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Mikkel Nørup Lund

OGLE-2011-BLG-0265Lb: A JOVIAN MICROLENSING PLANET ORBITING AN M DWARF

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DOI

  • J. Skowron, Univ Warsaw Observ, Warsaw University Observatory
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  • I. -G. Shin, Chungbuk Natl Univ, Chungbuk National University, Inst Astrophys, Dept Phys
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  • A. Udalski, Univ Warsaw Observ, Warsaw University Observatory
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  • C. Han, Chungbuk Natl Univ, Chungbuk National University, Inst Astrophys, Dept Phys
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  • T. Sumi, Osaka Univ, Osaka University, Grad Sch Sci, Dept Earth & Space Sci
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  • Y. Shvartzvald, Tel Aviv Univ, Tel Aviv University, Sch Phys & Astron
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  • A. Gould, Ohio State Univ, Ohio State University, Dept Astron
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  • D. Dominis Prester, Univ Rijeka, University of Rijeka, Fac Arts & Sci, Dept Phys
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  • R. A. Street, Las Cumbres Observ Global Telescope Network
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  • U. G. Jørgensen, Univ Copenhagen, Niels Bohr Institute, University of Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, Ctr Star & Planet Format, Geol Museum
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  • D. P. Bennett, University of Notre Dame
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  • V. Bozza, Ist Nazl Fis Nucl, Istituto Nazionale di Fisica Nucleare, LNS
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  • M. K. Szymanski, Univ Warsaw Observ, Warsaw University Observatory
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  • M. Kubiak, Univ Warsaw Observ, Warsaw University Observatory
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  • G. Pietrzynski, Univ Warsaw Observ, Warsaw University Observatory
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  • I. Soszynski, Univ Concepcion, Universidad de Concepcion, Dept Astron
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  • R. Poleski, Ohio State Univ, Ohio State University, Dept Astron
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  • S. Kozlowski, Univ Warsaw Observ, Warsaw University Observatory
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  • P. Pietrukowicz, Univ Warsaw Observ, Warsaw University Observatory
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  • K. Ulaczyk, Univ Warsaw Observ, Warsaw University Observatory
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  • L. Wyrzykowski, Univ Cambridge, University of Cambridge, Inst Astron
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  • F. Abe, Nagoya Univ, Nagoya University, Solar Terr Environm Lab
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  • A. Bhattacharya, University of Notre Dame
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  • I. A. Bond, Massey Univ, Massey University, Inst Informat & Math Sci, North Shore Mail Ctr
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  • C. S. Botzler, Univ Auckland, University of Auckland, Dept Phys
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  • M. Freeman, Univ Auckland, University of Auckland, Dept Phys
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  • A. Fukui, Natl Astron Observ Japan, National Astronomical Observatory of Japan, National Institutes of Natural Sciences (NINS) - Japan, Okayama Astrophys Observ
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  • D. Fukunaga, Nagoya Univ, Nagoya University, Solar Terr Environm Lab
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  • Y. Itow, Nagoya Univ, Nagoya University, Solar Terr Environm Lab
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  • C. H. Ling, Massey Univ, Massey University, Inst Informat & Math Sci, North Shore Mail Ctr
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  • N. Koshimoto, Osaka Univ, Osaka University, Grad Sch Sci, Dept Earth & Space Sci
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  • K. Masuda, Nagoya Univ, Nagoya University, Solar Terr Environm Lab
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  • Y. Matsubara, Nagoya Univ, Nagoya University, Solar Terr Environm Lab
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  • Y. Muraki, Konan Univ, Konan University, Dept Phys
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  • S. Namba, Osaka Univ, Osaka University, Grad Sch Sci, Dept Earth & Space Sci
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  • K. Ohnishi, Nagano Natl Coll Technol
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  • L. C. Philpott, Univ British Columbia, University of British Columbia, Dept Earth Ocean & Atmospher Sci
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  • N. Rattenbury, Univ Auckland, University of Auckland, Dept Phys
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  • T. Saito, Tokyo Metropolitan Coll Ind Technol
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  • D. J. Sullivan, Victoria Univ, Victoria University Wellington, Sch Chem & Phys Sci
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  • D. Suzuki, Osaka Univ, Osaka University, Grad Sch Sci, Dept Earth & Space Sci
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  • P. J. Tristram, Victoria Univ, Victoria University Wellington, Sch Chem & Phys Sci
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  • P. C. M. Yock, Univ Auckland, University of Auckland, Dept Phys
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  • D. Maoz, Tel Aviv Univ, Tel Aviv University, Sch Phys & Astron
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  • S. Kaspi, Tel Aviv Univ, Tel Aviv University, Sch Phys & Astron
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  • M. Friedmann, Tel Aviv Univ, Tel Aviv University, Sch Phys & Astron
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  • L. A. Almeida, Inst Nacl Pesquisas Espaciais, Instituto Nacional de Pesquisas Espaciais (INPE), Div Astrofis
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  • J. Jessen-Hansen
  • Mikkel Nørup Lund
  • M. Lundkvist
  • OGLE Collaboration
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  • MOA Collaboration
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  • Wise Grp
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  • FUN Collaboration
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  • PLANET Collaboration
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  • RoboNet Collaboration
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  • MiNDSTEp Consortium

We report the discovery of a Jupiter-mass planet orbiting an M-dwarf star that gave rise to the microlensing event OGLE-2011-BLG-0265. Such a system is very rare among known planetary systems and thus the discovery is important for theoretical studies of planetary formation and evolution. High-cadence temporal coverage of the planetary signal, combined with extended observations throughout the event, allows us to accurately model the observed light curve. However, the final microlensing solution remains degenerate, yielding two possible configurations of the planet and the host star. In the case of the preferred solution, the mass of the planet is M-p = 0.9 +/- 0.3 M-J, and the planet is orbiting a star with a mass M = 0.22 +/- 0.06 M-circle dot. The second possible configuration (2 sigma away) consists of a planet with M-p = 0.6 +/- 0.3M(J) and host star with M = 0.14 +/- 0.06M(circle dot). The system is located in the Galactic disk 3-4 kpc toward the Galactic bulge. In both cases, with an orbit size of 1.5-2.0 AU, the planet is a "cold Jupiter"-located well beyond the "snow line" of the host star. Currently available data make the secure selection of the correct solution difficult, but there are prospects for lifting the degeneracy with additional follow-up observations in the future, when the lens and source star separate.

OriginalsprogEngelsk
Artikelnummer33
TidsskriftAstrophysical Journal
Vol/bind804
Nummer1
Antal sider12
ISSN0004-637X
DOI
StatusUdgivet - 2015

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