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A COLD NEPTUNE-MASS PLANET OGLE-2007-BLG-368Lb: COLD NEPTUNES ARE COMMON

Authordc.contributor.authorSumi, T. 
Authordc.contributor.authorBennett, D. P. es_CL
Authordc.contributor.authorBond, I. A. es_CL
Authordc.contributor.authorUdalski, A. es_CL
Authordc.contributor.authorBatista, V. es_CL
Authordc.contributor.authorDominik, M. es_CL
Authordc.contributor.authorFouqué, P. es_CL
Authordc.contributor.authorKubas, D. es_CL
Authordc.contributor.authorGould, A. es_CL
Authordc.contributor.authorMacintosh, B. es_CL
Authordc.contributor.authorCook, K. es_CL
Authordc.contributor.authorDong, S. es_CL
Authordc.contributor.authorSkuljan, L. es_CL
Authordc.contributor.authorCassan, Arnaud es_CL
Authordc.contributor.authorAbe, F. es_CL
Authordc.contributor.authorBotzler, C. S. es_CL
Authordc.contributor.authorFukui, A. es_CL
Authordc.contributor.authorFurusawa, K. es_CL
Authordc.contributor.authorHearnshaw, J. B. es_CL
Authordc.contributor.authorItow, Y. es_CL
Authordc.contributor.authorKamiya, K. es_CL
Authordc.contributor.authorKilmartin, P. M. es_CL
Authordc.contributor.authorKorpela, A. es_CL
Authordc.contributor.authorLin, W. es_CL
Authordc.contributor.authorLing, C. H. es_CL
Authordc.contributor.authorMasuda, K. es_CL
Authordc.contributor.authorMatsubara, Y. es_CL
Authordc.contributor.authorMiyake, N. es_CL
Authordc.contributor.authorMuraki, Y. es_CL
Authordc.contributor.authorNagaya, M. es_CL
Authordc.contributor.authorNagayama, T. es_CL
Authordc.contributor.authorOhnishi, K. es_CL
Authordc.contributor.authorOkumura, T. es_CL
Authordc.contributor.authorPerrott, Y. C. es_CL
Authordc.contributor.authorRattenbury, N. es_CL
Authordc.contributor.authorSaito, To. es_CL
Authordc.contributor.authorSako, T. es_CL
Authordc.contributor.authorSullivan, D. J. es_CL
Authordc.contributor.authorSweatman, W. L. es_CL
Authordc.contributor.authorTristram, P. J. es_CL
Authordc.contributor.authorYock, P. C. M. es_CL
Authordc.contributor.authorBeaulieu, J. P. es_CL
Authordc.contributor.authorCole, A. es_CL
Authordc.contributor.authorCoutures, Ch. es_CL
Authordc.contributor.authorDuran, M. F. es_CL
Authordc.contributor.authorGreenhill, J. es_CL
Authordc.contributor.authorJablonski, F. es_CL
Authordc.contributor.authorMarboeuf, U. es_CL
Authordc.contributor.authorMartioli, E. es_CL
Authordc.contributor.authorPedretti, E. es_CL
Authordc.contributor.authorPejcha, O. es_CL
Authordc.contributor.authorRojo, P. es_CL
Authordc.contributor.authorAlbrow, M. D. es_CL
Authordc.contributor.authorBrillant, S. es_CL
Authordc.contributor.authorBode, Michael es_CL
Authordc.contributor.authorBramich, D. M. es_CL
Authordc.contributor.authorBurgdorf, M. J. es_CL
Authordc.contributor.authorCaldwell, J. A. R. es_CL
Authordc.contributor.authorCalitz, H. es_CL
Authordc.contributor.authorCorrales, E. es_CL
Authordc.contributor.authorDieters, S. es_CL
Authordc.contributor.authorDominis Prester, D. es_CL
Authordc.contributor.authorDonatowicz, J. es_CL
Authordc.contributor.authorHill, K. es_CL
Authordc.contributor.authorHoffman, M. es_CL
Authordc.contributor.authorHorne, Keith D. es_CL
Authordc.contributor.authorJørgensen, U. G. es_CL
Authordc.contributor.authorKains, N. es_CL
Authordc.contributor.authorKane, S. es_CL
Authordc.contributor.authorMarquette, J. B. es_CL
Authordc.contributor.authorMartin, R. es_CL
Authordc.contributor.authorMeintjes, P. es_CL
Authordc.contributor.authorMenzies, J. es_CL
Authordc.contributor.authorPollard, K. R. es_CL
Authordc.contributor.authorSahu, K. C. es_CL
Authordc.contributor.authorSnodgrass, C. es_CL
Authordc.contributor.authorSteele, I. es_CL
Authordc.contributor.authorStreet, R. es_CL
Authordc.contributor.authorTsapras, Y. es_CL
Authordc.contributor.authorWambsganss, J. es_CL
Authordc.contributor.authorWilliams, A. es_CL
Authordc.contributor.authorZub, M. es_CL
Authordc.contributor.authorSzymanski, M. K. es_CL
Authordc.contributor.authorKubiak, M. es_CL
Authordc.contributor.authorPietrzynski, G. es_CL
Authordc.contributor.authorSoszynski, I. es_CL
Authordc.contributor.authorSzewczyk, O. es_CL
Authordc.contributor.authorWyrzykowski, L. es_CL
Authordc.contributor.authorUlaczyk, K. es_CL
Authordc.contributor.authorAllen, W. es_CL
Authordc.contributor.authorChristie, G. W. es_CL
Authordc.contributor.authorL. DePoy, Darren 
Authordc.contributor.authorGaudi, B. S. 
Authordc.contributor.authorHan, C. 
Authordc.contributor.authorJanczak, J. 
Authordc.contributor.authorLee, C.-U. 
Authordc.contributor.authorMcCormick, J. 
Authordc.contributor.authorMallia, F. 
Authordc.contributor.authorMonard, B. 
Authordc.contributor.authorNatusch, T. 
Authordc.contributor.authorPark, B.-G. 
Authordc.contributor.authorPogge, R. W. 
Authordc.contributor.authorSantallo, R. 
Admission datedc.date.accessioned2010-07-27T16:20:51Z
Available datedc.date.available2010-07-27T16:20:51Z
Publication datedc.date.issued2010-02-20
Cita de ítemdc.identifier.citationThe Astrophysical Journal, 710:1641–1653, 2010 February 20en_US
Identifierdc.identifier.otherdoi:10.1088/0004-637X/710/2/1641
Identifierdc.identifier.urihttp://repositorio.uchile.cl/handle/2250/125444
Abstractdc.description.abstractWe 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 −0.26M andDl = 5.9+0.9 −1.4 kpc, respectively, so themass and separation of the planet areMp = 20+7 −8M⊕ 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 dNpl/d log q ∝ q−0.7±0.2 with a 95% confidence level upper limit of n < −0.35 (where dNpl/d log q ∝ 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.en_US
Patrocinadordc.description.sponsorshipThis work is supported by the grant JSPS18253002 and JSPS20340052 (MOA). T.S. was supported by MEXT Japan, Grant-in-Aid for Young Scientists (B), 18749004 and Grant-in- Aid for Scientific Research on Priority Areas, “Development of Extra-solar Planetary Science,” 19015005. D.P.B.was supported by grants AST-0708890 from the NSF and NNX07AL71G from NASA. The OGLE project is partially supported by the Polish MNiSW grant N20303032/4275 to AU. Work by A.G. was supported by NSF grant AST-0757888. Work by B.S.G., A.G., and R.P. is supported by NASA grant NNG04GL51G Dave Warren provided financial support for Mt Canopus Observatory. C.H. was supported by Creative Research Initiative Program (2009-0081561) of National Research Foundation of Korea (CH). B.-G.P. and C.-U.L. were supported by the grant of Korea Astronomy and Space Science Institute.en_US
Lenguagedc.language.isoenen_US
Keywordsdc.subjectgravitational lensing: microen_US
Títulodc.titleA COLD NEPTUNE-MASS PLANET OGLE-2007-BLG-368Lb: COLD NEPTUNES ARE COMMONen_US
Document typedc.typeArtículo de revistaen_US


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