A Cold Neptune-Mass Planet OGLE-2007-BLG-368Lb: Cold Neptunes Are Common

The μFUN Collaboration; T. Sumi; D.~P. Bennett; I.~A. Bond; A. Udalski; V. Batista; M. Dominik; P. Fouqué; D. Kubas; A. Gould; B. Macintosh; K. Cook; S. Dong; L. Skuljan; A. Cassan; F. Abe; C.~S. Botzler; A. Fukui; K. Furusawa; J.~B. Hearnshaw; Y. Itow; K. Kamiya; P.~M. Kilmartin; A. Korpela; W. Lin; C.~H. Ling; K. Masuda; Y. Matsubara; N. Miyake; Y. Muraki; M. Nagaya; T. Nagayama; K. Ohnishi; T. Okumura; Y.~C. Perrott; N. Rattenbury; T. Saito; T. Sako; D.~J. Sullivan; W.~L. Sweatman; P.~J. Tristram; P.~C.~M. Yock; MOA Collaboration; J.~P. Beaulieu; A. Cole; C. Coutures; M.~F. Duran; E. Pedretti; R. Martin; A. Williams; C.-U. Lee

doi:10.1088/0004-637X/710/2/1641

A Cold Neptune-Mass Planet OGLE-2007-BLG-368Lb: Cold Neptunes Are Common

The μFUN Collaboration, T. Sumi, D.~P. Bennett, I.~A. Bond, A. Udalski, V. Batista, M. Dominik, P. Fouqué, D. Kubas, A. Gould, B. Macintosh, K. Cook, S. Dong, L. Skuljan, A. Cassan, F. Abe, C.~S. Botzler, A. Fukui, K. Furusawa, J.~B. HearnshawY. Itow, K. Kamiya, P.~M. Kilmartin, A. Korpela, W. Lin, C.~H. Ling, K. Masuda, Y. Matsubara, N. Miyake, Y. Muraki, M. Nagaya, T. Nagayama, K. Ohnishi, T. Okumura, Y.~C. Perrott, N. Rattenbury, T. Saito, T. Sako, D.~J. Sullivan, W.~L. Sweatman, P.~J. Tristram, P.~C.~M. Yock, MOA Collaboration, J.~P. Beaulieu, A. Cole, C. Coutures, M.~F. Duran, E. Pedretti, R. Martin, A. Williams, C.-U. Lee

School of Engineering & Physical Sciences

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

181 Citations (Scopus)

Abstract

We present the discovery of a Neptune-mass planet OGLE-2007-BLG-368Lb with a planet-star mass ratio of q = [9.5 ± 2.1] × 10–5 via gravitational microlensing. The planetary deviation was detected in real-time thanks to the high cadence of the Microlensing Observations in Astrophysics survey, real-time light-curve monitoring and intensive follow-up observations. A Bayesian analysis returns the stellar mass and distance at Ml = 0.64+0.21 –0.26 M ☉ and Dl = 5.9+0.9 –1.4 kpc, respectively, so the mass and separation of the planet are Mp = 20+7 –8 M ⊕ and a = 3.3+1.4 –0.8 AU, respectively. This discovery adds another cold Neptune-mass planet to the planetary sample discovered by microlensing, which now comprises four cold Neptune/super-Earths, five gas giant planets, and another sub-Saturn mass planet whose nature is unclear. The discovery of these 10 cold exoplanets by the microlensing method implies that the mass ratio function of cold exoplanets scales as dN pl/dlog q vprop q –0.7±0.2 with a 95% confidence level upper limit of n < –0.35 (where dN pl/dlog q vprop qn ). As microlensing is most sensitive to planets beyond the snow-line, this implies that Neptune-mass planets are at least three times more common than Jupiters in this region at the 95% confidence level.

Original language	English
Pages (from-to)	1641-1653
Number of pages	13
Journal	Astrophysical Journal
Volume	710
Issue number	2
DOIs	https://doi.org/10.1088/0004-637X/710/2/1641
Publication status	Published - Feb 2010

Keywords

gravitational lensing: micro, planetary systems

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10.1088/0004-637X/710/2/1641

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The μFUN Collaboration, Sumi, T., Bennett, D. P., Bond, I. A., Udalski, A., Batista, V., Dominik, M., Fouqué, P., Kubas, D., Gould, A., Macintosh, B., Cook, K., Dong, S., Skuljan, L., Cassan, A., Abe, F., Botzler, C. S., Fukui, A., Furusawa, K., ... Lee, C.-U. (2010). A Cold Neptune-Mass Planet OGLE-2007-BLG-368Lb: Cold Neptunes Are Common. Astrophysical Journal, 710(2), 1641-1653. https://doi.org/10.1088/0004-637X/710/2/1641

@article{fd9255ffa264487f84997582101f15d7,

title = "A Cold Neptune-Mass Planet OGLE-2007-BLG-368Lb: Cold Neptunes Are Common",

abstract = "We present the discovery of a Neptune-mass planet OGLE-2007-BLG-368Lb with a planet-star mass ratio of q = [9.5 ± 2.1] × 10–5 via gravitational microlensing. The planetary deviation was detected in real-time thanks to the high cadence of the Microlensing Observations in Astrophysics survey, real-time light-curve monitoring and intensive follow-up observations. A Bayesian analysis returns the stellar mass and distance at Ml = 0.64+0.21 –0.26 M ☉ and Dl = 5.9+0.9 –1.4 kpc, respectively, so the mass and separation of the planet are Mp = 20+7 –8 M ⊕ and a = 3.3+1.4 –0.8 AU, respectively. This discovery adds another cold Neptune-mass planet to the planetary sample discovered by microlensing, which now comprises four cold Neptune/super-Earths, five gas giant planets, and another sub-Saturn mass planet whose nature is unclear. The discovery of these 10 cold exoplanets by the microlensing method implies that the mass ratio function of cold exoplanets scales as dN pl/dlog q vprop q –0.7±0.2 with a 95% confidence level upper limit of n < –0.35 (where dN pl/dlog q vprop qn ). As microlensing is most sensitive to planets beyond the snow-line, this implies that Neptune-mass planets are at least three times more common than Jupiters in this region at the 95% confidence level.",

keywords = "gravitational lensing: micro, planetary systems",

author = "{The μFUN Collaboration} and T. Sumi and D.~P. Bennett and I.~A. Bond and A. Udalski and V. Batista and M. Dominik and P. Fouqu{\'e} and D. Kubas and A. Gould and B. Macintosh and K. Cook and S. Dong and L. Skuljan and A. Cassan and F. Abe and C.~S. Botzler and A. Fukui and K. Furusawa and J.~B. Hearnshaw and Y. Itow and K. Kamiya and P.~M. Kilmartin and A. Korpela and W. Lin and C.~H. Ling and K. Masuda and Y. Matsubara and N. Miyake and Y. Muraki and M. Nagaya and T. Nagayama and K. Ohnishi and T. Okumura and Y.~C. Perrott and N. Rattenbury and T. Saito and T. Sako and D.~J. Sullivan and W.~L. Sweatman and P.~J. Tristram and P.~C.~M. Yock and MOA Collaboration and J.~P. Beaulieu and A. Cole and C. Coutures and M.~F. Duran and E. Pedretti and R. Martin and A. Williams and C.-U. Lee",

year = "2010",

month = feb,

doi = "10.1088/0004-637X/710/2/1641",

language = "English",

volume = "710",

pages = "1641--1653",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "IOP Publishing ",

number = "2",

}

The μFUN Collaboration, Sumi, T, Bennett, DP, Bond, IA, Udalski, A, Batista, V, Dominik, M, Fouqué, P, Kubas, D, Gould, A, Macintosh, B, Cook, K, Dong, S, Skuljan, L, Cassan, A, Abe, F, Botzler, CS, Fukui, A, Furusawa, K, Hearnshaw, JB, Itow, Y, Kamiya, K, Kilmartin, PM, Korpela, A, Lin, W, Ling, CH, Masuda, K, Matsubara, Y, Miyake, N, Muraki, Y, Nagaya, M, Nagayama, T, Ohnishi, K, Okumura, T, Perrott, YC, Rattenbury, N, Saito, T, Sako, T, Sullivan, DJ, Sweatman, WL, Tristram, PJ, Yock, PCM, Collaboration, MOA, Beaulieu, JP, Cole, A, Coutures, C, Duran, MF, Pedretti, E, Martin, R, Williams, A & Lee, C-U 2010, 'A Cold Neptune-Mass Planet OGLE-2007-BLG-368Lb: Cold Neptunes Are Common', Astrophysical Journal, vol. 710, no. 2, pp. 1641-1653. https://doi.org/10.1088/0004-637X/710/2/1641

TY - JOUR

T1 - A Cold Neptune-Mass Planet OGLE-2007-BLG-368Lb: Cold Neptunes Are Common

AU - The μFUN Collaboration

AU - Sumi, T.

AU - Bennett, D.~P.

AU - Bond, I.~A.

AU - Udalski, A.

AU - Batista, V.

AU - Dominik, M.

AU - Fouqué, P.

AU - Kubas, D.

AU - Gould, A.

AU - Macintosh, B.

AU - Cook, K.

AU - Dong, S.

AU - Skuljan, L.

AU - Cassan, A.

AU - Abe, F.

AU - Botzler, C.~S.

AU - Fukui, A.

AU - Furusawa, K.

AU - Hearnshaw, J.~B.

AU - Itow, Y.

AU - Kamiya, K.

AU - Kilmartin, P.~M.

AU - Korpela, A.

AU - Lin, W.

AU - Ling, C.~H.

AU - Masuda, K.

AU - Matsubara, Y.

AU - Miyake, N.

AU - Muraki, Y.

AU - Nagaya, M.

AU - Nagayama, T.

AU - Ohnishi, K.

AU - Okumura, T.

AU - Perrott, Y.~C.

AU - Rattenbury, N.

AU - Saito, T.

AU - Sako, T.

AU - Sullivan, D.~J.

AU - Sweatman, W.~L.

AU - Tristram, P.~J.

AU - Yock, P.~C.~M.

AU - Collaboration, MOA

AU - Beaulieu, J.~P.

AU - Cole, A.

AU - Coutures, C.

AU - Duran, M.~F.

AU - Pedretti, E.

AU - Martin, R.

AU - Williams, A.

AU - Lee, C.-U.

PY - 2010/2

Y1 - 2010/2

N2 - We present the discovery of a Neptune-mass planet OGLE-2007-BLG-368Lb with a planet-star mass ratio of q = [9.5 ± 2.1] × 10–5 via gravitational microlensing. The planetary deviation was detected in real-time thanks to the high cadence of the Microlensing Observations in Astrophysics survey, real-time light-curve monitoring and intensive follow-up observations. A Bayesian analysis returns the stellar mass and distance at Ml = 0.64+0.21 –0.26 M ☉ and Dl = 5.9+0.9 –1.4 kpc, respectively, so the mass and separation of the planet are Mp = 20+7 –8 M ⊕ and a = 3.3+1.4 –0.8 AU, respectively. This discovery adds another cold Neptune-mass planet to the planetary sample discovered by microlensing, which now comprises four cold Neptune/super-Earths, five gas giant planets, and another sub-Saturn mass planet whose nature is unclear. The discovery of these 10 cold exoplanets by the microlensing method implies that the mass ratio function of cold exoplanets scales as dN pl/dlog q vprop q –0.7±0.2 with a 95% confidence level upper limit of n < –0.35 (where dN pl/dlog q vprop qn ). As microlensing is most sensitive to planets beyond the snow-line, this implies that Neptune-mass planets are at least three times more common than Jupiters in this region at the 95% confidence level.

AB - We present the discovery of a Neptune-mass planet OGLE-2007-BLG-368Lb with a planet-star mass ratio of q = [9.5 ± 2.1] × 10–5 via gravitational microlensing. The planetary deviation was detected in real-time thanks to the high cadence of the Microlensing Observations in Astrophysics survey, real-time light-curve monitoring and intensive follow-up observations. A Bayesian analysis returns the stellar mass and distance at Ml = 0.64+0.21 –0.26 M ☉ and Dl = 5.9+0.9 –1.4 kpc, respectively, so the mass and separation of the planet are Mp = 20+7 –8 M ⊕ and a = 3.3+1.4 –0.8 AU, respectively. This discovery adds another cold Neptune-mass planet to the planetary sample discovered by microlensing, which now comprises four cold Neptune/super-Earths, five gas giant planets, and another sub-Saturn mass planet whose nature is unclear. The discovery of these 10 cold exoplanets by the microlensing method implies that the mass ratio function of cold exoplanets scales as dN pl/dlog q vprop q –0.7±0.2 with a 95% confidence level upper limit of n < –0.35 (where dN pl/dlog q vprop qn ). As microlensing is most sensitive to planets beyond the snow-line, this implies that Neptune-mass planets are at least three times more common than Jupiters in this region at the 95% confidence level.

KW - gravitational lensing: micro, planetary systems

U2 - 10.1088/0004-637X/710/2/1641

DO - 10.1088/0004-637X/710/2/1641

M3 - Article

SN - 0004-637X

VL - 710

SP - 1641

EP - 1653

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 2

ER -

A Cold Neptune-Mass Planet OGLE-2007-BLG-368Lb: Cold Neptunes Are Common

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