MOA 2010-BLG-477Lb: CONSTRAINING THE MASS OF A MICROLENSING PLANET FROM MICROLENSING PARALLAX, ORBITAL MOTION, AND DETECTION OF BLENDED LIGHT

被引：38

作者：

Bachelet, E. ^{[2
]}

Shin, I. -G. ^{[1
]}

Han, C. ^{[1
]}

Fouque, P. ^{[2
]}

Gould, A. ^{[3
]}

Menzies, J. W. ^{[4
]}

Beaulieu, J. -P. ^{[5
]}

Bennett, D. P. ^{[6
]}

Bond, I. A. ^{[7
]}

Dong, Subo ^{[3
,8
]}

Heyrovsky, D. ^{[9
]}

Marquette, J. -B. ^{[5
]}

Marshall, J. ^{[3
]}

Skowron, J. ^{[3
]}

Street, R. A. ^{[10
]}

Sumi, T. ^{[11
,12
]}

Udalski, A. ^{[13
]}

Abe, L. ^{[14
]}

Agabi, K. ^{[14
]}

Albrow, M. D. ^{[15
]}

Allen, W. ^{[16
]}

Bertin, E. ^{[5
]}

Bos, M. ^{[17
]}

Bramich, D. M. ^{[18
]}

Chavez, J. ^{[19
]}

Christie, G. W. ^{[20
]}

Cole, A. A. ^{[21
]}

Crouzet, N. ^{[14
]}

Dieters, S. ^{[21
]}

Dominik, M. ^{[22
]}

Drummond, J. ^{[23
]}

Greenhill, J. ^{[21
]}

Guillot, T. ^{[14
]}

Henderson, C. B. ^{[3
]}

Hessman, F. V. ^{[24
]}

Horne, K. ^{[22
]}

Hundertmark, M. ^{[22
,24
]}

Johnson, J. A. ^{[3
]}

Jorgensen, U. G. ^{[25
,26
]}

Kandori, R. ^{[27
]}

Liebig, C. ^{[22
,28
]}

Mekarnia, D. ^{[14
]}

McCormick, J. ^{[29
]}

Moorhouse, D. ^{[30
]}

Nagayama, T. ^{[31
]}

Nataf, D. ^{[3
]}

Natusch, T. ^{[20
,32
]}

Nishiyama, S. ^{[33
]}

Rivet, J. -P. ^{[14
]}

Sahu, K. C. ^{[34
]}

机构：

[1] Chungbuk Natl Univ, Dept Phys, Chonju 361763, South Korea

[2] Univ Toulouse, CNRS, IRAP, F-31400 Toulouse, France

[3] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA

[4] S African Astron Observ, ZA-7925 Observatory, South Africa

[5] UPMC, CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France

[6] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA

[7] Massey Univ, Inst Informat & Math Sci, Auckland 1330, New Zealand

[8] Inst Adv Study, Princeton, NJ 08540 USA

[9] Charles Univ Prague, Inst Theoret Phys, CR-18000 Prague, Czech Republic

[10] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA

[11] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan

[12] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan

[13] Univ Warsaw Observ, PL-00478 Warsaw, Poland

[14] Observ Cote Azur, Lab Fizeau, F-06300 Nice, France

[15] Univ Canterbury, Dept Phys & Astron, Christchurch 8020, New Zealand

[16] Vintage Lane Observ, Blenheim, New Zealand

[17] Molehill Astron Observ, N Shore, New Zealand

[18] European So Observ, D-85748 Garching, Germany

[19] McDonald Observ, Ft Davis, TX 79734 USA

[20] Auckland Observ, Auckland, New Zealand

[21] Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001, Australia

[22] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland

[23] Possum Observ, John Drummond, New Zealand

[24] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany

[25] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen O, Denmark

[26] Univ Copenhagen, Ctr Star & Planet Format, DK-1350 Copenhagen O, Denmark

[27] Natl Astron Observ, Mitaka, Tokyo 1818588, Japan

[28] Heidelberg Univ, Zentrum Astron, Astron Rech Inst, D-69120 Heidelberg, Germany

[29] Ctr Backyard Astrophys, Farm Cove Observ, Auckland, New Zealand

[30] Kumeu Observ, Kumeu, New Zealand

[31] Nagoya Univ, Grad Sch Sci, Chikusa Ku, Nagoya, Aichi 4648602, Japan

[32] AUT Univ, Inst Radiophys & Space Res, Auckland, New Zealand

[33] Natl Inst Nat Sci, Natl Astron Observ Japan, Extrasolar Planet Detect Project Off, Mitaka, Tokyo 1818588, Japan

[34] Space Telescope Sci Inst, Baltimore, MD 21218 USA

[35] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel

[36] Tel Aviv Univ, Wise Observ, IL-69978 Tel Aviv, Israel

[37] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA

[38] Queen Mary Univ London, Sch Phys & Astron, London E1 4NS, England

[39] MIT, Dept Phys, Cambridge, MA 02139 USA

[40] European So Observ, Santiago 19, Chile

[41] Univ Rijeka, Dept Phys, Rijeka 51000, Croatia

[42] Vienna Univ Technol, A-1040 Vienna, Austria

[43] Perth Observ, Perth, WA 6076, Australia

[44] Inst Nacl Pesquisas Espaciais, Div Astrofis, BR-12227010 Sao Jose Dos Campos, SP, Brazil

[45] Korea Astron & Space Sci Inst, Taejon 305348, South Korea

[46] Chungnam Natl Univ, Dept Astron & Space Sci, Taejon, South Korea

[47] Univ Valencia, Dept Astron & Astrofis, E-46100 Valencia, Spain

[48] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA

[49] Univ Auckland, Dept Phys, Auckland 1001, New Zealand

[50] Victoria Univ, Sch Chem & Phys Sci, Wellington, New Zealand

来源：

ASTROPHYSICAL JOURNAL | 2012年 / 754卷 / 01期

基金：

新加坡国家研究基金会; 美国国家科学基金会; 欧洲研究理事会;

关键词：

gravitational lensing: micro; planetary systems; DIFFERENCE IMAGE-ANALYSIS; HIGH-MAGNIFICATION; GALACTIC BULGE; SNOW LINE; JUPITER/SATURN ANALOG; PROTOPLANETARY DISK; MILKY-WAY; EVENTS; BINARY; STARS;

D O I：

10.1088/0004-637X/754/1/73

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Microlensing detections of cool planets are important for the construction of an unbiased sample to estimate the frequency of planets beyond the snow line, which is where giant planets are thought to form according to the core accretion theory of planet formation. In this paper, we report the discovery of a giant planet detected from the analysis of the light curve of a high-magnification microlensing event MOA 2010-BLG-477. The measured planet-star mass ratio is q = (2.181 +/- 0.004) x 10(-3) and the projected separation is s = 1.1228 +/- 0.0006 in units of the Einstein radius. The angular Einstein radius is unusually large theta(E) = 1.38 +/- 0.11 mas. Combining this measurement with constraints on the "microlens parallax" and the lens flux, we can only limit the host mass to the range 0.13 < M/M-circle dot < 1.0. In this particular case, the strong degeneracy between microlensing parallax and planet orbital motion prevents us from measuring more accurate host and planet masses. However, we find that adding Bayesian priors from two effects (Galactic model and Keplerian orbit) each independently favors the upper end of this mass range, yielding star and planet masses of M-* = 0.67(-0.13)(+0.33) M-circle dot and m(p) = 1.5(-0.3)(+0.8) M-JUP at a distance of D = 2.3 +/- 0.6 kpc, and with a semi-major axis of a = 2(-1)(+3) AU. Finally, we show that the lens mass can be determined from future high-resolution near-IR adaptive optics observations independently from two effects, photometric and astrometric.

引用

页数：17

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