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

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; To. Saito; T. Sako; D. J. Sullivan; W. L. Sweatman; P. J. Tristram; P. C. M. Yock; [No Value] MOA Collaboration; J. P. Beaulieu; A. Cole; Ch. Coutures; M. F. Duran; J. Greenhill; F. Jablonski; U. Marboeuf; E. Martioli; E. Pedretti; O. Pejcha; P. Rojo; M. D. Albrow; S. Brillant; M. Bode; D. M. Bramich; M. J. Burgdorf; J. A. R. Caldwell; H. Calitz; E. Corrales; S. Dieters; D. Dominis Prester; J. Donatowicz; K. Hill; M. Hoffman; K. Horne; U. G. Jørgensen; N. Kains; S. Kane; J. B. Marquette; R. Martin; P. Meintjes; J. Menzies; K. R. Pollard; K. C. Sahu; C. Snodgrass; I. Steele; R. Street; Y. Tsapras; J. Wambsganss; A. Williams; M. Zub; [No Value] PLANET Collaboration; M. K. Szyma¿ski; M. Kubiak; G. Pietrzy¿ski; I. Soszy¿ski; O. Szewczyk; ¿. Wyrzykowski; K. Ulaczyk; [No Value] OGLE Collaboration; W. Allen; G. W. Christie; D. L. DePoy; B. S. Gaudi; C. Han; J. Janczak; C.-U. Lee; J. McCormick; F. Mallia; B. Monard; T. Natusch; B.-G. Park; R. W. Pogge; R. Santallo; [No Value] ¿FUN Collaboration

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

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. ItowK. 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, To. Saito, T. Sako, D. J. Sullivan, W. L. Sweatman, P. J. Tristram, P. C. M. Yock, [No Value] MOA Collaboration, J. P. Beaulieu, A. Cole, Ch. Coutures, M. F. Duran, J. Greenhill, F. Jablonski, U. Marboeuf, E. Martioli, E. Pedretti, O. Pejcha, P. Rojo, M. D. Albrow, S. Brillant, M. Bode, D. M. Bramich, M. J. Burgdorf, J. A. R. Caldwell, H. Calitz, E. Corrales, S. Dieters, D. Dominis Prester, J. Donatowicz, K. Hill, M. Hoffman, K. Horne, U. G. Jørgensen, N. Kains, S. Kane, J. B. Marquette, R. Martin, P. Meintjes, J. Menzies, K. R. Pollard, K. C. Sahu, C. Snodgrass, I. Steele, R. Street, Y. Tsapras, J. Wambsganss, A. Williams, M. Zub, [No Value] PLANET Collaboration, M. K. Szyma¿ski, M. Kubiak, G. Pietrzy¿ski, I. Soszy¿ski, O. Szewczyk, ¿. Wyrzykowski, K. Ulaczyk, [No Value] OGLE Collaboration, W. Allen, G. W. Christie, D. L. DePoy, B. S. Gaudi, C. Han, J. Janczak, C.-U. Lee, J. McCormick, F. Mallia, B. Monard, T. Natusch, B.-G. Park, R. W. Pogge, R. Santallo, [No Value] ¿FUN Collaboration

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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 sun 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
Journal	The Astrophysical Journal
Volume	710
Issue number	2
Publication status	Published - 1 Feb 2010

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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., Hearnshaw, J. B., ... ¿FUN Collaboration, N. V. (2010). A Cold Neptune-Mass Planet OGLE-2007-BLG-368Lb: Cold Neptunes Are Common. The Astrophysical Journal, 710(2), 1641-1653. http://adsabs.harvard.edu/abs/2010ApJ...710.1641S

@article{be980fb92a9d437eb5cdf67b5ad79aae,

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 sun 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.",

author = "T. Sumi and Bennett, {D. P.} and Bond, {I. A.} 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 Botzler, {C. S.} and A. Fukui and K. Furusawa and Hearnshaw, {J. B.} and Y. Itow and K. Kamiya and Kilmartin, {P. M.} and A. Korpela and W. Lin and Ling, {C. H.} 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 Perrott, {Y. C.} and N. Rattenbury and To. Saito and T. Sako and Sullivan, {D. J.} and Sweatman, {W. L.} and Tristram, {P. J.} and Yock, {P. C. M.} and {MOA Collaboration}, {[No Value]} and Beaulieu, {J. P.} and A. Cole and Ch. Coutures and Duran, {M. F.} and J. Greenhill and F. Jablonski and U. Marboeuf and E. Martioli and E. Pedretti and O. Pejcha and P. Rojo and Albrow, {M. D.} and S. Brillant and M. Bode and Bramich, {D. M.} and Burgdorf, {M. J.} and Caldwell, {J. A. R.} and H. Calitz and E. Corrales and S. Dieters and {Dominis Prester}, D. and J. Donatowicz and K. Hill and M. Hoffman and K. Horne and J{\o}rgensen, {U. G.} and N. Kains and S. Kane and Marquette, {J. B.} and R. Martin and P. Meintjes and J. Menzies and Pollard, {K. R.} and Sahu, {K. C.} and C. Snodgrass and I. Steele and R. Street and Y. Tsapras and J. Wambsganss and A. Williams and M. Zub and {PLANET Collaboration}, {[No Value]} and Szyma¿ski, {M. K.} and M. Kubiak and G. Pietrzy¿ski and I. Soszy¿ski and O. Szewczyk and ¿. Wyrzykowski and K. Ulaczyk and {OGLE Collaboration}, {[No Value]} and W. Allen and Christie, {G. W.} and DePoy, {D. L.} and Gaudi, {B. S.} and C. Han and J. Janczak and C.-U. Lee and J. McCormick and F. Mallia and B. Monard and T. Natusch and B.-G. Park and Pogge, {R. W.} and R. Santallo and {¿FUN Collaboration}, {[No Value]}",

year = "2010",

month = feb,

day = "1",

language = "English",

volume = "710",

pages = "1641--1653",

journal = "The Astrophysical Journal",

issn = "1538-4357",

publisher = "American Astronomical Society",

number = "2",

}

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, MOA Collaboration, NV, Beaulieu, JP, Cole, A, Coutures, C, Duran, MF, Greenhill, J, Jablonski, F, Marboeuf, U, Martioli, E, Pedretti, E, Pejcha, O, Rojo, P, Albrow, MD, Brillant, S, Bode, M, Bramich, DM, Burgdorf, MJ, Caldwell, JAR, Calitz, H, Corrales, E, Dieters, S, Dominis Prester, D, Donatowicz, J, Hill, K, Hoffman, M, Horne, K, Jørgensen, UG, Kains, N, Kane, S, Marquette, JB, Martin, R, Meintjes, P, Menzies, J, Pollard, KR, Sahu, KC, Snodgrass, C, Steele, I, Street, R, Tsapras, Y, Wambsganss, J, Williams, A, Zub, M, PLANET Collaboration, NV, Szyma¿ski, MK, Kubiak, M, Pietrzy¿ski, G, Soszy¿ski, I, Szewczyk, O, Wyrzykowski, Ulaczyk, K, OGLE Collaboration, NV, Allen, W, Christie, GW, DePoy, DL, Gaudi, BS, Han, C, Janczak, J, Lee, C-U, McCormick, J, Mallia, F, Monard, B, Natusch, T, Park, B-G, Pogge, RW, Santallo, R & ¿FUN Collaboration, NV 2010, 'A Cold Neptune-Mass Planet OGLE-2007-BLG-368Lb: Cold Neptunes Are Common', The Astrophysical Journal, vol. 710, no. 2, pp. 1641-1653. <http://adsabs.harvard.edu/abs/2010ApJ...710.1641S>

TY - JOUR

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

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, To.

AU - Sako, T.

AU - Sullivan, D. J.

AU - Sweatman, W. L.

AU - Tristram, P. J.

AU - Yock, P. C. M.

AU - MOA Collaboration, [No Value]

AU - Beaulieu, J. P.

AU - Cole, A.

AU - Coutures, Ch.

AU - Duran, M. F.

AU - Greenhill, J.

AU - Jablonski, F.

AU - Marboeuf, U.

AU - Martioli, E.

AU - Pedretti, E.

AU - Pejcha, O.

AU - Rojo, P.

AU - Albrow, M. D.

AU - Brillant, S.

AU - Bode, M.

AU - Bramich, D. M.

AU - Burgdorf, M. J.

AU - Caldwell, J. A. R.

AU - Calitz, H.

AU - Corrales, E.

AU - Dieters, S.

AU - Dominis Prester, D.

AU - Donatowicz, J.

AU - Hill, K.

AU - Hoffman, M.

AU - Horne, K.

AU - Jørgensen, U. G.

AU - Kains, N.

AU - Kane, S.

AU - Marquette, J. B.

AU - Martin, R.

AU - Meintjes, P.

AU - Menzies, J.

AU - Pollard, K. R.

AU - Sahu, K. C.

AU - Snodgrass, C.

AU - Steele, I.

AU - Street, R.

AU - Tsapras, Y.

AU - Wambsganss, J.

AU - Williams, A.

AU - Zub, M.

AU - PLANET Collaboration, [No Value]

AU - Szyma¿ski, M. K.

AU - Kubiak, M.

AU - Pietrzy¿ski, G.

AU - Soszy¿ski, I.

AU - Szewczyk, O.

AU - Wyrzykowski, ¿.

AU - Ulaczyk, K.

AU - OGLE Collaboration, [No Value]

AU - Allen, W.

AU - Christie, G. W.

AU - DePoy, D. L.

AU - Gaudi, B. S.

AU - Han, C.

AU - Janczak, J.

AU - Lee, C.-U.

AU - McCormick, J.

AU - Mallia, F.

AU - Monard, B.

AU - Natusch, T.

AU - Park, B.-G.

AU - Pogge, R. W.

AU - Santallo, R.

AU - ¿FUN Collaboration, [No Value]

PY - 2010/2/1

Y1 - 2010/2/1

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 sun 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 sun 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.

M3 - Article

SN - 1538-4357

VL - 710

SP - 1641

EP - 1653

JO - The Astrophysical Journal

JF - The Astrophysical Journal

IS - 2

ER -

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

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