MOA-2010-BLG-328Lb: A SUB-NEPTUNE ORBITING VERY LATE M DWARF?
MOA-2010-BLG-328Lb: A SUB-NEPTUNE ORBITING VERY LATE M DWARF?
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DOI：
10.1088/0004-637x/779/2/91
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发表时间：
2013-09
期刊：
影响因子：
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通讯作者：
K. Furusawa;A. Udalski;T. Sumi;D. Bennett;I. Bond;A. Gould;U. Jørgensen;C. Snodgrass;D. Prester;M. Albrow;F. Abe;C. Botzler;P. Chote;M. Freeman;A. Fukui;P. Harris;Y. Itow;C. Ling;K. Masuda;Y. Matsubara;N. Miyake;Y. Muraki;K. Ohnishi;N. Rattenbury;T. Saito;D. Sullivan;D. Suzuki;W. Sweatman;P. Tristram;K. Wada;P. Yock;M. Szymański;I. Soszyński;M. Kubiak;R. Poleski;K. Ulaczyk;G. Pietrzyński;Ł. Wyrzykowski;J.-Y. Choi;G. Christie;D. Depoy;S. Dong;J. Drummond;B. Gaudi;C. Han;L. Hung;K. Hwang;C.‐U. Lee;J. Mccormick;D. Moorhouse;T. Natusch;M. Nola;E. Ofek;R. Pogge;I. Shin;J. Skowron;G. Thornley;J. Yee;K. Alsubai;V. Bozza;P. Browne;M. Burgdorf;S. Novati;P. Dodds;M. Dominik;F. Finet;T. Gerner;S. Hardis;K. Harpsoe;T. Hinse;M. Hundertmark;N. Kains;E. Kerins;C. Liebig;L. Mancini;M. Mathiasen;M. Penny;S. Proft;S. Rahvar;D. Ricci;G. Scarpetta;S. Schäfer;F. Schönebeck;J. Southworth;J. Surdej;J. Wambsganss;R. Street;D. Bramich;I. Steele;Y. Tsapras;K. Horne;J. Donatowicz;K. Sahu;E. Bachelet;V. Batista;T. Beatty;J. Beaulieu;C. S. Bennett;C. Black;R. Bowens-Rubin;S. Brillant;J. Caldwell;A. Cassan;A. Cole;E. Corrales;C. Coutures;S. Dieters;P. Fouqué;J. Greenhill;C. Henderson;D. Kubas;J. Marquette;R. Martin;J. Menzies;B. Shappee;A. Williams;D. Wouters;J. V. van Saders;R. Zellem;M. Zub
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文献类型：
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作者：
K. Furusawa;A. Udalski;T. Sumi;D. Bennett;I. Bond;A. Gould;U. Jørgensen;C. Snodgrass;D. Prester;M. Albrow;F. Abe;C. Botzler;P. Chote;M. Freeman;A. Fukui;P. Harris;Y. Itow;C. Ling;K. Masuda;Y. Matsubara;N. Miyake;Y. Muraki;K. Ohnishi;N. Rattenbury;T. Saito;D. Sullivan;D. Suzuki;W. Sweatman;P. Tristram;K. Wada;P. Yock;M. Szymański;I. Soszyński;M. Kubiak;R. Poleski;K. Ulaczyk;G. Pietrzyński;Ł. Wyrzykowski;J.-Y. Choi;G. Christie;D. Depoy;S. Dong;J. Drummond;B. Gaudi;C. Han;L. Hung;K. Hwang;C.‐U. Lee;J. Mccormick;D. Moorhouse;T. Natusch;M. Nola;E. Ofek;R. Pogge;I. Shin;J. Skowron;G. Thornley;J. Yee;K. Alsubai;V. Bozza;P. Browne;M. Burgdorf;S. Novati;P. Dodds;M. Dominik;F. Finet;T. Gerner;S. Hardis;K. Harpsoe;T. Hinse;M. Hundertmark;N. Kains;E. Kerins;C. Liebig;L. Mancini;M. Mathiasen;M. Penny;S. Proft;S. Rahvar;D. Ricci;G. Scarpetta;S. Schäfer;F. Schönebeck;J. Southworth;J. Surdej;J. Wambsganss;R. Street;D. Bramich;I. Steele;Y. Tsapras;K. Horne;J. Donatowicz;K. Sahu;E. Bachelet;V. Batista;T. Beatty;J. Beaulieu;C. S. Bennett;C. Black;R. Bowens-Rubin;S. Brillant;J. Caldwell;A. Cassan;A. Cole;E. Corrales;C. Coutures;S. Dieters;P. Fouqué;J. Greenhill;C. Henderson;D. Kubas;J. Marquette;R. Martin;J. Menzies;B. Shappee;A. Williams;D. Wouters;J. V. van Saders;R. Zellem;M. Zub
我们分析了行星微透镜事件MOA-2010-BLG-328。最佳拟合得到宿主质量为Mh=0.11±0.01M☉，行星质量为Mp=9.2±2.2M⊕，分别对应于一颗M型矮行星和亚海王星质量行星。Dl=0.81±0.10kpc，投影分离r⊥=0.92±0.16AU。由于宿主事先不太可能的近距离，以及系统的不同寻常的性质，我们考虑了这样一种可能性，即决定宿主质量和距离的微透镜视差信号实际上是由于被误解为视差的xallarap(源轨道运动)。我们给出了一个支持视差解决方案的结果，即使考虑到它与主机的距离很近。我们表明，未来的高分辨率天体测量可以决定性地解决这些解决方案的剩余模糊性。
We analyze the planetary microlensing event MOA-2010-BLG-328. The best fit yields host and planetary masses of Mh = 0.11 ± 0.01 M☉ and Mp = 9.2 ± 2.2 M⊕, corresponding to a very late M dwarf and sub-Neptune-mass planet, respectively. The system lies at DL = 0.81 ± 0.10 kpc with projected separation r⊥ = 0.92 ± 0.16 AU. Because of the host's a priori unlikely close distance, as well as the unusual nature of the system, we consider the possibility that the microlens parallax signal, which determines the host mass and distance, is actually due to xallarap (source orbital motion) that is being misinterpreted as parallax. We show a result that favors the parallax solution, even given its close host distance. We show that future high-resolution astrometric measurements could decisively resolve the remaining ambiguity of these solutions.