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arXiv 1111.4032astro-ph.SR
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透镜通过源星的高倍率单透镜引力微透镜事例的透镜和透镜星的特征

Characterizing Lenses and Lensed Stars of High-Magnification Single-lens Gravitational Microlensing Events With Lenses Passing Over Source Stars

J. -Y. Choi, I. -G. Shin, S. -Y. Park, C. Han, A. Gould, T. Sumi, A. Udalski, J. -P. Beaulieu, R. Street, M. Dominik, W. Allen, L. A. Almeida, M. Bos, G. W. Chr… 展开作者

J. -Y. Choi, I. -G. Shin, S. -Y. Park, C. Han, A. Gould, T. Sumi, A. Udalski, J. -P. Beaulieu, R. Street, M. Dominik, W. Allen, L. A. Almeida, M. Bos, G. W. Christie, D. L. Depoy, S. Dong, J. Drummond, A. Gal-Yam, B. S. Gaudi, C. B. Henderson, L. -W. Hung, F. Jablonski, J. Janczak, C. -U. Lee, F. Mallia, A. Maury, J. McCormick, D. McGregor, L. A. G. Monard, D. Moorhouse, J. A. Muñoz, T. Natusch, C. Nelson, B. -G. Park, R. W. Pogge, T. -G. "TG" Tan, G. Thornley, J. C. Yee, F. Abe, E. Barnard, J. Baudry, D. P. Bennett, I. A. Bond, C. S. Botzler, M. Freeman, A. Fukui, K. Furusawa, F. Hayashi, J. B. Hearnshaw, S. Hosaka, Y. Itow, K. Kamiya, P. M. Kilmartin, S. Kobara, A. Korpela, W. Lin, C. H. Ling, S. Makita, K. Masuda, Y. Matsubara, N. Miyake, Y. Muraki, M. Nagaya, K. Nishimoto, K. Ohnishi, T. Okumura, K. Omori, Y. C. Perrott, N. Rattenbury, To. Saito, L. Skuljan, D. J. Sullivan, D. Suzuki, K. Suzuki, W. L. Sweatman, S. Takino, P. J. Tristram, K. Wada, P. C. M. Yock, M. K. Szymański, M. Kubiak, G. Pietrzyński, I. Soszyński, R. Poleski, K. Ulaczyk, Ł. Wyrzykowski, S. Kozłowski, P. Pietrukowicz, M. D. Albrow, E. Bachelet, V. Batista, C. S. Bennett, R. Bowens-Rubin, S. Brillant, A. Cassan, A. Cole, E. Corrales, Ch. Coutures, S. Dieters, D. Dominis Prester, J. Donatowicz, P. Fouqué, J. Greenhill, S. R. Kane, J. Menzies, K. C. Sahu, J. Wambsganss, A. Williams, M. Zub, A. Allan, D. M. Bramich, P. Browne, N. Clay, S. Fraser, K. Horne, N. Kains, C. Mottram, C. Snodgrass, I. Steele, Y. Tsapras, K. A. Alsubai, V. Bozza, M. J. Burgdorf, S. Calchi Novati, P. Dodds, S. Dreizler, F. Finet, T. Gerner, M. Glitrup, F. Grundahl, S. Hardis, K. Harpsøe, T. C. Hinse, M. Hundertmark, U. G. Jørgensen, E. Kerins, C. Liebig, G. Maier, L. Mancini, M. Mathiasen, M. T. Penny, S. Proft, S. Rahvar, D. Ricci, G. Scarpetta, S. Schäfer, F. Schönebeck, J. Skottfelt, J. Surdej, J. Southworth, F. Zimmer

备注：
14 pages, 12 figures, 5 tables
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摘要：

分析了OGLE-2004-BLG-254、MOA-2007-BLG-176、MOA-2007-BLG-233/OGLE-2007-BLG-302、MOA-2009-BLG-174、MOA-2010-BLG-436、MOA-2011-BLG-093、MOA-2011-BLG-274、OGLE-2011-BLG-0990/MOA-2011-BLG-300和OGLE-2011-BLG-1101/MOA-2011-BLG-325。对于所有的事件，我们测量的线性边缘暗化系数的源星的表面亮度轮廓通过测量的光变曲线附近的有限源效应的影响的峰值的偏差。对7个事件，我们测量了爱因斯坦半径和透镜-源的相对自行。其中，5个事件的爱因斯坦半径小于0.2质量，使透镜的候选人非常低质量的恒星或褐矮星。特别是对于MOA-2011-BLG-274，小的爱因斯坦半径$θ_{\rm E}\sim 0.08$ mas与短的时间尺度$t_{\rm E}\sim 2.7$天相结合，表明透镜可能是一个自由漂浮的行星。对于MOA-2009-BLG-174，我们测量镜头视差，从而唯一确定镜头的物理参数。我们还发现，测量的透镜质量的$\sim 0.84\ M_\odot$是一致的恒星混合源，这表明混合很可能是透镜。虽然我们发现行星信号没有事件，我们提供的排除图显示的置信水平排除存在的行星作为分离和质量比的函数。

英文摘要：

We present the analysis of the light curves of 9 high-magnification single-lens gravitational microlensing events with lenses passing over source stars, including OGLE-2004-BLG-254, MOA-2007-BLG-176, MOA-2007-BLG-233/OGLE-2007-BLG-302, MOA-2009-BLG-174, MOA-2010-BLG-436, MOA-2011-BLG-093, MOA-2011-BLG-274, OGLE-2011-BLG-0990/MOA-2011-BLG-300, and OGLE-2011-BLG-1101/MOA-2011-BLG-325. For all events, we measure the linear limb-darkening coefficients of the surface brightness profile of source stars by measuring the deviation of the light curves near the peak affected by the finite-source effect. For 7 events, we measure the Einstein radii and the lens-source relative proper motions. Among them, 5 events are found to have Einstein radii less than 0.2 mas, making the lenses candidates of very low-mass stars or brown dwarfs. For MOA-2011-BLG-274, especially, the small Einstein radius of $θ_{\rm E}\sim 0.08$ mas combined with the short time scale of $t_{\rm E}\sim 2.7$ days suggests the possibility that the lens is a free-floating planet. For MOA-2009-BLG-174, we measure the lens parallax and thus uniquely determine the physical parameters of the lens. We also find that the measured lens mass of $\sim 0.84\ M_\odot$ is consistent with that of a star blended with the source, suggesting that the blend is likely to be the lens. Although we find planetary signals for none of events, we provide exclusion diagrams showing the confidence levels excluding the existence of a planet as a function of the separation and mass ratio.

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