在强引力透镜效应下用NFW质量分布拟合星系团Abell 2390(英文)

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

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χ2拟合,得到在巨型弧(38″或177.25kpc)内的投影质量为7.028×1013h0-1M⊙.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.

Strong lensing effect is a powerful approach to measure the masses of clusters. We use asymmetric NFW （ Navarro, Frenk, and White ） mass model for cluster Abell 2390. The modeling is based on a standardχ^2 minimization （ Comerford et al. , 2005 ）. With our best - fit NFW mass model, the projected mass within giant arc （ 38＂ or 177.25 kpc ） is 7. 028 × 10^13 h0^-1 Mo . This result is well coincident with X - ray method mass measurement （ S. W. Allen et al. , 2007 ） and strong lensing 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 galaxy 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 ） atz = 4. 05 .