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. Fouque; P. Browne; C. Han; C. Snodgrass; F. Finet; K. Furusawa; K. Harpsoe; W. Allen; M. Hundertmark; M. Freeman; D. Suzuki; 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. Kozlowski; Y. Lee; F. Mallia; A. Maury; D. Maoz; J. McCormick; L. A. G. Monard; D. Moorhouse; J. A. Munoz; 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. Jorgensen; 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

doi: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. Fouque, P. Browne, C. Han, C. Snodgrass, F. Finet, K. Furusawa, K. Harpsoe, W. Allen, M. HundertmarkM. Freeman, D. Suzuki, 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. Kozlowski, Y. Lee, F. Mallia, A. Maury, D. Maoz, J. McCormick, L. A. G. Monard, D. Moorhouse, J. A. Munoz, 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. Jorgensen, 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

School of Physics and Astronomy

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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) x 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,theta(E), along with a standard Galactic model indicates a host star mass of M-L = 0.38(-0.18)(+0.34) M-circle dot and a planet mass of M-p = 50(-24)(+44)M(circle plus), which is half the mass of Saturn. This analysis also yields a planet-star three-dimensional separation of a = 2.4(-0.6)(+1.2) AU and a distance to the planetary system of D-L = 6.1(-1.2)(+1.1) kpc. This separation is similar to 2 times the distance of the snow line, a separation similar to most of the other planets discovered by microlensing.

Original language	English
Pages (from-to)	120
Number of pages	10
Journal	Astrophysical Journal
Volume	728
Issue number	2
DOIs	https://doi.org/10.1088/0004-637X/728/2/120
Publication status	Published - 20 Feb 2011

Keywords

gravitational lensing: micro
planetary systems
DIFFERENCE IMAGE-ANALYSIS
MAGNIFICATION MICROLENSING EVENTS
CLUMP ABSOLUTE MAGNITUDE
GALACTIC BULGE
SNOW LINE
JUPITER/SATURN ANALOG
EXTRASOLAR PLANETS
OPTICAL DEPTH
GIANT PLANETS
PARALLAX

Access to Document

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

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

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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., Fouque, P., Browne, P., Han, C., Snodgrass, C., Finet, F., Furusawa, K., Harpsoe, K., Allen, W., ... Menzies, J. (2011). A Sub-Saturn Mass Planet, MOA-2009-BLG-319Lb. Astrophysical Journal, 728(2), 120. https://doi.org/10.1088/0004-637X/728/2/120

@article{cae0ef89f9ce40f688d0959204a4b28e,

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) x 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,theta(E), along with a standard Galactic model indicates a host star mass of M-L = 0.38(-0.18)(+0.34) M-circle dot and a planet mass of M-p = 50(-24)(+44)M(circle plus), which is half the mass of Saturn. This analysis also yields a planet-star three-dimensional separation of a = 2.4(-0.6)(+1.2) AU and a distance to the planetary system of D-L = 6.1(-1.2)(+1.1) kpc. This separation is similar to 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, DIFFERENCE IMAGE-ANALYSIS, MAGNIFICATION MICROLENSING EVENTS, CLUMP ABSOLUTE MAGNITUDE, GALACTIC BULGE, SNOW LINE, JUPITER/SATURN ANALOG, EXTRASOLAR PLANETS, OPTICAL DEPTH, GIANT PLANETS, PARALLAX",

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. Fouque and P. Browne and C. Han and C. Snodgrass and F. Finet and K. Furusawa and K. Harpsoe and W. Allen and M. Hundertmark and M. Freeman and D. Suzuki 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. Kozlowski and Y. Lee and F. Mallia and A. Maury and D. Maoz and J. McCormick and Monard, {L. A. G.} and D. Moorhouse and Munoz, {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 Jorgensen, {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",

year = "2011",

month = feb,

day = "20",

doi = "10.1088/0004-637X/728/2/120",

language = "English",

volume = "728",

pages = "120",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "American Astronomical Society",

number = "2",

}

Miyake, N, Sumi, T, Dong, S, Street, R, Mancini, L, Gould, A, Bennett, DP, Tsapras, Y, Yee, JC, Albrow, MD, Bond, IA, Fouque, P, Browne, P, Han, C, Snodgrass, C, Finet, F, Furusawa, K, Harpsoe, K, Allen, W, Hundertmark, M, Freeman, M, Suzuki, 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, K-H, Janczak, J, Kaspi, S, Lee, C-U, Koo, J-R, Kozlowski, S, Lee, Y, Mallia, F, Maury, A, Maoz, D, McCormick, J, Monard, LAG, Moorhouse, D, Munoz, 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, Jorgensen, 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, pp. 120. 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 - Fouque, P.

AU - Browne, P.

AU - Han, C.

AU - Snodgrass, C.

AU - Finet, F.

AU - Furusawa, K.

AU - Harpsoe, K.

AU - Allen, W.

AU - Hundertmark, M.

AU - Freeman, M.

AU - Suzuki, 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 - Kozlowski, 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 - Munoz, 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 - Jorgensen, 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) x 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,theta(E), along with a standard Galactic model indicates a host star mass of M-L = 0.38(-0.18)(+0.34) M-circle dot and a planet mass of M-p = 50(-24)(+44)M(circle plus), which is half the mass of Saturn. This analysis also yields a planet-star three-dimensional separation of a = 2.4(-0.6)(+1.2) AU and a distance to the planetary system of D-L = 6.1(-1.2)(+1.1) kpc. This separation is similar to 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) x 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,theta(E), along with a standard Galactic model indicates a host star mass of M-L = 0.38(-0.18)(+0.34) M-circle dot and a planet mass of M-p = 50(-24)(+44)M(circle plus), which is half the mass of Saturn. This analysis also yields a planet-star three-dimensional separation of a = 2.4(-0.6)(+1.2) AU and a distance to the planetary system of D-L = 6.1(-1.2)(+1.1) kpc. This separation is similar to 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

KW - DIFFERENCE IMAGE-ANALYSIS

KW - MAGNIFICATION MICROLENSING EVENTS

KW - CLUMP ABSOLUTE MAGNITUDE

KW - GALACTIC BULGE

KW - SNOW LINE

KW - JUPITER/SATURN ANALOG

KW - EXTRASOLAR PLANETS

KW - OPTICAL DEPTH

KW - GIANT PLANETS

KW - PARALLAX

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

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

M3 - Article

SN - 0004-637X

VL - 728

SP - 120

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 2

ER -

A Sub-Saturn Mass Planet, MOA-2009-BLG-319Lb

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Keywords

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

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