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. Kozlowski; D. Kubas; B. S. Gaudi; 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. Harpsoe; F. V. Hessman; T. C. Hinse; M. Hundertmark; U. G. Jorgensen; 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

doi:10.1051/0004-6361/201016111

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. Kozlowski, D. Kubas, B. S. GaudiC. 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. Harpsoe, F. V. Hessman, T. C. Hinse, M. Hundertmark, U. G. Jorgensen, 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

School of Physics and Astronomy

Research output: Contribution to journal › Article › peer-review

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-circle dot < M-host < 0.49 M-circle dot 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 m(p) = 2.6 Jupiter masses for the median host mass, M = 0.19 M-circle dot.

Methods. The host mass is determined from two "higher order" microlensing parameters. One of these, the angular Einstein radius theta(E) = 0.31 +/- 0.03 mas has been accurately measured, but the other (the microlens parallax pi(E), 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 < D-L < 7.9 kpc, 1.1 AU < a < 2.7 AU, and 3.8 yr < P < 7.6 yr, respectively.

Original language	English
Article number	A102
Number of pages	16
Journal	Astronomy & Astrophysics
Volume	529
DOIs	https://doi.org/10.1051/0004-6361/201016111
Publication status	Published - May 2011

Keywords

gravitational lensing: micro
methods: data analysis
planets and satellites: detection
methods: numerical
instrumentation: adaptive optics
instrumentation: photometers
GALACTIC BULGE
MICROLENSING EVENT
JUPITER/SATURN ANALOG
GIANT PLANETS
SNOW LINE
STARS
MASSES
PHOTOMETRY
COOL
LUMINOSITY

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10.1051/0004-6361/201016111

Astrophysics in St Andrews: Astrophysics in St Andrews / SUPA (Continuan of Rolling Grant - XPP089
Bonnell, I. A. (PI), Cameron, A. C. (CoI), Dominik, M. (CoI), Driver, S. P. (CoI), Greaves, J. S. (CoI), Horne, K. D. (CoI), Jardine, M. M. (CoI), Wood, K. (CoI) & Zhao, H. (CoI)
Science & Technology Facilities Council
1/04/09 → 31/03/12
Project: Standard

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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., Kozlowski, S., Kubas, D., ... Street, R. A. (2011). MOA-2009-BLG-387Lb: a massive planet orbiting an M dwarf. Astronomy & Astrophysics, 529, Article A102. https://doi.org/10.1051/0004-6361/201016111

@article{900cb7cd3660499a807168cf2bb24754,

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-circle dot < M-host < 0.49 M-circle dot 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 m(p) = 2.6 Jupiter masses for the median host mass, M = 0.19 M-circle dot.Methods. The host mass is determined from two {"}higher order{"} microlensing parameters. One of these, the angular Einstein radius theta(E) = 0.31 +/- 0.03 mas has been accurately measured, but the other (the microlens parallax pi(E), 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 < D-L < 7.9 kpc, 1.1 AU < a < 2.7 AU, and 3.8 yr < P < 7.6 yr, respectively.",

keywords = "gravitational lensing: micro, methods: data analysis, planets and satellites: detection, methods: numerical, instrumentation: adaptive optics, instrumentation: photometers, GALACTIC BULGE, MICROLENSING EVENT, JUPITER/SATURN ANALOG, GIANT PLANETS, SNOW LINE, STARS, MASSES, PHOTOMETRY, COOL, LUMINOSITY",

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. Kozlowski 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 Prester, {D. Dominis} 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. Harpsoe and Hessman, {F. V.} and Hinse, {T. C.} and M. Hundertmark and Jorgensen, {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 = may,

doi = "10.1051/0004-6361/201016111",

language = "English",

volume = "529",

journal = "Astronomy & Astrophysics",

issn = "0004-6361",

publisher = "EDP SCIENCES S A",

}

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, Kozlowski, 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, Prester, DD, Donatowicz, J, Greenhill, J, Hoffman, M, Jablonski, F, Kane, SR, Kains, N, Marquette, J-B, 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, C-U, Mallia, F, Maury, A, Monard, LAG, Moorhouse, D, Morgan, N, Natusch, T, Ofek, EO, Park, B-G, 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, Harpsoe, K, Hessman, FV, Hinse, TC, Hundertmark, M, Jorgensen, 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 & Astrophysics, vol. 529, A102. https://doi.org/10.1051/0004-6361/201016111

TY - JOUR

T1 - MOA-2009-BLG-387Lb: 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 - Kozlowski, 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 - Prester, D. Dominis

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 - Harpsoe, K.

AU - Hessman, F. V.

AU - Hinse, T. C.

AU - Hundertmark, M.

AU - Jorgensen, 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 - 2011/5

Y1 - 2011/5

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-circle dot < M-host < 0.49 M-circle dot 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 m(p) = 2.6 Jupiter masses for the median host mass, M = 0.19 M-circle dot.Methods. The host mass is determined from two "higher order" microlensing parameters. One of these, the angular Einstein radius theta(E) = 0.31 +/- 0.03 mas has been accurately measured, but the other (the microlens parallax pi(E), 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 < D-L < 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-circle dot < M-host < 0.49 M-circle dot 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 m(p) = 2.6 Jupiter masses for the median host mass, M = 0.19 M-circle dot.Methods. The host mass is determined from two "higher order" microlensing parameters. One of these, the angular Einstein radius theta(E) = 0.31 +/- 0.03 mas has been accurately measured, but the other (the microlens parallax pi(E), 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 < D-L < 7.9 kpc, 1.1 AU < a < 2.7 AU, and 3.8 yr < P < 7.6 yr, respectively.

KW - gravitational lensing: micro

KW - methods: data analysis

KW - planets and satellites: detection

KW - methods: numerical

KW - instrumentation: adaptive optics

KW - instrumentation: photometers

KW - GALACTIC BULGE

KW - MICROLENSING EVENT

KW - JUPITER/SATURN ANALOG

KW - GIANT PLANETS

KW - SNOW LINE

KW - STARS

KW - MASSES

KW - PHOTOMETRY

KW - COOL

KW - LUMINOSITY

U2 - 10.1051/0004-6361/201016111

DO - 10.1051/0004-6361/201016111

M3 - Article

SN - 0004-6361

VL - 529

JO - Astronomy & Astrophysics

JF - Astronomy & Astrophysics

M1 - A102

ER -

MOA-2009-BLG-387Lb: a massive planet orbiting an M dwarf

Abstract

Keywords

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Astrophysics in St Andrews: Astrophysics in St Andrews / SUPA (Continuan of Rolling Grant - XPP089

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