A sub-Saturn mass planet, MOA-2009-BLG-319Lb

N. Miyake; T. Sumi; Subo Dong; R. Street; L. Mancini; A. Gould; D. P. Bennett; Y. Tsapras; J. C. Yee; M. D. Albrow; I. A. Bond; P. Fouqué; P. Browne; C. Han; C. Snodgrass; F. Finet; K. Furusawa; K. Harpsøe; W. Allen; M. Hundertmark; M. Freeman; D. Suzuk; F. Abe; C. S. Botzler; D. Douchin; A. Fukui; F. Hayashi; 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; Y. Muraki; T. Nagayama; K. Nishimoto; K. Ohnishi; Y. C. Perrott; N. Rattenbury; To Saito; L. Skuljan; D. J. Sullivan; W. L. Sweatman; P. J. Tristram; K. Wada; P. C.M. Yock; G. Bolt; M. Bos; G. W. Christie; D. L. Depoy; J. Drummond; A. Gal-Yam; B. S. Gaudi; E. Gorbikov; D. Higgins; K. H. Hwang; J. Janczak; S. Kaspi; C. U. Lee; J. R. Koo; S. Kozllowski; Y. Lee; F. Mallia; A. Maury; D. Maoz; J. McCormick; L. A.G. Monard; D. Moorhouse; J. A. Muñoz; T. Natusch; E. O. Ofek; R. W. Pogge; D. Polishook; R. Santallo; A. Shporer; O. Spector; G. Thornley; A. Allan; D. M. Bramich; K. Horne; N. Kains; I. Steele; V. Bozza; M. J. Burgdorf; S. Calchi Novati; M. Dominik; S. Dreizler; M. Glitrup; F. V. Hessman; T. C. Hinse; U. G. Jørgensen; C. Liebig; G. Maier; M. Mathiasen; S. Rahvar; D. Ricci; G. Scarpetta; J. Skottfelt; J. Southworth; J. Surdej; J. Wambsganss; F. Zimmer; V. Batista; J. P. Beaulieu; S. Brillant; A. Cassan; A. Cole; E. Corrales; Ch Coutures; S. Dieters; J. Greenhill; D. Kubas; J. Menzies; K. Harpsoe

doi:https://doi.org/10.1088/0004-637X/728/2/120

A sub-Saturn mass planet, MOA-2009-BLG-319Lb

N. Miyake, T. Sumi, Subo Dong, R. Street, L. Mancini, A. Gould, D. P. Bennett, Y. Tsapras, J. C. Yee, M. D. Albrow, I. A. Bond, P. Fouqué, P. Browne, C. Han, C. Snodgrass, F. Finet, K. Furusawa, K. Harpsøe, W. Allen, M. HundertmarkM. Freeman, D. Suzuk, F. Abe, C. S. Botzler, D. Douchin, A. Fukui, F. Hayashi, 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, Y. Muraki, T. Nagayama, K. Nishimoto, K. Ohnishi, Y. C. Perrott, N. Rattenbury, To Saito, L. Skuljan, D. J. Sullivan, W. L. Sweatman, P. J. Tristram, K. Wada, P. C.M. Yock, G. Bolt, M. Bos, G. W. Christie, D. L. Depoy, J. Drummond, A. Gal-Yam, B. S. Gaudi, E. Gorbikov, D. Higgins, K. H. Hwang, J. Janczak, S. Kaspi, C. U. Lee, J. R. Koo, S. Kozllowski, Y. Lee, F. Mallia, A. Maury, D. Maoz, J. McCormick, L. A.G. Monard, D. Moorhouse, J. A. Muñoz, T. Natusch, E. O. Ofek, R. W. Pogge, D. Polishook, R. Santallo, A. Shporer, O. Spector, G. Thornley, A. Allan, D. M. Bramich, K. Horne, N. Kains, I. Steele, V. Bozza, M. J. Burgdorf, S. Calchi Novati, M. Dominik, S. Dreizler, M. Glitrup, F. V. Hessman, T. C. Hinse, U. G. Jørgensen, C. Liebig, G. Maier, M. Mathiasen, S. Rahvar, D. Ricci, G. Scarpetta, J. Skottfelt, J. Southworth, J. Surdej, J. Wambsganss, F. Zimmer, V. Batista, J. P. Beaulieu, S. Brillant, A. Cassan, A. Cole, E. Corrales, Ch Coutures, S. Dieters, J. Greenhill, D. Kubas, J. Menzies, K. Harpsoe

Tel Aviv University, Technion - Israel Institute of Technology

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

Abstract

We report the gravitational microlensing discovery of a sub-Saturn mass planet, MOA-2009-BLG-319Lb, orbiting a K-or M-dwarf star in the inner Galactic disk or Galactic bulge. The high-cadence observations of the MOA-II survey discovered this microlensing event and enabled its identification as a high-magnification event approximately 24 hr prior to peak magnification. As a result, the planetary signal at the peak of this light curve was observed by 20 different telescopes, which is the largest number of telescopes to contribute to a planetary discovery to date. The microlensing model for this event indicates a planet-star mass ratio of q = (3.95 ± 0.02) × 10^-4 and a separation of d = 0.97537 ± 0.00007 in units of the Einstein radius. A Bayesian analysis based on the measured Einstein radius crossing time, t _e, and angular Einstein radius, θ_e, along with a standard Galactic model indicates a host star mass of M_l = 0.38 ^+0.34_-0.18 M_⊙ and a planet mass of M _p = 50⁺⁴⁴_-24 M_>, which is half the mass of Saturn. This analysis also yields a planet-star three-dimensional separation of a = 2.4^+1.2_-0.6 AU and a distance to the planetary system of D_l = 6.1^+1.1_-1.2 kpc. This separation is ∼2 times the distance of the snow line, a separation similar to most of the other planets discovered by microlensing.

Original language	English
Journal	Astrophysical Journal
Volume	728
Issue number	2
DOIs	https://doi.org/10.1088/0004-637X/728/2/120
State	Published - 20 Feb 2011

Keywords

Gravitational lensing: micro
Planetary systems

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

Access to Document

https://doi.org/10.1088/0004-637X/728/2/120

Cite this

Miyake, N., Sumi, T., Dong, S., Street, R., Mancini, L., Gould, A., Bennett, D. P., Tsapras, Y., Yee, J. C., Albrow, M. D., Bond, I. A., Fouqué, P., Browne, P., Han, C., Snodgrass, C., Finet, F., Furusawa, K., Harpsøe, K., Allen, W., ... Harpsoe, K. (2011). A sub-Saturn mass planet, MOA-2009-BLG-319Lb. Astrophysical Journal, 728(2). https://doi.org/10.1088/0004-637X/728/2/120

@article{6f920b64fa6d4f13ba8566a8fd238011,

title = "A sub-Saturn mass planet, MOA-2009-BLG-319Lb",

abstract = "We report the gravitational microlensing discovery of a sub-Saturn mass planet, MOA-2009-BLG-319Lb, orbiting a K-or M-dwarf star in the inner Galactic disk or Galactic bulge. The high-cadence observations of the MOA-II survey discovered this microlensing event and enabled its identification as a high-magnification event approximately 24 hr prior to peak magnification. As a result, the planetary signal at the peak of this light curve was observed by 20 different telescopes, which is the largest number of telescopes to contribute to a planetary discovery to date. The microlensing model for this event indicates a planet-star mass ratio of q = (3.95 ± 0.02) × 10-4 and a separation of d = 0.97537 ± 0.00007 in units of the Einstein radius. A Bayesian analysis based on the measured Einstein radius crossing time, t e, and angular Einstein radius, θe, along with a standard Galactic model indicates a host star mass of Ml = 0.38 +0.34-0.18 M⊙ and a planet mass of M p = 50+44-24 M>, which is half the mass of Saturn. This analysis also yields a planet-star three-dimensional separation of a = 2.4+1.2-0.6 AU and a distance to the planetary system of Dl = 6.1+1.1-1.2 kpc. This separation is ∼2 times the distance of the snow line, a separation similar to most of the other planets discovered by microlensing.",

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

author = "N. Miyake and T. Sumi and Subo Dong and R. Street and L. Mancini and A. Gould and Bennett, {D. P.} and Y. Tsapras and Yee, {J. C.} and Albrow, {M. D.} and Bond, {I. A.} and P. Fouqu{\'e} and P. Browne and C. Han and C. Snodgrass and F. Finet and K. Furusawa and K. Harps{\o}e and W. Allen and M. Hundertmark and M. Freeman and D. Suzuk and F. Abe and Botzler, {C. S.} and D. Douchin and A. Fukui and F. Hayashi 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 Y. Muraki and T. Nagayama and K. Nishimoto and K. Ohnishi and Perrott, {Y. C.} and N. Rattenbury and To Saito and L. Skuljan and Sullivan, {D. J.} and Sweatman, {W. L.} and Tristram, {P. J.} and K. Wada and Yock, {P. C.M.} and G. Bolt and M. Bos and Christie, {G. W.} and Depoy, {D. L.} and J. Drummond and A. Gal-Yam and Gaudi, {B. S.} and E. Gorbikov and D. Higgins and Hwang, {K. H.} and J. Janczak and S. Kaspi and Lee, {C. U.} and Koo, {J. R.} and S. Kozllowski and Y. Lee and F. Mallia and A. Maury and D. Maoz and J. McCormick and Monard, {L. A.G.} and D. Moorhouse and Mu{\~n}oz, {J. A.} and T. Natusch and Ofek, {E. O.} and Pogge, {R. W.} and D. Polishook and R. Santallo and A. Shporer and O. Spector and G. Thornley and A. Allan and Bramich, {D. M.} and K. Horne and N. Kains and I. Steele and V. Bozza and Burgdorf, {M. J.} and {Calchi Novati}, S. and M. Dominik and S. Dreizler and M. Glitrup and Hessman, {F. V.} and Hinse, {T. C.} and J{\o}rgensen, {U. G.} and C. Liebig and G. Maier and M. Mathiasen and S. Rahvar and D. Ricci and G. Scarpetta and J. Skottfelt and J. Southworth and J. Surdej and J. Wambsganss and F. Zimmer and V. Batista and Beaulieu, {J. P.} and S. Brillant and A. Cassan and A. Cole and E. Corrales and Ch Coutures and S. Dieters and J. Greenhill and D. Kubas and J. Menzies and K. Harpsoe",

note = "JSPS [JSPS20340052, JSPS18253002, JSPS20740104]; Nagoya University; MEXT of Japan; Massey University and the University of Auckland; NASA [NNX07AL71G, NNX10AI81G, NNG04GL51G]; NSF [AST-0708890, AST-0757888]; National Research Foundation of Korea [2009-0081561]; Department of Culture, Arts, and Leisure (DCAL), Northern Ireland; Communaute francaise de Belgique-Actions de recherche concertees-Academie universitaire Wallonie-EuropeThe MOA project and a part of authors were supported by the Grant-in-Aid for Scientific Research, the grant JSPS20340052, JSPS18253002, JSPS Research fellowships, the Global COE Program of Nagoya University {"}Quest for Fundamental Principles in the Universe{"} from JSPS and MEXT of Japan, the for Research and Technology, and grants-in-aid from Massey University and the University of Auckland. N.M. was supported by JSPS Research Fellowships for Young Scientists. T.S. was supported by the grant JSPS20740104. D.P.B. was supported by grants NNX07AL71G and NNX10AI81G from NASA and AST-0708890 from the NSF. A.G. and S.D. were supported in part by NSF AST-0757888. A.G., S.D., S.G., and R.P. were supported in part by NASA NNG04GL51G. Work by S.D. was performed in part under contract with the California Institute of Technology (Caltech) funded by NASA through the Sagan Fellowship Program. J.C.Y. was supported by an NSF Graduate Research Fellowship. Work by C.H. was supported by the Creative Research Initiative program (2009-0081561) of the National Research Foundation of Korea. Astronomical research at Armagh Observatory was supported by the Department of Culture, Arts, and Leisure (DCAL), Northern Ireland, UK. F.F., D.R., and J.S. acknowledge support from the Communaute francaise de Belgique-Actions de recherche concertees-Academie universitaire Wallonie-Europe.",

year = "2011",

month = feb,

day = "20",

doi = "https://doi.org/10.1088/0004-637X/728/2/120",

language = "الإنجليزيّة",

volume = "728",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "IOP Publishing Ltd.",

number = "2",

}

Miyake, N, Sumi, T, Dong, S, Street, R, Mancini, L, Gould, A, Bennett, DP, Tsapras, Y, Yee, JC, Albrow, MD, Bond, IA, Fouqué, P, Browne, P, Han, C, Snodgrass, C, Finet, F, Furusawa, K, Harpsøe, K, Allen, W, Hundertmark, M, Freeman, M, Suzuk, D, Abe, F, Botzler, CS, Douchin, D, Fukui, A, Hayashi, F, Hearnshaw, JB, Hosaka, S, Itow, Y, Kamiya, K, Kilmartin, PM, Korpela, A, Lin, W, Ling, CH, Makita, S, Masuda, K, Matsubara, Y, Muraki, Y, Nagayama, T, Nishimoto, K, Ohnishi, K, Perrott, YC, Rattenbury, N, Saito, T, Skuljan, L, Sullivan, DJ, Sweatman, WL, Tristram, PJ, Wada, K, Yock, PCM, Bolt, G, Bos, M, Christie, GW, Depoy, DL, Drummond, J, Gal-Yam, A, Gaudi, BS, Gorbikov, E, Higgins, D, Hwang, KH, Janczak, J, Kaspi, S, Lee, CU, Koo, JR, Kozllowski, S, Lee, Y, Mallia, F, Maury, A, Maoz, D, McCormick, J, Monard, LAG, Moorhouse, D, Muñoz, JA, Natusch, T, Ofek, EO, Pogge, RW, Polishook, D, Santallo, R, Shporer, A, Spector, O, Thornley, G, Allan, A, Bramich, DM, Horne, K, Kains, N, Steele, I, Bozza, V, Burgdorf, MJ, Calchi Novati, S, Dominik, M, Dreizler, S, Glitrup, M, Hessman, FV, Hinse, TC, Jørgensen, UG, Liebig, C, Maier, G, Mathiasen, M, Rahvar, S, Ricci, D, Scarpetta, G, Skottfelt, J, Southworth, J, Surdej, J, Wambsganss, J, Zimmer, F, Batista, V, Beaulieu, JP, Brillant, S, Cassan, A, Cole, A, Corrales, E, Coutures, C, Dieters, S, Greenhill, J, Kubas, D, Menzies, J & Harpsoe, K 2011, 'A sub-Saturn mass planet, MOA-2009-BLG-319Lb', Astrophysical Journal, vol. 728, no. 2. https://doi.org/10.1088/0004-637X/728/2/120

TY - JOUR

T1 - A sub-Saturn mass planet, MOA-2009-BLG-319Lb

AU - Miyake, N.

AU - Sumi, T.

AU - Dong, Subo

AU - Street, R.

AU - Mancini, L.

AU - Gould, A.

AU - Bennett, D. P.

AU - Tsapras, Y.

AU - Yee, J. C.

AU - Albrow, M. D.

AU - Bond, I. A.

AU - Fouqué, P.

AU - Browne, P.

AU - Han, C.

AU - Snodgrass, C.

AU - Finet, F.

AU - Furusawa, K.

AU - Harpsøe, K.

AU - Allen, W.

AU - Hundertmark, M.

AU - Freeman, M.

AU - Suzuk, D.

AU - Abe, F.

AU - Botzler, C. S.

AU - Douchin, D.

AU - Fukui, A.

AU - Hayashi, F.

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 - Muraki, Y.

AU - Nagayama, T.

AU - Nishimoto, K.

AU - Ohnishi, K.

AU - Perrott, Y. C.

AU - Rattenbury, N.

AU - Saito, To

AU - Skuljan, L.

AU - Sullivan, D. J.

AU - Sweatman, W. L.

AU - Tristram, P. J.

AU - Wada, K.

AU - Yock, P. C.M.

AU - Bolt, G.

AU - Bos, M.

AU - Christie, G. W.

AU - Depoy, D. L.

AU - Drummond, J.

AU - Gal-Yam, A.

AU - Gaudi, B. S.

AU - Gorbikov, E.

AU - Higgins, D.

AU - Hwang, K. H.

AU - Janczak, J.

AU - Kaspi, S.

AU - Lee, C. U.

AU - Koo, J. R.

AU - Kozllowski, S.

AU - Lee, Y.

AU - Mallia, F.

AU - Maury, A.

AU - Maoz, D.

AU - McCormick, J.

AU - Monard, L. A.G.

AU - Moorhouse, D.

AU - Muñoz, J. A.

AU - Natusch, T.

AU - Ofek, E. O.

AU - Pogge, R. W.

AU - Polishook, D.

AU - Santallo, R.

AU - Shporer, A.

AU - Spector, O.

AU - Thornley, G.

AU - Allan, A.

AU - Bramich, D. M.

AU - Horne, K.

AU - Kains, N.

AU - Steele, I.

AU - Bozza, V.

AU - Burgdorf, M. J.

AU - Calchi Novati, S.

AU - Dominik, M.

AU - Dreizler, S.

AU - Glitrup, M.

AU - Hessman, F. V.

AU - Hinse, T. C.

AU - Jørgensen, U. G.

AU - Liebig, C.

AU - Maier, G.

AU - Mathiasen, M.

AU - Rahvar, S.

AU - Ricci, D.

AU - Scarpetta, G.

AU - Skottfelt, J.

AU - Southworth, J.

AU - Surdej, J.

AU - Wambsganss, J.

AU - Zimmer, F.

AU - Batista, V.

AU - Beaulieu, J. P.

AU - Brillant, S.

AU - Cassan, A.

AU - Cole, A.

AU - Corrales, E.

AU - Coutures, Ch

AU - Dieters, S.

AU - Greenhill, J.

AU - Kubas, D.

AU - Menzies, J.

AU - Harpsoe, K.

N1 - JSPS [JSPS20340052, JSPS18253002, JSPS20740104]; Nagoya University; MEXT of Japan; Massey University and the University of Auckland; NASA [NNX07AL71G, NNX10AI81G, NNG04GL51G]; NSF [AST-0708890, AST-0757888]; National Research Foundation of Korea [2009-0081561]; Department of Culture, Arts, and Leisure (DCAL), Northern Ireland; Communaute francaise de Belgique-Actions de recherche concertees-Academie universitaire Wallonie-EuropeThe MOA project and a part of authors were supported by the Grant-in-Aid for Scientific Research, the grant JSPS20340052, JSPS18253002, JSPS Research fellowships, the Global COE Program of Nagoya University "Quest for Fundamental Principles in the Universe" from JSPS and MEXT of Japan, the for Research and Technology, and grants-in-aid from Massey University and the University of Auckland. N.M. was supported by JSPS Research Fellowships for Young Scientists. T.S. was supported by the grant JSPS20740104. D.P.B. was supported by grants NNX07AL71G and NNX10AI81G from NASA and AST-0708890 from the NSF. A.G. and S.D. were supported in part by NSF AST-0757888. A.G., S.D., S.G., and R.P. were supported in part by NASA NNG04GL51G. Work by S.D. was performed in part under contract with the California Institute of Technology (Caltech) funded by NASA through the Sagan Fellowship Program. J.C.Y. was supported by an NSF Graduate Research Fellowship. Work by C.H. was supported by the Creative Research Initiative program (2009-0081561) of the National Research Foundation of Korea. Astronomical research at Armagh Observatory was supported by the Department of Culture, Arts, and Leisure (DCAL), Northern Ireland, UK. F.F., D.R., and J.S. acknowledge support from the Communaute francaise de Belgique-Actions de recherche concertees-Academie universitaire Wallonie-Europe.

PY - 2011/2/20

Y1 - 2011/2/20

N2 - We report the gravitational microlensing discovery of a sub-Saturn mass planet, MOA-2009-BLG-319Lb, orbiting a K-or M-dwarf star in the inner Galactic disk or Galactic bulge. The high-cadence observations of the MOA-II survey discovered this microlensing event and enabled its identification as a high-magnification event approximately 24 hr prior to peak magnification. As a result, the planetary signal at the peak of this light curve was observed by 20 different telescopes, which is the largest number of telescopes to contribute to a planetary discovery to date. The microlensing model for this event indicates a planet-star mass ratio of q = (3.95 ± 0.02) × 10-4 and a separation of d = 0.97537 ± 0.00007 in units of the Einstein radius. A Bayesian analysis based on the measured Einstein radius crossing time, t e, and angular Einstein radius, θe, along with a standard Galactic model indicates a host star mass of Ml = 0.38 +0.34-0.18 M⊙ and a planet mass of M p = 50+44-24 M>, which is half the mass of Saturn. This analysis also yields a planet-star three-dimensional separation of a = 2.4+1.2-0.6 AU and a distance to the planetary system of Dl = 6.1+1.1-1.2 kpc. This separation is ∼2 times the distance of the snow line, a separation similar to most of the other planets discovered by microlensing.

AB - We report the gravitational microlensing discovery of a sub-Saturn mass planet, MOA-2009-BLG-319Lb, orbiting a K-or M-dwarf star in the inner Galactic disk or Galactic bulge. The high-cadence observations of the MOA-II survey discovered this microlensing event and enabled its identification as a high-magnification event approximately 24 hr prior to peak magnification. As a result, the planetary signal at the peak of this light curve was observed by 20 different telescopes, which is the largest number of telescopes to contribute to a planetary discovery to date. The microlensing model for this event indicates a planet-star mass ratio of q = (3.95 ± 0.02) × 10-4 and a separation of d = 0.97537 ± 0.00007 in units of the Einstein radius. A Bayesian analysis based on the measured Einstein radius crossing time, t e, and angular Einstein radius, θe, along with a standard Galactic model indicates a host star mass of Ml = 0.38 +0.34-0.18 M⊙ and a planet mass of M p = 50+44-24 M>, which is half the mass of Saturn. This analysis also yields a planet-star three-dimensional separation of a = 2.4+1.2-0.6 AU and a distance to the planetary system of Dl = 6.1+1.1-1.2 kpc. This separation is ∼2 times the distance of the snow line, a separation similar to most of the other planets discovered by microlensing.

KW - Gravitational lensing: micro

KW - Planetary systems

UR - http://www.scopus.com/inward/record.url?scp=84891196283&partnerID=8YFLogxK

U2 - https://doi.org/10.1088/0004-637X/728/2/120

DO - https://doi.org/10.1088/0004-637X/728/2/120

M3 - مقالة

SN - 0004-637X

VL - 728

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 2

ER -

A sub-Saturn mass planet, MOA-2009-BLG-319Lb

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