MASSES AND ORBITAL CONSTRAINTS FOR THE OGLE-2006-BLG-109Lb,c JUPITER/SATURN ANALOG PLANETARY SYSTEM

被引：121

作者：

Bennett, D. P. ^{[1
]}

Rhie, S. H. ^{[1
]}

Nikolaev, S. ^{[2
]}

Gaudi, B. S. ^{[3
]}

Udalski, A. ^{[4
]}

Gould, A. ^{[3
]}

Christie, G. W. ^{[5
]}

Maoz, D. ^{[6
]}

Dong, S. ^{[3
]}

McCormick, J. ^{[7
]}

Szymanski, M. K. ^{[4
]}

Tristram, P. J. ^{[8
]}

Macintosh, B. ^{[2
]}

Cook, K. H. ^{[2
]}

Kubiak, M. ^{[4
]}

Pietrzynski, G. ^{[4
,9
]}

Soszynski, I. ^{[4
]}

Szewczyk, O. ^{[9
]}

Ulaczyk, K. ^{[4
]}

Wyrzykowski, L. ^{[4
,10
]}

DePoy, D. L. ^{[11
]}

Han, C. ^{[12
]}

Kaspi, S. ^{[6
]}

Lee, C-U. ^{[13
]}

Mallia, F. ^{[14
]}

Natusch, T. ^{[15
]}

Park, B-G. ^{[13
]}

Pogge, R. W. ^{[3
]}

Polishook, D. ^{[6
]}

Abe, F. ^{[16
]}

Bond, I. A. ^{[17
]}

Botzler, C. S. ^{[18
]}

Fukui, A. ^{[16
]}

Hearnshaw, J. B. ^{[19
]}

Itow, Y. ^{[16
]}

Kamiya, K. ^{[16
]}

Korpela, A. V. ^{[20
]}

Kilmartin, P. M. ^{[8
]}

Lin, W. ^{[17
]}

Ling, J. ^{[17
]}

Masuda, K. ^{[16
]}

Matsubara, Y. ^{[16
]}

Motomura, M. ^{[16
]}

Muraki, Y. ^{[21
]}

Nakamura, S. ^{[16
]}

Okumura, T. ^{[16
]}

Ohnishi, K. ^{[22
]}

Perrott, Y. C. ^{[18
]}

Rattenbury, N. J. ^{[18
]}

Sako, T. ^{[16
]}

机构：

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

[2] Lawrence Livermore Natl Lab, IGPP, Livermore, CA 94550 USA

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

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

[5] Auckland Observ, Auckland, New Zealand

[6] Tel Aviv Univ, Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel

[7] Farm Cove Observ, Auckland 1706, New Zealand

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

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

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

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

[12] Chungbuk Natl Univ, Dept Phys, Chonju 371763, South Korea

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

[14] Campo Catino Astron Observ, I-03016 Frosinone, Italy

[15] AUT Univ, Sch Comp & Math Sci, Auckland, New Zealand

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

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

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

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

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

[21] Konan Univ, Dept Phys, Kobe, Hyogo 6588501+, Japan

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

[23] Tokyo Metropolitan Coll Aeronaut, Tokyo 1168523, Japan

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

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

[26] CNRS, Inst Astrophys Paris, F-75014 Paris, France

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

[28] NASA, Ames Res Ctr, SOFIA Sci Ctr, Moffett Field, CA 94035 USA

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

[30] Univ Toulouse, LATT, CNRS, F-31400 Toulouse, France

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

[32] European So Observ, Santiago 19, Chile

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

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

[35] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA

[36] Univ Massachusetts, Dept Astron, Amherst, MA 01002 USA

来源：

ASTROPHYSICAL JOURNAL | 2010年 / 713卷 / 02期

基金：

美国国家科学基金会;

关键词：

gravitational lensing: micro; planetary systems; GRAVITATIONAL LENSING EXPERIMENT; SURFACE BRIGHTNESS RELATIONS; LIMB-DARKENING COEFFICIENTS; GALACTIC BULGE; SNOW LINE; MICROLENSING EVENTS; LUMINOSITY FUNCTION; SOLAR NEIGHBORHOOD; ANGULAR SIZES; GIANT PLANETS;

D O I：

10.1088/0004-637X/713/2/837

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present a new analysis of the Jupiter+Saturn analog system, OGLE-2006-BLG-109Lb,c, which was the first double planet system discovered with the gravitational microlensing method. This is the only multi-planet system discovered by any method with measured masses for the star and both planets. In addition to the signatures of two planets, this event also exhibits a microlensing parallax signature and finite source effects that provide a direct measure of the masses of the star and planets, and the expected brightness of the host star is confirmed by Keck AO imaging, yielding masses of M-* = 0.51(-0.04)(+0.05) M-circle dot, M-b = 231 +/- 19 M-circle plus, and M-c = 86 +/- 7 M-circle plus. The Saturn-analog planet in this system had a planetary light-curve deviation that lasted for 11 days, and as a result, the effects of the orbital motion are visible in the microlensing light curve. We find that four of the six orbital parameters are tightly constrained and that a fifth parameter, the orbital acceleration, is weakly constrained. No orbital information is available for the Jupiter-analog planet, but its presence helps to constrain the orbital motion of the Saturn-analog planet. Assuming co-planar orbits, we find an orbital eccentricity of epsilon = 0.15(-0.10) (+0.17) and an orbital inclination of i = 64 degrees(+ 4 degrees)(-7 degrees) The 95% confidence level lower limit on the inclination of i > 49 degrees implies that this planetary system can be detected and studied via radial velocity measurements using a telescope of greater than or similar to 30 m aperture.

引用

页码：837 / 855

页数：19

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