PLANETARY AND OTHER SHORT BINARY MICROLENSING EVENTS FROM THE MOA SHORT-EVENT ANALYSIS

被引：56

作者：

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

Sumi, T. ^{[2
]}

Bond, I. A. ^{[3
]}

Kamiya, K. ^{[4
]}

Abe, F. ^{[4
]}

Botzler, C. S. ^{[5
]}

Fukui, A. ^{[4
]}

Furusawa, K. ^{[4
]}

Itow, Y. ^{[4
]}

Korpela, A. V. ^{[6
]}

Kilmartin, P. M. ^{[7
]}

Ling, C. H. ^{[3
]}

Masuda, K. ^{[4
]}

Matsubara, Y. ^{[4
]}

Miyake, N. ^{[4
]}

Muraki, Y. ^{[4
]}

Ohnishi, K. ^{[8
]}

Rattenbury, N. J. ^{[5
]}

Saito, To ^{[9
]}

Sullivan, D. J. ^{[6
]}

Suzuki, D. ^{[2
]}

Sweatman, W. L. ^{[3
]}

Tristram, P. J. ^{[7
]}

Wada, K. ^{[2
]}

Yock, P. C. M. ^{[5
]}

机构：

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

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

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

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

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

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

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

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

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

来源：

ASTROPHYSICAL JOURNAL | 2012年 / 757卷 / 02期

基金：

美国国家科学基金会;

关键词：

gravitational lensing: micro; planets and satellites: detection; GRAVITATIONAL LENSING EXPERIMENT; JOVIAN-MASS PLANET; GALACTIC BULGE; EXTRASOLAR PLANETS; SNOW LINE; GIANT PLANETS; GAS GIANTS; JUPITER/SATURN ANALOG; STELLAR-MASS; LIGHT CURVES;

D O I：

10.1088/0004-637X/757/2/119

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present the analysis of four candidate short-duration binary microlensing events from the 2006-2007 MOA Project short-event analysis. These events were discovered as a by-product of an analysis designed to find short-timescale single-lens events that may be due to free-floating planets. Three of these events are determined to be microlensing events, while the fourth is most likely caused by stellar variability. For each of the three microlensing events, the signal is almost entirely due to a brief caustic feature with little or no lensing attributable mainly to the lens primary. One of these events, MOA-bin-1, is due to a planet, and it is the first example of a planetary event in which the stellar host is only detected through binary microlensing effects. The mass ratio and separation are q = (4.9 +/- 1.4) x 10(-3) and s = 2.10 +/- 0.05, respectively. A Bayesian analysis based on a standard Galactic model indicates that the planet, MOA-bin-1Lb, has a mass of m(p) = 3.7 +/- 2.1M(Jup) and orbits a star of M-* = 0.75(-0.41)(+0.33) M-circle dot at a semimajor axis of a = 8.3(-2.7)(+4.5) AU. This is one of the most massive and widest separation planets found by microlensing. The scarcity of such wide-separation planets also has implications for interpretation of the isolated planetary mass objects found by this analysis. If we assume that we have been able to detect wide-separation planets with an efficiency at least as high as that for isolated planets, then we can set limits on the distribution of planets in wide orbits. In particular, if the entire isolated planet sample found by Sumi et al. consists of planets bound in wide orbits around stars, we find that it is likely that the median orbital semimajor axis is > 30 AU.

引用

页数：17

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