在强引力透镜效应下用NFW质量分布拟合星系团Abell 2390

利用强引力透镜效应来测量星系团的质量是一个非常有效的方法．将非对称NFW质量模型用于星系团Abell 2390．通过标准的χ^2 拟合，得到在巨型弧（38″或177．25kpc）内的投影质量为7. 028 × 10^13 h0^-1Mo．这一结果与（S．W．Allen等人，2007年）用X-ray的方法和（Pierre等人，1996年）用强引力透镜效应的方法得到的结果非常一致．对有争议的直型弧，根据最佳拟合，分析了它的形态，它仅仅是一个在透镜体焦散曲线附近的天体被强烈拉伸的像，没有断裂或多重像交叠的像结构．此外，第一次发现了一组多重像A（它的红移为1．533）和红移为4．05的弧H5的第三个对应多重像H5-c．

The modeling of Abell 2390 in strong lensing with NFW mass profile

Strong lensing effect is a powerful approach to measure the masses of dusters. We use asymmetric NFW( Navarro, Frenk, and White ) mass model for cluster Abell 2390. The modeling is based on a standardx2 minimiza-tion ( Comerford et al. , 2005 ). With our best -fit NFW mass model, the projected mass within giant arc ( 38" or177.25 kpc ) is 7. 028 x 1013 h0-1 Mo . This result is well coincident with X- ray method mass measurement ( S-.W. Allen et al., 2007 ) and strong leusing mass of Pierre et al. (1996). For notorious "straight arc" in A2390 at z=0. 913 , we analyzed its morphology with our best -fit modeling. It is just strongly elongated singular lensed gal-axy near the cusp caustic of the cluster lens and no broken or counter images region configuration. Moreover, we first find new counter arc A at redshift 1. 533 and the third counter arc H5 - c of multiple - imaged source namely H5 ( J.P. Kneib et al., 1999 ) at z=4.05.