利用正交基函数重建引力透镜星系团内部的质量分布

引力透镜现象是探测星系团物质（包括暗物质）分布的最直接有效的信息来源。现有的方法中有一类采用模型拟合的办法，但是结果显然会受到模型本身的偏向，并且实际上星系团内部结构复杂，简单的模型并不普适。另外一类采用非参数拟合，这一般会引入很精细的正则算法，并且计算量非常大。本计划拟用一种折中的办法,采用正交基函数来重构星系团内部的物质分布。在保持拟合的灵活性的同时大大降低计算量，从而为利用引力透镜信号重建星系团质量分布开辟一条新的途径。

Gravitational lensing is the most powerful tool to detect the mass distribution of cluster of galaxies. Usually people use a model, such as NFW to fit the signal therefore the result is model dependent. Or we could use non-parametric method but such methods are too flexible and need sophisticated regularization. Here we propose an new method; use a set of orthogonal basis function to remove the model dependence and to keep the flexibility simultaneously. This will provide an new way out for the mass reconstruction of galaxy clusters by using gravitational lensing.