MOA 2010-BLG-477Lb: CONSTRAINING THE MASS OF A MICROLENSING PLANET FROM MICROLENSING PARALLAX, ORBITAL MOTION, AND DETECTION OF BLENDED LIGHT
MOA 2010-BLG-477Lb: CONSTRAINING THE MASS OF A MICROLENSING PLANET FROM MICROLENSING PARALLAX, ORBITAL MOTION, AND DETECTION OF BLENDED LIGHT
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DOI：
10.1088/0004-637x/754/1/73
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发表时间：
2012-05
期刊：
影响因子：
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通讯作者：
E. Bachelet;I. Shin;C. Han;P. Fouqu'e;A. Gould;J. Menzies;J. Beaulieu;D. Bennett;I. Bond;S. Dong;D. Heyrovsk'y;J. Marquette;J. Marshall;J. Skowron;R. Street;T. Sumi;A. Udalski;L. Abe;K. Agabi;M. Albrow;W. Allen;E. Bertin;M. Bos;D. Bramich;J. Chavez;G. Christie;A. Cole;N. Crouzet;S. Dieters;M. Dominik;J. Drummond;J. Greenhill;T. Guillot;C. Henderson;F. Hessman;K. Horne;M. Hundertmark;J. Johnson;U. Jørgensen;R. Kandori;C. Liebig;D. M'ekarnia;J. Mccormick;D. Moorhouse;T. Nagayama;D. Nataf;T. Natusch;S. Nishiyama;J. Rivet;K. Sahu;Y. Shvartzvald;G. Thornley;A. Tomczak;Y. Tsapras;J. Yee;V. Batista;C. S. Bennett;S. Brillant;J. Caldwell;A. Cassan;E. Corrales;C. Coutures;D. Prester;J. Donatowicz;D. Kubas;R. Martin;A. Williams;M. Zub;L. Almeida;D. Depoy;B. Gaudi;L. Hung;F. Jablonski;S. Kaspi;N. Klein;C.‐U. Lee;Y. Lee;J. Koo;D. Maoz;J. A. Muñoz;R. Pogge;D. Polishook;Avi Shporer;F. Abe;C. Botzler;P. Chote;M. Freeman;A. Fukui;K. Furusawa;P. Harris;Y. Itow;S. Kobara;C. Ling;K. Masuda;Y. Matsubara;N. Miyake;K. Ohmori;K. Ohnishi;N. Rattenbury;T. Saito;D. Sullivan;D. Suzuki;W. Sweatman;P. Tristram;K. Wada;P. Yock;M. Szyma'nski;I. Soszy'nski;M. Kubiak;R. Poleski;K. Ulaczyk;G. Pietrzy'nski;L. Wyrzykowski;N. Kains;C. Snodgrass;I. Steele;K. Alsubai;V. Bozza;P. Browne;M. Burgdorf;S. Novati;P. Dodds;S. Dreizler;F. Finet;T. Gerner;S. Hardis;K. Harpsoe;T. Hinse;E. Kerins;L. Mancini;M. Mathiasen;M. Penny;S. Proft;S. Rahvar;D. Ricci;G. Scarpetta;S. Schafer;F. Schonebeck;J. Southworth;J. Surdej;J. Wambsganss
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作者：
E. Bachelet;I. Shin;C. Han;P. Fouqu'e;A. Gould;J. Menzies;J. Beaulieu;D. Bennett;I. Bond;S. Dong;D. Heyrovsk'y;J. Marquette;J. Marshall;J. Skowron;R. Street;T. Sumi;A. Udalski;L. Abe;K. Agabi;M. Albrow;W. Allen;E. Bertin;M. Bos;D. Bramich;J. Chavez;G. Christie;A. Cole;N. Crouzet;S. Dieters;M. Dominik;J. Drummond;J. Greenhill;T. Guillot;C. Henderson;F. Hessman;K. Horne;M. Hundertmark;J. Johnson;U. Jørgensen;R. Kandori;C. Liebig;D. M'ekarnia;J. Mccormick;D. Moorhouse;T. Nagayama;D. Nataf;T. Natusch;S. Nishiyama;J. Rivet;K. Sahu;Y. Shvartzvald;G. Thornley;A. Tomczak;Y. Tsapras;J. Yee;V. Batista;C. S. Bennett;S. Brillant;J. Caldwell;A. Cassan;E. Corrales;C. Coutures;D. Prester;J. Donatowicz;D. Kubas;R. Martin;A. Williams;M. Zub;L. Almeida;D. Depoy;B. Gaudi;L. Hung;F. Jablonski;S. Kaspi;N. Klein;C.‐U. Lee;Y. Lee;J. Koo;D. Maoz;J. A. Muñoz;R. Pogge;D. Polishook;Avi Shporer;F. Abe;C. Botzler;P. Chote;M. Freeman;A. Fukui;K. Furusawa;P. Harris;Y. Itow;S. Kobara;C. Ling;K. Masuda;Y. Matsubara;N. Miyake;K. Ohmori;K. Ohnishi;N. Rattenbury;T. Saito;D. Sullivan;D. Suzuki;W. Sweatman;P. Tristram;K. Wada;P. Yock;M. Szyma'nski;I. Soszy'nski;M. Kubiak;R. Poleski;K. Ulaczyk;G. Pietrzy'nski;L. Wyrzykowski;N. Kains;C. Snodgrass;I. Steele;K. Alsubai;V. Bozza;P. Browne;M. Burgdorf;S. Novati;P. Dodds;S. Dreizler;F. Finet;T. Gerner;S. Hardis;K. Harpsoe;T. Hinse;E. Kerins;L. Mancini;M. Mathiasen;M. Penny;S. Proft;S. Rahvar;D. Ricci;G. Scarpetta;S. Schafer;F. Schonebeck;J. Southworth;J. Surdej;J. Wambsganss
对冷行星的微透镜探测对于构建无偏样本以估计雪线以外行星的频率非常重要，根据行星形成的核心吸积理论，雪线以外的行星被认为是形成巨行星的地方。本文报道了通过对高倍微透镜事件MOA 2010-BLG-477的光曲线的分析，发现了一颗巨行星。测得的行星-恒星质量比Q=(2.181±0.004)×10−3，投影分离为S=1.1228±0.0006，单位为爱因斯坦半径。角爱因斯坦半径非常大，θE=1.38±0.11ma。结合这一测量以及对微透镜视差和透镜通量的限制，我们只能将主机质量限制在0.13M/M☉<；1.0的范围内。在这种特殊情况下，微透镜视差和行星轨道运动之间的强烈简并性使我们无法更准确地测量宿主和行星的质量。然而，我们发现，添加来自两种效应(银河系模型和开普勒式轨道)的贝叶斯先验分别独立地有利于这个质量范围的上端，得到恒星和行星的质量M*=0.67+0.33−0.13M☉和MP=1.5+0.8KPC=0.3MJUP，距离D=2.3±0.6KPC，半长轴a=2+3−1AU。最后，我们证明了透镜质量可以从未来的高分辨率近红外自适应光学观测中确定，而不受光度学和天体测量学两个效应的影响。
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) × 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 θE = 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☉ < 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+0.33− 0.13 M☉ and mp = 1.5+0.8− 0.3 MJUP at a distance of D = 2.3 ± 0.6 kpc, and with a semi-major axis of a = 2+3− 1 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.