MOA-2010-BLG-073L: AN M-DWARF WITH A SUBSTELLAR COMPANION AT THE PLANET/BROWN DWARF BOUNDARY

被引：30

作者：

Street, R. A. ^{[1
]}

Choi, J. -Y. ^{[2
]}

Tsapras, Y. ^{[1
,3
]}

Han, C. ^{[2
]}

Furusawa, K. ^{[4
]}

Hundertmark, M. ^{[5
]}

Gould, A. ^{[6
]}

Sumi, T. ^{[7
]}

Bond, I. A. ^{[8
]}

Wouters, D. ^{[9
]}

Zellem, R. ^{[10
]}

Udalski, A. ^{[11
]}

Snodgrass, C. ^{[12
]}

Horne, K. ^{[5
]}

Dominik, M. ^{[5
]}

Browne, P. ^{[5
]}

Kains, N. ^{[13
]}

Bramich, D. M. ^{[13
]}

Bajek, D. ^{[5
]}

Steele, I. A. ^{[14
]}

Ipatov, S. ^{[15
]}

Abe, F. ^{[4
]}

Bennett, D. P. ^{[16
]}

Botzler, C. S. ^{[17
]}

Chote, P. ^{[18
]}

Freeman, M. ^{[17
]}

Fukui, A. ^{[4
]}

Harris, P. ^{[18
]}

Itow, Y. ^{[4
]}

Ling, C. H. ^{[8
]}

Masuda, K. ^{[4
]}

Matsubara, Y. ^{[4
]}

Miyake, N. ^{[4
]}

Muraki, Y. ^{[19
]}

Nagayama, T. ^{[20
]}

Nishimaya, S. ^{[21
]}

Ohnishi, K. ^{[22
]}

Rattenbury, N. ^{[17
]}

Saito, To. ^{[23
]}

Sullivan, D. J. ^{[18
]}

Suzuki, D. ^{[7
]}

Sweatman, W. L. ^{[8
]}

Tristram, P. J. ^{[24
]}

Wada, K. ^{[7
]}

Yock, P. C. M. ^{[17
]}

Szymanski, M. K. ^{[11
]}

Kubiak, M. ^{[11
]}

Pietrzynski, G. ^{[11
,25
]}

Soszynski, I. ^{[11
]}

Poleski, R. ^{[11
]}

机构：

[1] LCOGT, Goleta, CA 93117 USA

[2] Chungbuk Natl Univ, Inst Astrophys, Dept Phys, Cheongju 361763, South Korea

[3] Univ London, Sch Math Sci, London E1 4NS, England

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

[5] Univ St Andrews, Dept Phys & Astron, SUPA St Andrews, St Andrews KY16 9SS, Fife, Scotland

[6] Ohio State Univ, Dept Astron, McPherson Lab, Columbus, OH 43210 USA

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

[8] Massey Univ, Inst Informat & Math Sci, N Shore Mail Ctr, Auckland, New Zealand

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

[10] Univ Arizona, Dept Planetary Sci, Lunar & Planetary Lab, Tucson, AZ 85721 USA

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

[12] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany

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

[14] Liverpool John Moores Univ, Astrophys Res Inst, Wirral CH41 1LD, Merseyside, England

[15] Qatar Fdn, Doha, Qatar

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

[17] Univ Auckland, Dept Phys, Auckland, New Zealand

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

[19] Konan Univ, Dept Phys, Kobe, Hyogo 6588501, Japan

[20] Nagoya Univ, Fac Sci, Dept Phys & Astrophys, Nagoya, Aichi 4648602, Japan

[21] Natl Astron Observ Japan, Extrasolar Planet Detect Project Off, Mitaka, Tokyo 1818588, Japan

[22] Nagano Natl Coll Technol, Nagano 3818550, Japan

[23] Tokyo Metropolitan Coll Ind Technol, Tokyo 1168523, Japan

[24] Mt John Observ, Lake Tekapo 8770, New Zealand

[25] Univ Concepcion, Dept Astron, Concepcion, Chile

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

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

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

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

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

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

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

[33] Farm Cove Observ, Auckland 2010, New Zealand

[34] Auckland Observ, Auckland, New Zealand

[35] Vintage Lane Observ, Blenheim, New Zealand

[36] Possum Observ, Patutahi, New Zealand

[37] Kumeu Observ, Kumeu, W Auckland, New Zealand

[38] Molehill Astron Observ, N Shore City, New Zealand

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

[40] European So Observ, Santiago 19, Chile

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

[42] Univ Paris 06, CNRS, UMR7095, Inst Astrophys Paris, F-75014 Paris, France

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

[44] Univ Rijeka, Fac Arts & Sci, Dept Phys, Rijeka 51000, Croatia

[45] Vienna Univ Technol, Dept Comp, A-1060 Vienna, Austria

[46] Univ Toulouse, UPS OMP, IRAP, Inst Rech Astrophys & Planetol, F-31028 Toulouse 04, France

[47] IRAP, CNRS, F-31400 Toulouse, France

[48] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA

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

[50] S African Astron Observ, ZA-7935 Observatory, South Africa

来源：

ASTROPHYSICAL JOURNAL | 2013年 / 763卷 / 01期

基金：

美国国家科学基金会; 新加坡国家研究基金会; 欧洲研究理事会; 美国国家航空航天局;

关键词：

brown dwarfs; gravitational lensing: micro; planetary systems; planets and satellites: formation; planets and satellites: general; techniques: photometric; GRAVITATIONAL LENSING EXPERIMENT; GAS GIANT PLANETS; BROWN DWARFS; MICROLENSING BINARIES; VARIABLE-STARS; GALACTIC BULGE; MINIMUM MASS; VARIABILITY; PHOTOMETRY; DISCOVERY;

D O I：

10.1088/0004-637X/763/1/67

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present an analysis of the anomalous microlensing event, MOA-2010-BLG-073, announced by the Microlensing Observations in Astrophysics survey on 2010 March 18. This event was remarkable because the source was previously known to be photometrically variable. Analyzing the pre-event source light curve, we demonstrate that it is an irregular variable over timescales >200 days. Its dereddened color, (V - I)(S),(0), is 1.221 +/- 0.051 mag, and from our lens model we derive a source radius of 14.7 +/- 1.3 R-circle dot, suggesting that it is a red giant star. We initially explored a number of purely microlensing models for the event but found a residual gradient in the data taken prior to and after the event. This is likely to be due to the variability of the source rather than part of the lensing event, so we incorporated a slope parameter in our model in order to derive the true parameters of the lensing system. We find that the lensing system has a mass ratio of q = 0.0654 +/- 0.0006. The Einstein crossing time of the event, t(E) = 44.3 +/- 0.1 days, was sufficiently long that the light curve exhibited parallax effects. In addition, the source trajectory relative to the large caustic structure allowed the orbital motion of the lens system to be detected. Combining the parallax with the Einstein radius, we were able to derive the distance to the lens, D-L = 2.8 +/- 0.4 kpc, and the masses of the lensing objects. The primary of the lens is an M-dwarf with M-L,M-1 = 0.16 +/- 0.03 M-circle dot, while the companion has M-L,M-2 = 11.0 +/- 2.0 M-J, putting it in the boundary zone between planets and brown dwarfs.

引用

页数：13

共 25 条

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