Combined Analysis of the Binary Lens Caustic-crossing Event MACHO 98-SMC-1
Combined Analysis of the Binary Lens Caustic-crossing Event MACHO 98-SMC-1
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二元透镜焦散穿越事件MACHO 98-SMC-1的联合分析
DOI：
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发表时间：
1999
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通讯作者：
A. Williams
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作者：
C. Afonso;C. Alard;J. Albert;J. Andersen;R. Ansari;E. Aubourg;P. Bareyre;P. Bareyre;F. Bauer;J. Beaulieu;A. Bouquet;S. Char;X. Charlot;F. Couchot;C. Coutures;F. Derue;R. Ferlet;J. Glicenstein;B. Goldman;A. Gould;D. Graff;D. Graff;M. Gros;J. Haissinski;J. Hamilton;D. Hardin;J. Kat;A. Kim;T. Lasserre;É. Lesquoy;C. Loup;C. Magneville;J. Marquette;E. Maurice;A. Milsztajn;M. Moniez;N. Palanque;O. Perdereau;L. Prévot;N. Regnault;J. Rich;M. Spiro;A. Vidal;L. Vigroux;S. Zylberajch;C. Alcock;C. Alcock;R. Allsman;D. Alves;T. Axelrod;A. Becker;K. Cook;A. J. Drake;Kenneth C. Freeman;K. Griest;K. Griest;L. King;M. Lehner;S. Marshall;D. Minniti;B. Peterson;M. Pratt;P. Quinn;A. Rodgers;P. Stetson;C. Stubbs;C. Stubbs;W. Sutherland;A. Tomaney;T. Vandehei;T. Vandehei;S. Rhie;D. Bennett;P. C. Fragile;B.R. Johnson;J. Quinn;A. Udalski;M. Kubiak;M. Szymański;G. Pietrzyński;P. Woźniak;K. Żebruń;M. Albrow;J. Caldwell;D. Depoy;M. Dominik;B. Gaudi;J. Greenhill;K. Hill;Stephen R. Kane;R. Martin;J. Menzies;R. M. Naber;R. Pogge;K. Pollard;P. Sackett;K. Sahu;P. Vermaak;R. Watson;A. Williams
我们对来自五个不同微透镜协作的双透镜微透镜事件MACHO 98-SMC-1的数据进行了拟合，发现了两个不同的解：(d，q)=(0.54，0.50)和(d，q)=(3.65，0.36)，其中d是爱因斯坦半径的单位。然而，透镜的相对自行在两种溶液中非常相似，即1.30kmS-1kpc-1和1.48kmS-1kpc-1，从而证实该透镜位于小麦哲伦星云中。近二进制可以是旋转的，也可以是近似静态的，但宽二进制必须以接近其最大允许速率的速度旋转，才能与所有数据保持一致。我们测量了从I到V的五个波段的肢体变暗系数，正如预期的那样，这些系数随着波长的增加而逐渐减小。这是第一次对一颗金属贫乏的A星进行肢体暗化测量。
We fit the data for the binary lens microlensing event MACHO 98-SMC-1 from five different microlensing collaborations and find two distinct solutions characterized by binary separation d and mass ratio q: (d,q) = (0.54,0.50) and (d,q) = (3.65,0.36), where d is in units of the Einstein radius. However, the relative proper motion of the lens is very similar in the two solutions, 1.30 km s-1 kpc-1 and 1.48 km s-1 kpc-1, thus confirming that the lens is in the Small Magellanic Cloud. The close binary can be either rotating or approximately static but the wide binary must be rotating at close to its maximum allowed rate to be consistent with all the data. We measure limb-darkening coefficients for five bands ranging from I to V. As expected, these progressively decrease with rising wavelength. This is the first measurement of limb darkening for a metal-poor A star.