A POSSIBLE BINARY SYSTEM OF A STELLAR REMNANT IN THE HIGH-MAGNIFICATION GRAVITATIONAL MICROLENSING EVENT OGLE-2007-BLG-514

被引：16

作者：

Miyake, N. ^{[1
]}

Udalski, A. ^{[2
]}

Sumi, T. ^{[3
]}

Bennett, D. P. ^{[4
]}

Dong, S. ^{[5
]}

Street, R. A. ^{[6
]}

Greenhill, J. ^{[7
]}

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

Gould, A. ^{[5
]}

Kubiak, M. ^{[2
]}

Szymanski, M. K. ^{[2
]}

Pietrzynski, G. ^{[2
,9
]}

Soszynski, I. ^{[2
]}

Ulaczyk, K. ^{[2
]}

Wyrzykowski, L. ^{[2
,10
]}

Abe, F. ^{[1
]}

Fukui, A. ^{[11
]}

Furusawa, K. ^{[1
]}

Holderness, S. ^{[12
]}

Itow, Y. ^{[1
]}

Korpela, A. ^{[13
]}

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

Masuda, K. ^{[1
]}

Matsubara, Y. ^{[1
]}

Muraki, Y. ^{[1
]}

Nagayama, T. ^{[14
]}

Ohnishi, K. ^{[15
]}

Rattenbury, N. ^{[16
]}

Saito, To ^{[17
]}

Sako, T. ^{[1
]}

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

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

Tristram, P. J. ^{[13
]}

Yock, P. C. M. ^{[16
]}

Allen, W. ^{[19
]}

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

DePoy, D. L. ^{[5
]}

Gaudi, B. S. ^{[5
]}

Han, C. ^{[21
]}

Lee, C. -U. ^{[22
]}

McCormick, J. ^{[23
]}

Monard, B. ^{[19
]}

Natusch, T. ^{[24
]}

Park, B. -G. ^{[22
]}

Pogge, R. W. ^{[5
]}

Allan, A. ^{[25
]}

Bode, M. ^{[26
]}

Bramich, D. M. ^{[27
]}

Clay, N. ^{[26
]}

Dominik, M. ^{[28
]}

机构：

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

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

[3] Osaka Univ, Dept Earth & Space Sci, Osaka 5600043, Japan

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

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

[6] Las Cumbres Observ, Goleta, CA 93117 USA

[7] Univ Tasmania, Sch Maths & Phys, Gpo Hobart, Tas 7001, Australia

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

[9] Univ Concepcion, Dept Fis, Concepcion, Chile

[10] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England

[11] Natl Inst Nat Sci, Natl Astron Observ Japan, Okayama Astrophys Observ, Kamogatacho, Okayama 7190232, Japan

[12] Univ Auckland, Dept Comp Sci, Auckland 1, New Zealand

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

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

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

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

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

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

[19] Ctr Backyard Astrophys Pretoria, Bronberg Observ, Pretoria, South Africa

[20] Auckland Observ, Auckland, New Zealand

[21] Chungbuk Natl Univ, Dept Phys, Program Brain Korea, Chonju 371763, South Korea

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

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

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

[25] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England

[26] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England

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

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

[29] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany

[30] European So Observ, Santiago 19, Chile

[31] Queen Mary Univ London, Sch Math Sci, London E1 4NS, England

[32] Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand

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

[34] SOFIA Sci Ctr, Moffett Field, CA 94035 USA

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

[36] Lawrence Livermore Natl Lab, IGPP, Livermore, CA 94551 USA

[37] CEA Saclay, DSM, DAPNIA, F-91191 Gif Sur Yvette, France

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

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

[40] Observ Midi Pyrenees, UMR 5572, F-31400 Toulouse, France

[41] Astron Observ, Niels Bohr Inst, DK-2100 Copenhagen, Denmark

[42] NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA

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

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

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

[46] Univ Heidelberg, Zentrum Astron, Astron Rechen Inst, D-69120 Heidelberg, Germany

来源：

ASTROPHYSICAL JOURNAL | 2012年 / 752卷 / 02期

基金：

欧洲研究理事会; 美国国家科学基金会;

关键词：

binaries: general; Galaxy: bulge; gravitational lensing: micro; GALACTIC BULGE; CHEMICAL EVOLUTION; LENSING EXPERIMENT; MASS-DISTRIBUTION; BLACK-HOLES; DWARF; PHOTOMETRY; PLANET; STARS; ATMOSPHERE;

D O I：

10.1088/0004-637X/752/2/82

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We report the extremely high-magnification (A > 1000) binary microlensing event OGLE-2007-BLG-514. We obtained good coverage around the double peak structure in the light curve via follow-up observations from different observatories. The binary lens model that includes the effects of parallax (known orbital motion of the Earth) and orbital motion of the lens yields a binary lens mass ratio of q = 0.321 +/- 0.007 and a projected separation of s = 0.072 +/- 0.001 in units of the Einstein radius. The parallax parameters allow us to determine the lens distance D-L = 3.11 +/- 0.39 kpc and total mass M-L = 1.40 +/- 0.18 M-circle dot; this leads to the primary and secondary components having masses of M-1 = 1.06 +/- 0.13 M-circle dot and M-2 = 0.34 +/- 0.04 M-circle dot, respectively. The parallax model indicates that the binary lens system is likely constructed by the main-sequence stars. On the other hand, we used a Bayesian analysis to estimate probability distributions by the model that includes the effects of xallarap (possible orbital motion of the source around a companion) and parallax (q = 0.270 +/- 0.005, s = 0.083 +/- 0.001). The primary component of the binary lens is relatively massive, with M-1 = 0.9(-0.3)(+4.6) M-circle dot and it is at a distance of D-L = 2.6(-0.9)(+3.8) kpc. Given the secure mass ratio measurement, the companion mass is therefore M-2 = 0.2(-0.1)(+1.2) M-circle dot. The xallarap model implies that the primary lens is likely a stellar remnant, such as a white dwarf, a neutron star, or a black hole.

引用

页数：12

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