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

Research output: Contribution to journalArticle

14 Citations (Scopus)

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.

Original languageEnglish
JournalAstrophysical Journal
Volume728
Issue number2
DOIs
Publication statusPublished - 20 Feb 2011
Externally publishedYes

Fingerprint

Saturn
planets
planet
magnification
stars
radii
telescopes
dwarf stars
galactic bulge
M stars
Bayesian analysis
planetary systems
snow
mass ratios
light curve

Keywords

  • Gravitational lensing: micro
  • Planetary systems

ASJC Scopus subject areas

  • Space and Planetary Science
  • Astronomy and Astrophysics

Cite this

Miyake, N., Sumi, T., Dong, S., Street, R., Mancini, L., Gould, A., ... Menzies, J. (2011). A sub-Saturn mass planet, MOA-2009-BLG-319Lb. Astrophysical Journal, 728(2). https://doi.org/10.1088/0004-637X/728/2/120

A sub-Saturn mass planet, MOA-2009-BLG-319Lb. / Miyake, N.; Sumi, T.; Dong, Subo; 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.; Hundertmark, M.; Freeman, M.; Suzuk, D.; Abe, F.; Botzler, C. S.; Douchin, D.; Fukui, A.; Hayashi, F.; 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.; Muraki, Y.; Nagayama, T.; Nishimoto, K.; Ohnishi, K.; Perrott, Y. C.; Rattenbury, N.; Saito, To; Skuljan, L.; Sullivan, D. J.; Sweatman, W. L.; Tristram, P. J.; Wada, K.; Yock, P. C M; Bolt, G.; Bos, M.; Christie, G. W.; Depoy, D. L.; Drummond, J.; Gal-Yam, A.; Gaudi, B. S.; Gorbikov, E.; Higgins, D.; Hwang, K. H.; Janczak, J.; Kaspi, S.; Lee, C. U.; Koo, J. R.; Kozllowski, S.; Lee, Y.; Mallia, F.; Maury, A.; Maoz, D.; McCormick, J.; Monard, L. A G; Moorhouse, D.; Muñoz, J. A.; Natusch, T.; Ofek, E. O.; Pogge, R. W.; Polishook, D.; Santallo, R.; Shporer, A.; Spector, O.; Thornley, G.; Allan, A.; Bramich, D. M.; Horne, K.; Kains, N.; Steele, I.; Bozza, V.; Burgdorf, M. J.; Calchi Novati, S.; Dominik, M.; Dreizler, S.; Glitrup, M.; Hessman, F. V.; Hinse, T. C.; Jørgensen, U. G.; 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, J. P.; Brillant, S.; Cassan, A.; Cole, A.; Corrales, E.; Coutures, Ch; Dieters, S.; Greenhill, J.; Kubas, D.; Menzies, J.

In: Astrophysical Journal, Vol. 728, No. 2, 20.02.2011.

Research output: Contribution to journalArticle

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 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
Miyake N, Sumi T, Dong S, Street R, Mancini L, Gould A et al. A sub-Saturn mass planet, MOA-2009-BLG-319Lb. Astrophysical Journal. 2011 Feb 20;728(2). https://doi.org/10.1088/0004-637X/728/2/120
Miyake, N. ; Sumi, T. ; Dong, Subo ; 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. ; Hundertmark, M. ; Freeman, M. ; Suzuk, D. ; Abe, F. ; Botzler, C. S. ; Douchin, D. ; Fukui, A. ; Hayashi, F. ; 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. ; Muraki, Y. ; Nagayama, T. ; Nishimoto, K. ; Ohnishi, K. ; Perrott, Y. C. ; Rattenbury, N. ; Saito, To ; Skuljan, L. ; Sullivan, D. J. ; Sweatman, W. L. ; Tristram, P. J. ; Wada, K. ; Yock, P. C M ; Bolt, G. ; Bos, M. ; Christie, G. W. ; Depoy, D. L. ; Drummond, J. ; Gal-Yam, A. ; Gaudi, B. S. ; Gorbikov, E. ; Higgins, D. ; Hwang, K. H. ; Janczak, J. ; Kaspi, S. ; Lee, C. U. ; Koo, J. R. ; Kozllowski, S. ; Lee, Y. ; Mallia, F. ; Maury, A. ; Maoz, D. ; McCormick, J. ; Monard, L. A G ; Moorhouse, D. ; Muñoz, J. A. ; Natusch, T. ; Ofek, E. O. ; Pogge, R. W. ; Polishook, D. ; Santallo, R. ; Shporer, A. ; Spector, O. ; Thornley, G. ; Allan, A. ; Bramich, D. M. ; Horne, K. ; Kains, N. ; Steele, I. ; Bozza, V. ; Burgdorf, M. J. ; Calchi Novati, S. ; Dominik, M. ; Dreizler, S. ; Glitrup, M. ; Hessman, F. V. ; Hinse, T. C. ; Jørgensen, U. G. ; 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, J. P. ; Brillant, S. ; Cassan, A. ; Cole, A. ; Corrales, E. ; Coutures, Ch ; Dieters, S. ; Greenhill, J. ; Kubas, D. ; Menzies, J. / A sub-Saturn mass planet, MOA-2009-BLG-319Lb. In: Astrophysical Journal. 2011 ; Vol. 728, No. 2.
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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.",
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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.

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

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U2 - 10.1088/0004-637X/728/2/120

DO - 10.1088/0004-637X/728/2/120

M3 - Article

AN - SCOPUS:84891196283

VL - 728

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

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ER -