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dc.contributor.authorFukui, A.
dc.contributor.authorGould, A.
dc.contributor.authorSumi, T.
dc.contributor.authorBennett, D. P.
dc.contributor.authorBond, I. A.
dc.contributor.authorHan, C.
dc.contributor.authorSuzuki, D.
dc.contributor.authorBeaulieu, J.-P.
dc.contributor.authorBatista, V.
dc.contributor.authorUdalski, A.
dc.contributor.authorStreet, R. A.
dc.contributor.authorTsapras, Y.
dc.contributor.authorHundertmark, Markus Peter Gerhard
dc.contributor.authorAbe, F.
dc.contributor.authorBhattacharya, A.
dc.contributor.authorFreeman, M.
dc.contributor.authorItow, Y.
dc.contributor.authorLing, C. H.
dc.contributor.authorKoshimoto, N.
dc.contributor.authorMasuda, K.
dc.contributor.authorMatsubara, Y.
dc.contributor.authorMuraki, Y.
dc.contributor.authorOhnishi, K.
dc.contributor.authorPhilpott, L. C.
dc.contributor.authorRattenbury, N.
dc.contributor.authorSaito, T.
dc.contributor.authorSullivan, D. J.
dc.contributor.authorTristram, P. J.
dc.contributor.authorYonehara, A.
dc.contributor.authorChoi, J.-Y.
dc.contributor.authorChristie, G. W.
dc.contributor.authorDePoy, D. L.
dc.contributor.authorDong, Subo
dc.contributor.authorDrummond, J.
dc.contributor.authorGaudi, B. S.
dc.contributor.authorHwang, K.-H.
dc.contributor.authorKavka, A.
dc.contributor.authorLee, C.-U.
dc.contributor.authorMcCormick, J.
dc.contributor.authorNatusch, T.
dc.contributor.authorNgan, H.
dc.contributor.authorPark, H.
dc.contributor.authorPogge, R. W.
dc.contributor.authorShin, I.-G.
dc.contributor.authorTan, T.-G.
dc.contributor.authorYee, J. C.
dc.contributor.authorSzymański, M. K.
dc.contributor.authorPietrzyński, G.
dc.contributor.authorSoszyński, I.
dc.contributor.authorPoleski, R.
dc.contributor.authorKozłowski, S.
dc.contributor.authorPietrukowicz, P.
dc.contributor.authorUlaczyk, K.
dc.contributor.authorWyrzykowski, Ł.
dc.contributor.authorBramich, D. M.
dc.contributor.authorBrowne, Paul
dc.contributor.authorDominik, Martin
dc.contributor.authorHorne, Keith Douglas
dc.contributor.authorIpatov, S.
dc.contributor.authorKains, N.
dc.contributor.authorSnodgrass, C.
dc.contributor.authorSteele, I. A.
dc.date.accessioned2015-09-29T09:40:04Z
dc.date.available2015-09-29T09:40:04Z
dc.date.issued2015-08-11
dc.identifier.citationFukui , A , Gould , A , Sumi , T , Bennett , D P , Bond , I A , Han , C , Suzuki , D , Beaulieu , J-P , Batista , V , Udalski , A , Street , R A , Tsapras , Y , Hundertmark , M P G , Abe , F , Bhattacharya , A , Freeman , M , Itow , Y , Ling , C H , Koshimoto , N , Masuda , K , Matsubara , Y , Muraki , Y , Ohnishi , K , Philpott , L C , Rattenbury , N , Saito , T , Sullivan , D J , Tristram , P J , Yonehara , A , Choi , J-Y , Christie , G W , DePoy , D L , Dong , S , Drummond , J , Gaudi , B S , Hwang , K-H , Kavka , A , Lee , C-U , McCormick , J , Natusch , T , Ngan , H , Park , H , Pogge , R W , Shin , I-G , Tan , T-G , Yee , J C , Szymański , M K , Pietrzyński , G , Soszyński , I , Poleski , R , Kozłowski , S , Pietrukowicz , P , Ulaczyk , K , Wyrzykowski , Ł , Bramich , D M , Browne , P , Dominik , M , Horne , K D , Ipatov , S , Kains , N , Snodgrass , C & Steele , I A 2015 , ' OGLE-2012-BLG-0563Lb : a Saturn-mass planet around an M dwarf with the mass constrained by Subaru AO imaging ' , Astrophysical Journal , vol. 809 , no. 1 . https://doi.org/10.1088/0004-637X/809/1/74en
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 220037999
dc.identifier.otherPURE UUID: 8d578f63-e1e0-4b1c-8800-d9a1dfdf627e
dc.identifier.otherBibCode: 2015ApJ...809...74F
dc.identifier.otherScopus: 84945264841
dc.identifier.otherWOS: 000361653500074
dc.identifier.otherORCID: /0000-0002-3202-0343/work/75996732
dc.identifier.urihttps://hdl.handle.net/10023/7562
dc.descriptionA.F. was supported by the Astrobiology Project of the Center for Novel Science Initiatives (CNSI), National Institutes of Natural Sciences (NINS; Grant Number AB261005). T.S. acknowledges the financial support from the JSPS, JSPS23103002, JSPS24253004, and JSPS26247023. The MOA project is supported by grants JSPS25103508 and 23340064. NJR is a Royal Society of New Zealand Rutherford Discovery Fellow. Work by C.H. was supported by Creative Research Initiative Program (2009-0081561) of National Research Foundation of Korea. S.D. is supported by "the Strategic Priority Research Program—The Emergence of Cosmological Structures" of the Chinese Academy of Sciences (grant No. 09000000). The OGLE project has received funding from the National Science Centre, Poland, grant MAESTRO 2014/14/A/ST9/00121 to A.U. C.S. received funding from the European Union Seventh Framework Programme (FP7/2007–2013) under grant agreement No. 268421. K.A., D.M.B., M.D., K.H., M.H., C.L., C.S., R.A.S., and Y.T. would like to thank the Qatar Foundation for support from QNRF grant NPRP-09-476-1-078.en
dc.description.abstractWe report the discovery of a microlensing exoplanet OGLE-2012-BLG-0563Lb with the planet–star mass ratio of ∼1 x 10-3. Intensive photometric observations of a high-magnification microlensing event allow us to detect a clear signal of the planet. Although no parallax signal is detected in the light curve, we instead succeed at detecting the flux from the host star in high-resolution JHK'-band images obtained by the Subaru/AO188 and Infrared Camera and Spectrograph instruments, allowing us to constrain the absolute physical parameters of the planetary system. With the help of spectroscopic information about the source star obtained during the high-magnification state by Bensby et al., we find that the lens system is located at 1.3-0.8+0.6 kpc from us, and consists of an M dwarf (0.34+0.12-0.20MΘ) orbited by a Saturn-mass planet (0.39-0.23+0.14 MJup) at the projected separation of 0.74-0.42+0.26 AU (close model) or 4.3-2.5+1.5 AU (wide model). The probability of contamination in the host star's flux, which would reduce the masses by a factor of up to three, is estimated to be 17%. This possibility can be tested by future high-resolution imaging. We also estimate the (J-Ks) and (H-Ks) colors of the host star, which are marginally consistent with a low metallicity mid-to-early M dwarf, although further observations are required for the metallicity to be conclusive. This is the fifth sub-Jupiter-mass (0.2 < mp/MJup < 1) microlensing planet around an M dwarf with the mass well constrained. The relatively rich harvest of sub-Jupiters around M dwarfs is contrasted with a possible paucity of ~1–2 Jupiter-mass planets around the same type of star, which can be explained by the planetary formation process in the core-accretion scheme.
dc.language.isoeng
dc.relation.ispartofAstrophysical Journalen
dc.rights© 2015. The American Astronomical Society. All rights reserved. This work is made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at http://dx.doi.org/10.1088/0004-637X/809/1/74en
dc.subjectPlanetary systemsen
dc.subjectPlanets and satellites: detectionen
dc.subjectPlanets and satellites: gaseous planetsen
dc.subjectStars: late-typeen
dc.subjectTechniques: high angular resolutionen
dc.subjectTechniques: photometricen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectNDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleOGLE-2012-BLG-0563Lb : a Saturn-mass planet around an M dwarf with the mass constrained by Subaru AO imagingen
dc.typeJournal articleen
dc.contributor.sponsorThe Royal Societyen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.1088/0004-637X/809/1/74
dc.description.statusPeer revieweden
dc.identifier.urlhttp://adsabs.harvard.edu/abs/2015ApJ...809...74Fen
dc.identifier.grantnumberUF100010 / UF130581en
dc.identifier.grantnumberST/J001651/1en
dc.identifier.grantnumberST/M001296/1en
dc.identifier.grantnumberST/K001515/1en


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