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OGLE-2011-BLG-0265Lb: A Jovian Microlensing Planet Orbiting an M Dwarf

Skowron, J, Shin, I-G, Udalski, A, Han, C, Sumi, T, Shvartzvald, Y, Gould, A, Prester, DD, Street, RA, Jorgensen, UG, Bennett, DP, Bozza, V, Szymanski, MK, Kubiak, M, Pietrzynski, G, Soszynski, I, Poleski, R, Kozlowski, S, Pietrukowicz, P, Ulaczyk, K , Wyrzykowski, L, Abe, F, Bhattacharya, A, Bond, IA, Botzler, CS, Freeman, M, Fukui, A, Fukunaga, D, Itow, Y, Ling, CH, Koshimoto, N, Masuda, K, Matsubara, Y, Muraki, Y, Namba, S, Ohnishi, K, Philpott, LC, Rattenbury, N, Saito, T, Sullivan, DJ, Suzuki, D, Tristram, PJ, Yock, PCM, Maoz, D, Kaspi, S, Friedmann, M, Almeida, LA, Batista, V, Christie, G, Choi, J-Y, Depoy, DL, Gaudi, BS, Henderson, C, Hwang, K-H, Jablonski, F, Jung, YK, Lee, C-U, McCormick, J, Natusch, T, Ngan, H, Park, H, Pogge, RW, Yee, JC, Albrow, MD, Bachelet, E, Beaulieu, J-P, Brillant, S, Caldwell, JAR, Cassan, A, Cole, A, Corrales, E, Coutures, CH, Dieters, S, Donatowicz, J, Fouque, P, Greenhill, J, Kains, N, Kane, SR, Kubas, D, Marquette, J-B, Martin, R, Menzies, J, Pollard, KR, Ranc, C, Sahu, KC, Wambsganss, J, Williams, A, Wouters, D, Tsapras, Y, Bramich, DM, Horne, K, Hundertmark, M, Snodgrass, C, Steele, IA, Alsubai, KA, Browne, P, Burgdorf, MJ, Novati, SC, Dodds, P, Dominik, M, Dreizler, S, Fang, X-S, Gu, C-H, Hardis, K, Harpsoe, K, Hessman, FV, Hinse, TC, Hornstrup, A, Jessen-Hansen, J, Kerins, E, Liebig, C, Lund, M, Lundkvist, M, Mancini, L, Mathiasen, M, Penny, MT, Rahvar, S, Ricci, D, Scarpetta, G, Skottfelt, J, Southworth, J, Surdej, J, Tregloan-Reed, J and Wertz, O (2015) OGLE-2011-BLG-0265Lb: A Jovian Microlensing Planet Orbiting an M Dwarf. Astrophysical Journal, 804 (1). ISSN 0004-637X

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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 ${{M}_{{\rm p}}}=0.9\pm 0.3\ {{M}_{{\rm J}}}$, and the planet is orbiting a star with a mass $M=0.22\pm 0.06\ {{M}_{\odot }}$. The second possible configuration (2σ away) consists of a planet with ${{M}_{{\rm p}}}=0.6\pm 0.3\ {{M}_{{\rm J}}}$ and host star with $M=0.14\pm 0.06\ {{M}_{\odot }}$. 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.

Item Type: Article
Uncontrolled Keywords: 0201 Astronomical And Space Sciences, 0305 Organic Chemistry, 0306 Physical Chemistry (Incl. Structural)
Subjects: Q Science > QB Astronomy
Q Science > QC Physics
Divisions: Astrophysics Research Institute
Publisher: American Astronomical Society; IOP Publishing
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Date Deposited: 09 May 2017 09:15
Last Modified: 18 May 2022 09:56
DOI or ID number: 10.1088/0004-637X/804/1/33
URI: https://researchonline.ljmu.ac.uk/id/eprint/6387
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