU - Botzler, C. S.

AU - Chote, P.

AU - Freeman, M.

AU - Fukui, A.

AU - Furusawa, K.

AU - Harris, P.

AU - Itow, Y.

AU - Kobara, S.

AU - Ling, C. H.

AU - Masuda, K.

AU - Matsubara, Y.

AU - Miyake, N.

AU - Ohmori, K.

AU - Ohnishi, K.

AU - Rattenbury, N. J.

AU - Saito, To

AU - Sullivan, D. J.

AU - Suzuki, D.

AU - Sweatman, W. L.

AU - Tristram, P. J.

AU - Wada, K.

AU - Yock, P. C M

AU - Szymański, M. K.

AU - Soszyński, I.

AU - Kubiak, M.

AU - Poleski, R.

AU - Ulaczyk, K.

AU - Pietrzyński, G.

AU - Wyrzykowski,

AU - Kains, N.

AU - Snodgrass, C.

AU - Steele, I. A.

AU - Al-Subai, Khalid

AU - Bozza, V.

AU - Browne, P.

AU - Burgdorf, M. J.

AU - Calchi Novati, S.

AU - Dodds, P.

AU - Dreizler, S.

AU - Finet, F.

AU - Gerner, T.

AU - Hardis, S.

AU - Harpsoe, K.

AU - Hinse, T. C.

AU - Kerins, E.

AU - Mancini, L.

AU - Mathiasen, M.

AU - Penny, M. T.

AU - Proft, S.

AU - Rahvar, S.

AU - Ricci, D.

AU - Scarpetta, G.

AU - Schäfer, S.

AU - Schönebeck, F.

AU - Southworth, J.

AU - Surdej, J.

AU - Wambsganss, J.

PY - 2012/7/20

Y1 - 2012/7/20

N2 - Microlensing detections of cool planets are important for the construction of an unbiased sample to estimate the frequency of planets beyond the snow line, which is where giant planets are thought to form according to the core accretion theory of planet formation. In this paper, we report the discovery of a giant planet detected from the analysis of the light curve of a high-magnification microlensing event MOA 2010-BLG-477. The measured planet-star mass ratio is q = (2.181 ± 0.004) × 10-3 and the projected separation is s = 1.1228 ± 0.0006 in units of the Einstein radius. The angular Einstein radius is unusually large θE = 1.38 ± 0.11 mas. Combining this measurement with constraints on the "microlens parallax" and the lens flux, we can only limit the host mass to the range 0.13 < M/M < 1.0. In this particular case, the strong degeneracy between microlensing parallax and planet orbital motion prevents us from measuring more accurate host and planet masses. However, we find that adding Bayesian priors from two effects (Galactic model and Keplerian orbit) each independently favors the upper end of this mass range, yielding star and planet masses of M * = 0.67+0.33 - 0.13 M and mp1.5+0.8 - 0.3 M JUP at a distance of D = 2.3 ± 0.6kpc, and with a semi-major axis of a = 2 +3 - 1AU. Finally, we show that the lens mass can be determined from future high-resolution near-IR adaptive optics observations independently from two effects, photometric and astrometric.

AB - Microlensing detections of cool planets are important for the construction of an unbiased sample to estimate the frequency of planets beyond the snow line, which is where giant planets are thought to form according to the core accretion theory of planet formation. In this paper, we report the discovery of a giant planet detected from the analysis of the light curve of a high-magnification microlensing event MOA 2010-BLG-477. The measured planet-star mass ratio is q = (2.181 ± 0.004) × 10-3 and the projected separation is s = 1.1228 ± 0.0006 in units of the Einstein radius. The angular Einstein radius is unusually large θE = 1.38 ± 0.11 mas. Combining this measurement with constraints on the "microlens parallax" and the lens flux, we can only limit the host mass to the range 0.13 < M/M < 1.0. In this particular case, the strong degeneracy between microlensing parallax and planet orbital motion prevents us from measuring more accurate host and planet masses. However, we find that adding Bayesian priors from two effects (Galactic model and Keplerian orbit) each independently favors the upper end of this mass range, yielding star and planet masses of M * = 0.67+0.33 - 0.13 M and mp1.5+0.8 - 0.3 M JUP at a distance of D = 2.3 ± 0.6kpc, and with a semi-major axis of a = 2 +3 - 1AU. Finally, we show that the lens mass can be determined from future high-resolution near-IR adaptive optics observations independently from two effects, photometric and astrometric.

KW - gravitational lensing: micro

KW - planetary systems

UR - http://www.scopus.com/inward/record.url?scp=84863652082&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=84863652082&partnerID=8YFLogxK

U2 - 10.1088/0004-637X/754/1/73

DO - 10.1088/0004-637X/754/1/73

M3 - Article

VL - 754

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 1

M1 - 73

ER -