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Title:
MOA-2011-BLG-262Lb: A Sub-Earth-Mass Moon Orbiting a Gas Giant Primary or a High Velocity Planetary System in the Galactic Bulge
Authors:
Bennett, D. P.; Batista, V.; Bond, I. A.; Bennett, C. S.; Suzuki, D.; Beaulieu, J.-P.; Udalski, A.; Donatowicz, J.; Bozza, V.; Abe, F.; Botzler, C. S.; Freeman, M.; Fukunaga, D.; Fukui, A.; Itow, Y.; Koshimoto, N.; Ling, C. H.; Masuda, K.; Matsubara, Y.; Muraki, Y.; Namba, S.; Ohnishi, K.; Rattenbury, N. J.; Saito, To.; Sullivan, D. J.; Sumi, T.; Sweatman, W. L.; Tristram, P. J.; Tsurumi, N.; Wada, K.; Yock, P. C. M.; MOA Collaboration; Albrow, M. D.; Bachelet, E.; Brillant, S.; Caldwell, J. A. R.; Cassan, A.; Cole, A. A.; Corrales, E.; Coutures, C.; Dieters, S.; Dominis Prester, D.; Fouqué, P.; Greenhill, J.; Horne, K.; Koo, J.-R.; Kubas, D.; Marquette, J.-B.; Martin, R.; Menzies, J. W.; Sahu, K. C.; Wambsganss, J.; Williams, A.; Zub, M.; PLANET Collaboration; Choi, J. Y.; DePoy, D. L.; Dong, Subo; Gaudi, B. S.; Gould, A.; Han, C.; Henderson, C. B.; McGregor, D.; Lee, C.-U.; Pogge, R. W.; Shin, I.-G.; Yee, J. C.; μFUN Collaboration; Szymański, M. K.; Skowron, J.; Poleski, R.; Kozłowski, S.; Wyrzykowski, Ł.; Kubiak, M.; Pietrukowicz, P.; Pietrzyński, G.; Soszyński, I.; Ulaczyk, K.; OGLE Collaboration; Tsapras, Y.; Street, R. A.; Dominik, M.; Bramich, D. M.; Browne, P.; Hundertmark, M.; Kains, N.; Snodgrass, C.; Steele, I. A.; RoboNet Collaboration; Dekany, I.; Gonzalez, O. A.; Heyrovský, D.; Kandori, R.; Kerins, E.; Lucas, P. W.; Minniti, D.; Nagayama, T.; Rejkuba, M.; Robin, A. C.; Saito, R.
Affiliation:
AA(Department of Physics, University of Notre Dame, 225 Nieuwland Science Hall, Notre Dame, IN 46556, USA; Microlensing Observations in Astrophysics (MOA) Collaboration.; Probing Lensing Anomalies NETwork (PLANET) Collaboration.; ), AB(Department of Astronomy, Ohio State University, 140 West 18th Avenue, Columbus, OH 43210, USA; UPMC-CNRS, UMR 7095, Institut d'Astrophysique de Paris, 98bis Boulevard Arago, F-75014 Paris, France; Probing Lensing Anomalies NETwork (PLANET) Collaboration.; Microlensing Follow-up Network (μFUN Collaboration).), AC(Institute of Natural and Mathematical Sciences, Massey University, Auckland 0745, New Zealand; Microlensing Observations in Astrophysics (MOA) Collaboration.), AD(Department of Physics, Massachussets Institute of Technology, Cambridge, MA 02139, USA; Goddard Space Flight Center, Greenbelt, MD 20771, USA; Probing Lensing Anomalies NETwork (PLANET) Collaboration.), AE(Department of Earth and Space Science, Osaka University, Osaka 560-0043, Japan; Microlensing Observations in Astrophysics (MOA) Collaboration.), AF(UPMC-CNRS, UMR 7095, Institut d'Astrophysique de Paris, 98bis Boulevard Arago, F-75014 Paris, France; Probing Lensing Anomalies NETwork (PLANET) Collaboration.), AG(Warsaw University Observatory, Al. Ujazdowskie 4, 00-478 Warszawa, Poland; Optical Gravitational Lensing Experiment (OGLE) Collaboration.), AH(Technische Universität Wien, Wieder Hauptst. 8-10, A-1040 Vienna, Austria), AI(Dipartimento di Fisica, Università di Salerno, Via Ponte Don Melillo 132, I-84084 Fisciano, Italy; Istituto Nazionale di Fisica Nucleare, Sezione di Napoli, Via Cintia, I-80126 Napoli, Italy), AJ(Solar-Terrestrial Environment Laboratory, Nagoya University, Nagoya 464-8601, Japan), AK(Department of Physics, University of Auckland, Private Bag 92-019, Auckland 1001, New Zealand), AL(Department of Physics, University of Auckland, Private Bag 92-019, Auckland 1001, New Zealand), AM(Solar-Terrestrial Environment Laboratory, Nagoya University, Nagoya 464-8601, Japan), AN(Okayama Astrophysical Observatory, National Astronomical Observatory of Japan, Okayama 719-0232, Japan), AO(Solar-Terrestrial Environment Laboratory, Nagoya University, Nagoya 464-8601, Japan), AP(Department of Earth and Space Science, Osaka University, Osaka 560-0043, Japan), AQ(Institute of Natural and Mathematical Sciences, Massey University, Auckland 0745, New Zealand), AR(Solar-Terrestrial Environment Laboratory, Nagoya University, Nagoya 464-8601, Japan), AS(Solar-Terrestrial Environment Laboratory, Nagoya University, Nagoya 464-8601, Japan), AT(Solar-Terrestrial Environment Laboratory, Nagoya University, Nagoya 464-8601, Japan), AU(Department of Earth and Space Science, Osaka University, Osaka 560-0043, Japan), AV(Nagano National College of Technology, Nagano 381-8550, Japan), AW(Department of Physics, University of Auckland, Private Bag 92-019, Auckland 1001, New Zealand), AX(Tokyo Metropolitan College of Aeronautics, Tokyo 116-8523, Japan), AY(School of Chemical and Physical Sciences, Victoria University, Wellington 6140, New Zealand), AZ(Department of Earth and Space Science, Osaka University, Osaka 560-0043, Japan), BA(Institute of Natural and Mathematical Sciences, Massey University, Auckland 0745, New Zealand), BB(Mt. John University Observatory, P.O. Box 56, Lake Tekapo 8770, New Zealand), BC(Solar-Terrestrial Environment Laboratory, Nagoya University, Nagoya 464-8601, Japan), BD(Department of Earth and Space Science, Osaka University, Osaka 560-0043, Japan), BE(Department of Physics, University of Auckland, Private Bag 92-019, Auckland 1001, New Zealand), BF(), BG(Department of Physics and Astronomy, University of Canterbury, Christchurch 8020, New Zealand), BH(IRAP, CNRS, Université de Toulouse, F-31400 Toulouse, France), BI(European Southern Observatory, Casilla 19001, Vitacura 19, Santiago, Chile), BJ(McDonald Observatory, Fort Davis, TX 79734, USA), BK(UPMC-CNRS, UMR 7095, Institut d'Astrophysique de Paris, 98bis Boulevard Arago, F-75014 Paris, France), BL(School of Mathematics and Physics, University of Tasmania, Hobart, TAS 7001, Australia), BM(UPMC-CNRS, UMR 7095, Institut d'Astrophysique de Paris, 98bis Boulevard Arago, F-75014 Paris, France), BN(UPMC-CNRS, UMR 7095, Institut d'Astrophysique de Paris, 98bis Boulevard Arago, F-75014 Paris, France), BO(School of Mathematics and Physics, University of Tasmania, Hobart, TAS 7001, Australia), BP(Department of Physics, University of Rijeka, Omladinska 14, 51000 Rijeka, Croatia), BQ(IRAP, CNRS, Université de Toulouse, F-31400 Toulouse, France), BR(School of Mathematics and Physics, University of Tasmania, Hobart, TAS 7001, Australia), BS(SUPA, University of St Andrews, School of Physics & Astronomy, St Andrews KY16 9SS, UK; RoboNet Collaboration.), BT(Department of Physics, Chungbuk National University, Chongju 371-763, Korea), BU(UPMC-CNRS, UMR 7095, Institut d'Astrophysique de Paris, 98bis Boulevard Arago, F-75014 Paris, France), BV(UPMC-CNRS, UMR 7095, Institut d'Astrophysique de Paris, 98bis Boulevard Arago, F-75014 Paris, France), BW(Perth Observatory, Walnut Road, Bickley, Perth, WA 6076, Australia), BX(South African Astronomical Observatory, P.O. Box 9 Observatory 7925, South Africa), BY(Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA), BZ(Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg (ZAH), D-69120 Heidelberg, Germany), CA(Perth Observatory, Walnut Road, Bickley, Perth, WA 6076, Australia), CB(Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg (ZAH), D-69120 Heidelberg, Germany), CC(), CD(Department of Physics, Chungbuk National University, Chongju 371-763, Korea), CE(Department of Physics, Texas A&M University, College Station, TX 77843-4242, USA), CF(Kavli Institute for Astronomy and Astrophysics, Peking University, Hai Dian District, Beijing 100871, China), CG(Department of Astronomy, Ohio State University, 140 West 18th Avenue, Columbus, OH 43210, USA), CH(Department of Astronomy, Ohio State University, 140 West 18th Avenue, Columbus, OH 43210, USA), CI(Department of Physics, Chungbuk National University, Chongju 371-763, Korea), CJ(Department of Astronomy, Ohio State University, 140 West 18th Avenue, Columbus, OH 43210, USA), CK(Department of Astronomy, Ohio State University, 140 West 18th Avenue, Columbus, OH 43210, USA), CL(Korea Astronomy and Space Science Institute, Yuseong-gu 305-348 Daejeon, Korea), CM(Department of Astronomy, Ohio State University, 140 West 18th Avenue, Columbus, OH 43210, USA), CN(Department of Physics, Chungbuk National University, Chongju 371-763, Korea), CO(Department of Astronomy, Ohio State University, 140 West 18th Avenue, Columbus, OH 43210, USA; Sagan Fellow; Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA.), CP(), CQ(Warsaw University Observatory, Al. Ujazdowskie 4, 00-478 Warszawa, Poland), CR(Warsaw University Observatory, Al. Ujazdowskie 4, 00-478 Warszawa, Poland), CS(Department of Astronomy, Ohio State University, 140 West 18th Avenue, Columbus, OH 43210, USA; Warsaw University Observatory, Al. Ujazdowskie 4, 00-478 Warszawa, Poland), CT(Warsaw University Observatory, Al. Ujazdowskie 4, 00-478 Warszawa, Poland), CU(Warsaw University Observatory, Al. Ujazdowskie 4, 00-478 Warszawa, Poland; Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK), CV(Warsaw University Observatory, Al. Ujazdowskie 4, 00-478 Warszawa, Poland), CW(Warsaw University Observatory, Al. Ujazdowskie 4, 00-478 Warszawa, Poland), CX(Warsaw University Observatory, Al. Ujazdowskie 4, 00-478 Warszawa, Poland; Departamento de Astronomía, Universidad de Concepción, Casilla 160-C, Concepción, Chile), CY(Warsaw University Observatory, Al. Ujazdowskie 4, 00-478 Warszawa, Poland), CZ(Warsaw University Observatory, Al. Ujazdowskie 4, 00-478 Warszawa, Poland), DA(), DB(Las Cumbres Observatory Global Telescope Network, 6740B Cortona Drive, Goleta, CA 93117, USA; School of Physics and Astronomy, Queen Mary University of London, Mile End Road, London E1 4NS, UK), DC(Las Cumbres Observatory Global Telescope Network, 6740B Cortona Drive, Goleta, CA 93117, USA), DD(SUPA, University of St Andrews, School of Physics & Astronomy, St Andrews KY16 9SS, UK; Royal Society University Research Fellow.), DE(ESO Headquarters, Karl-Schwarzschild-Str. 2, D-85748 Garching bei München, Germany; Qatar Environment and Energy Research Institute, Qatar Foundation, Doha, Qatar), DF(SUPA, University of St Andrews, School of Physics & Astronomy, St Andrews KY16 9SS, UK), DG(SUPA, University of St Andrews, School of Physics & Astronomy, St Andrews KY16 9SS, UK), DH(ESO Headquarters, Karl-Schwarzschild-Str. 2, D-85748 Garching bei München, Germany), DI(Max Planck Institute for Solar System Research, D-37191 Katlenburg-Lindau, Germany), DJ(Astrophysics Research Institute, Liverpool John Moores University, Liverpool CH41 1LD, UK), DK(), DL(Pontificia Universidad Catolica de Chile, Casilla 306, Santiago 22, Chile), DM(European Southern Observatory, Casilla 19001, Vitacura 19, Santiago, Chile), DN(Institute of Theoretical Physics, Charles University, 18000 Prague, Czech Republic), DO(Graduate School of Science, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8602, Japan), DP(Jodrell Bank Centre for Astrophysics, University of Manchester, Oxford Road, Manchester M13 9PL, UK), DQ(University of Hertfordshire, Hatfield, Hertfordshire AL10 9AB, UK), DR(Pontificia Universidad Catolica de Chile, Casilla 306, Santiago 22, Chile), DS(Graduate School of Science, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8602, Japan), DT(European Southern Observatory, Casilla 19001, Vitacura 19, Santiago, Chile), DU(Observatoire de Besancon Institut UTINAM, Universite Franche-Comte, CNRS-UMR 6213, BP 1615, F-25010 Besancon Cedex, France), DV(Pontificia Universidad Catolica de Chile, Casilla 306, Santiago 22, Chile)
Publication:
The Astrophysical Journal, Volume 785, Issue 2, article id. 155, 13 pp. (2014). (ApJ Homepage)
Publication Date:
04/2014
Origin:
IOP
Astronomy Keywords:
gravitational lensing: micro, planetary systems
DOI:
10.1088/0004-637X/785/2/155
Bibliographic Code:
2014ApJ...785..155B

Abstract

We present the first microlensing candidate for a free-floating exoplanet-exomoon system, MOA-2011-BLG-262, with a primary lens mass of M host ~ 4 Jupiter masses hosting a sub-Earth mass moon. The argument for an exomoon hinges on the system being relatively close to the Sun. The data constrain the product ML πrel where ML is the lens system mass and πrel is the lens-source relative parallax. If the lens system is nearby (large πrel), then ML is small (a few Jupiter masses) and the companion is a sub-Earth-mass exomoon. The best-fit solution has a large lens-source relative proper motion, μrel = 19.6 ± 1.6 mas yr-1, which would rule out a distant lens system unless the source star has an unusually high proper motion. However, data from the OGLE collaboration nearly rule out a high source proper motion, so the exoplanet+exomoon model is the favored interpretation for the best fit model. However, there is an alternate solution that has a lower proper motion and fits the data almost as well. This solution is compatible with a distant (so stellar) host. A Bayesian analysis does not favor the exoplanet+exomoon interpretation, so Occam's razor favors a lens system in the bulge with host and companion masses of M_host = 0.12^{+0.19}_{ -0.06}\,M_\odot and m_comp = 18^{+28}_{ -10}\,{M_\oplus }, at a projected separation of a_\perp = 0.84^{+0.25}_{ -0.14} AU. The existence of this degeneracy is an unlucky accident, so current microlensing experiments are in principle sensitive to exomoons. In some circumstances, it will be possible to definitively establish the mass of such lens systems through the microlensing parallax effect. Future experiments will be sensitive to less extreme exomoons.
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